VSA Browser

Glossary of VSA attributes

This Glossary alphabetically lists all attributes used in the VSAv20241206 database(s) held in the VSA. If you would like to have more information about the schema tables please use the VSAv20241206 Schema Browser (other Browser versions).

A B C D E F G H I J K L M
N O P Q R S T U V W X Y Z

H

Name Schema Table Database Description Type Length Unit Default Value Unified Content Descriptor

H twomass SIXDF H magnitude (HEXT) used for H selection real 4 mag

h_1AperMag1 vvvSource VVVDR5 Point source H_1 aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

h_1AperMag1Err vvvSource VVVDR5 Error in point source H_1 mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

h_1AperMag3 vvvSource VVVDR5 Default point source H_1 aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

h_1AperMag3Err vvvSource VVVDR5 Error in default point source H_1 mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

h_1AperMag4 vvvSource VVVDR5 Point source H_1 aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

h_1AperMag4Err vvvSource VVVDR5 Error in point source H_1 mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

h_1AverageConf vvvSource VVVDR5 average confidence in 2 arcsec diameter default aperture (aper3) H_1 real 4 -0.9999995e9 stat.likelihood;em.IR.H

h_1Class vvvSource VVVDR5 discrete image classification flag in H_1 smallint 2 -9999 src.class;em.IR.H

h_1ClassStat vvvSource VVVDR5 S-Extractor classification statistic in H_1 real 4 -0.9999995e9 stat;em.IR.H

h_1Ell vvvSource VVVDR5 1-b/a, where a/b=semi-major/minor axes in H_1 real 4 -0.9999995e9 src.ellipticity;em.IR.H

h_1eNum vvvMergeLog VVVDR5 the extension number of this H_1 frame tinyint 1 meta.number;em.IR.H

h_1eNum vvvPsfDophotZYJHKsMergeLog VVVDR5 the extension number of this 1st epoch H frame tinyint 1 meta.number;em.IR.H

h_1ErrBits vvvSource VVVDR5 processing warning/error bitwise flags in H_1 int 4 -99999999 meta.code;em.IR.H

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

h_1Eta vvvSource VVVDR5 Offset of H_1 detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

h_1Gausig vvvSource VVVDR5 RMS of axes of ellipse fit in H_1 real 4 pixels -0.9999995e9 src.morph.param;em.IR.H

h_1mfID vvvMergeLog VVVDR5 the UID of the relevant H_1 multiframe bigint 8 meta.id;obs.field;em.IR.H

h_1mfID vvvPsfDophotZYJHKsMergeLog VVVDR5 the UID of the relevant 1st epoch H tile multiframe bigint 8 meta.id;obs.field;em.IR.H

h_1Mjd vvvPsfDophotZYJHKsMergeLog VVVDR5 the MJD of the 1st epoch H tile multiframe float 8 time;em.IR.H

h_1Mjd vvvSource VVVDR5 Modified Julian Day in H_1 band float 8 days -0.9999995e9 time.epoch;em.IR.H

h_1mks_1Pnt vvvSource VVVDR5 Point source colour H_1-Ks_1 (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

h_1mks_1PntErr vvvSource VVVDR5 Error on point source colour H_1-Ks_1 real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

h_1PA vvvSource VVVDR5 ellipse fit celestial orientation in H_1 real 4 Degrees -0.9999995e9 pos.posAng;em.IR.H

h_1ppErrBits vvvSource VVVDR5 additional WFAU post-processing error bits in H_1 int 4 0 meta.code;em.IR.H

h_1SeqNum vvvSource VVVDR5 the running number of the H_1 detection int 4 -99999999 meta.number;em.IR.H

h_1Xi vvvSource VVVDR5 Offset of H_1 detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

h_2AperMag1 vvvSource VVVDR5 Point source H_2 aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

h_2AperMag1Err vvvSource VVVDR5 Error in point source H_2 mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

h_2AperMag3 vvvSource VVVDR5 Default point source H_2 aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

h_2AperMag3Err vvvSource VVVDR5 Error in default point source H_2 mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

h_2AperMag4 vvvSource VVVDR5 Point source H_2 aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

h_2AperMag4Err vvvSource VVVDR5 Error in point source H_2 mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

h_2AverageConf vvvSource VVVDR5 average confidence in 2 arcsec diameter default aperture (aper3) H_2 real 4 -0.9999995e9 stat.likelihood;em.IR.H

h_2Class vvvSource VVVDR5 discrete image classification flag in H_2 smallint 2 -9999 src.class;em.IR.H

h_2ClassStat vvvSource VVVDR5 S-Extractor classification statistic in H_2 real 4 -0.9999995e9 stat;em.IR.H

h_2Ell vvvSource VVVDR5 1-b/a, where a/b=semi-major/minor axes in H_2 real 4 -0.9999995e9 src.ellipticity;em.IR.H

h_2eNum vvvMergeLog VVVDR5 the extension number of this H_2 frame tinyint 1 meta.number;em.IR.H

h_2eNum vvvPsfDophotZYJHKsMergeLog VVVDR5 the extension number of this 2nd epoch H frame tinyint 1 meta.number;em.IR.H

h_2ErrBits vvvSource VVVDR5 processing warning/error bitwise flags in H_2 int 4 -99999999 meta.code;em.IR.H

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

h_2Eta vvvSource VVVDR5 Offset of H_2 detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

h_2Gausig vvvSource VVVDR5 RMS of axes of ellipse fit in H_2 real 4 pixels -0.9999995e9 src.morph.param;em.IR.H

h_2mfID vvvMergeLog VVVDR5 the UID of the relevant H_2 multiframe bigint 8 meta.id;obs.field;em.IR.H

h_2mfID vvvPsfDophotZYJHKsMergeLog VVVDR5 the UID of the relevant 2nd epoch H tile multiframe bigint 8 meta.id;obs.field;em.IR.H

h_2Mjd vvvPsfDophotZYJHKsMergeLog VVVDR5 the MJD of the 2nd epoch H tile multiframe float 8 time;em.IR.H

h_2Mjd vvvSource VVVDR5 Modified Julian Day in H_2 band float 8 days -0.9999995e9 time.epoch;em.IR.H

h_2mks_2Pnt vvvSource VVVDR5 Point source colour H_2-Ks_2 (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

h_2mks_2PntErr vvvSource VVVDR5 Error on point source colour H_2-Ks_2 real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

h_2mrat twomass_scn TWOMASS H-band average 2nd image moment ratio. real 4 stat.fit.param

h_2mrat twomass_sixx2_scn TWOMASS H band average 2nd image moment ratio for scan real 4

h_2PA vvvSource VVVDR5 ellipse fit celestial orientation in H_2 real 4 Degrees -0.9999995e9 pos.posAng;em.IR.H

h_2ppErrBits vvvSource VVVDR5 additional WFAU post-processing error bits in H_2 int 4 0 meta.code;em.IR.H

h_2SeqNum vvvSource VVVDR5 the running number of the H_2 detection int 4 -99999999 meta.number;em.IR.H

h_2Xi vvvSource VVVDR5 Offset of H_2 detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

h_5sig_ba twomass_xsc TWOMASS H minor/major axis ratio fit to the 5-sigma isophote. real 4 phys.size.axisRatio

h_5sig_phi twomass_xsc TWOMASS H angle to 5-sigma major axis (E of N). smallint 2 degrees stat.error

h_5surf twomass_xsc TWOMASS H central surface brightness (r<=5). real 4 mag phot.mag.sb

h_ba twomass_xsc TWOMASS H minor/major axis ratio fit to the 3-sigma isophote. real 4 phys.size.axisRatio

h_back twomass_xsc TWOMASS H coadd median background. real 4 meta.code

h_bisym_chi twomass_xsc TWOMASS H bi-symmetric cross-correlation chi. real 4 stat.fit.param

h_bisym_rat twomass_xsc TWOMASS H bi-symmetric flux ratio. real 4 phot.flux;arith.ratio

h_bndg_amp twomass_xsc TWOMASS H banding maximum FT amplitude on this side of coadd. real 4 DN stat.fit.param

h_bndg_per twomass_xsc TWOMASS H banding Fourier Transf. period on this side of coadd. int 4 arcsec stat.fit.param

h_cmsig twomass_psc TWOMASS Corrected photometric uncertainty for the default H-band magnitude. real 4 mag H-band phot.flux

h_con_indx twomass_xsc TWOMASS H concentration index r_75%/r_25%. real 4 phys.size;arith.ratio

h_d_area twomass_xsc TWOMASS H 5-sigma to 3-sigma differential area. smallint 2 stat.fit.residual

h_flg_10 twomass_xsc TWOMASS H confusion flag for 10 arcsec circular ap. mag. smallint 2 meta.code

h_flg_15 twomass_xsc TWOMASS H confusion flag for 15 arcsec circular ap. mag. smallint 2 meta.code

h_flg_20 twomass_xsc TWOMASS H confusion flag for 20 arcsec circular ap. mag. smallint 2 meta.code

h_flg_25 twomass_xsc TWOMASS H confusion flag for 25 arcsec circular ap. mag. smallint 2 meta.code

h_flg_30 twomass_xsc TWOMASS H confusion flag for 30 arcsec circular ap. mag. smallint 2 meta.code

h_flg_40 twomass_xsc TWOMASS H confusion flag for 40 arcsec circular ap. mag. smallint 2 meta.code

h_flg_5 twomass_xsc TWOMASS H confusion flag for 5 arcsec circular ap. mag. smallint 2 meta.code

h_flg_50 twomass_xsc TWOMASS H confusion flag for 50 arcsec circular ap. mag. smallint 2 meta.code

h_flg_60 twomass_xsc TWOMASS H confusion flag for 60 arcsec circular ap. mag. smallint 2 meta.code

h_flg_7 twomass_sixx2_xsc TWOMASS H confusion flag for 7 arcsec circular ap. mag smallint 2

h_flg_7 twomass_xsc TWOMASS H confusion flag for 7 arcsec circular ap. mag. smallint 2 meta.code

h_flg_70 twomass_xsc TWOMASS H confusion flag for 70 arcsec circular ap. mag. smallint 2 meta.code

h_flg_c twomass_xsc TWOMASS H confusion flag for Kron circular mag. smallint 2 meta.code

h_flg_e twomass_xsc TWOMASS H confusion flag for Kron elliptical mag. smallint 2 meta.code

h_flg_fc twomass_xsc TWOMASS H confusion flag for fiducial Kron circ. mag. smallint 2 meta.code

h_flg_fe twomass_xsc TWOMASS H confusion flag for fiducial Kron ell. mag. smallint 2 meta.code

h_flg_i20c twomass_xsc TWOMASS H confusion flag for 20mag/sq." iso. circ. mag. smallint 2 meta.code

h_flg_i20e twomass_xsc TWOMASS H confusion flag for 20mag/sq." iso. ell. mag. smallint 2 meta.code

h_flg_i21c twomass_xsc TWOMASS H confusion flag for 21mag/sq." iso. circ. mag. smallint 2 meta.code

h_flg_i21e twomass_xsc TWOMASS H confusion flag for 21mag/sq." iso. ell. mag. smallint 2 meta.code

h_flg_j21fc twomass_xsc TWOMASS H confusion flag for 21mag/sq." iso. fid. circ. mag. smallint 2 meta.code

h_flg_j21fe twomass_xsc TWOMASS H confusion flag for 21mag/sq." iso. fid. ell. mag. smallint 2 meta.code

h_flg_k20fc twomass_xsc TWOMASS H confusion flag for 20mag/sq." iso. fid. circ. mag. smallint 2 meta.code

h_flg_k20fe twomass_sixx2_xsc TWOMASS H confusion flag for 20mag/sq.″ iso. fid. ell. mag smallint 2

h_flg_k20fe twomass_xsc TWOMASS H confusion flag for 20mag/sq." iso. fid. ell. mag. smallint 2 meta.code

h_k twomass_sixx2_psc TWOMASS The H-Ks color, computed from the H-band and Ks-band magnitudes (h_m and k_m, respectively) of the source. In cases where the second or third digit in rd_flg is equal to either "0", "4", "6", or "9", no color is computed because the photometry in one or both bands is of lower quality or the source is not detected. real 4

h_m twomass_psc TWOMASS Default H-band magnitude real 4 mag phot.flux

h_m twomass_sixx2_psc TWOMASS H selected "default" magnitude real 4 mag

h_m_10 twomass_xsc TWOMASS H 10 arcsec radius circular aperture magnitude. real 4 mag phot.flux

h_m_15 twomass_xsc TWOMASS H 15 arcsec radius circular aperture magnitude. real 4 mag phot.flux

h_m_20 twomass_xsc TWOMASS H 20 arcsec radius circular aperture magnitude. real 4 mag phot.flux

h_m_25 twomass_xsc TWOMASS H 25 arcsec radius circular aperture magnitude. real 4 mag phot.flux

h_m_2mass allwise_sc WISE 2MASS H-band magnitude or magnitude upper limit of the associated 2MASS PSC source. This column is "null" if there is no associated 2MASS PSC source or if the 2MASS PSC H-band magnitude entry is "null". float 8 mag

h_m_2mass wise_allskysc WISE 2MASS H-band magnitude or magnitude upper limit of the associated 2MASS PSC source.
This column is default if there is no associated 2MASS PSC source or if the 2MASS PSC H-band magnitude entry is default. real 4 mag -0.9999995e9

h_m_2mass wise_prelimsc WISE 2MASS H-band magnitude or magnitude upper limit of the associated 2MASS PSC source
This column is default if there is no associated 2MASS PSC source or if the 2MASS PSC H-band magnitude entry is default real 4 mag -0.9999995e9

h_m_30 twomass_xsc TWOMASS H 30 arcsec radius circular aperture magnitude. real 4 mag phot.flux

h_m_40 twomass_xsc TWOMASS H 40 arcsec radius circular aperture magnitude. real 4 mag phot.flux

h_m_5 twomass_xsc TWOMASS H 5 arcsec radius circular aperture magnitude. real 4 mag phot.flux

h_m_50 twomass_xsc TWOMASS H 50 arcsec radius circular aperture magnitude. real 4 mag phot.flux

h_m_60 twomass_xsc TWOMASS H 60 arcsec radius circular aperture magnitude. real 4 mag phot.flux

h_m_7 twomass_sixx2_xsc TWOMASS H 7 arcsec radius circular aperture magnitude real 4 mag

h_m_7 twomass_xsc TWOMASS H 7 arcsec radius circular aperture magnitude. real 4 mag phot.flux

h_m_70 twomass_xsc TWOMASS H 70 arcsec radius circular aperture magnitude. real 4 mag phot.flux

h_m_c twomass_xsc TWOMASS H Kron circular aperture magnitude. real 4 mag phot.flux

h_m_e twomass_xsc TWOMASS H Kron elliptical aperture magnitude. real 4 mag phot.flux

h_m_ext twomass_sixx2_xsc TWOMASS H mag from fit extrapolation real 4 mag

h_m_ext twomass_xsc TWOMASS H mag from fit extrapolation. real 4 mag phot.flux

h_m_fc twomass_xsc TWOMASS H fiducial Kron circular magnitude. real 4 mag phot.flux

h_m_fe twomass_xsc TWOMASS H fiducial Kron ell. mag aperture magnitude. real 4 mag phot.flux

h_m_i20c twomass_xsc TWOMASS H 20mag/sq." isophotal circular ap. magnitude. real 4 mag phot.flux

h_m_i20e twomass_xsc TWOMASS H 20mag/sq." isophotal elliptical ap. magnitude. real 4 mag phot.flux

h_m_i21c twomass_xsc TWOMASS H 21mag/sq." isophotal circular ap. magnitude. real 4 mag phot.flux

h_m_i21e twomass_xsc TWOMASS H 21mag/sq." isophotal elliptical ap. magnitude. real 4 mag phot.flux

h_m_j21fc twomass_xsc TWOMASS H 21mag/sq." isophotal fiducial circ. ap. mag. real 4 mag phot.flux

h_m_j21fe twomass_xsc TWOMASS H 21mag/sq." isophotal fiducial ell. ap. magnitude. real 4 mag phot.flux

h_m_k20fc twomass_xsc TWOMASS H 20mag/sq." isophotal fiducial circ. ap. mag. real 4 mag phot.flux

H_M_K20FE twomass SIXDF H 20mag/sq." isophotal fiducial ell. ap. magnitude real 4 mag

h_m_k20fe twomass_sixx2_xsc TWOMASS H 20mag/sq.″ isophotal fiducial ell. ap. magnitude real 4 mag

h_m_k20fe twomass_xsc TWOMASS H 20mag/sq." isophotal fiducial ell. ap. magnitude. real 4 mag phot.flux

h_m_stdap twomass_psc TWOMASS H-band "standard" aperture magnitude. real 4 mag phot.flux

h_m_sys twomass_xsc TWOMASS H system photometry magnitude. real 4 mag phot.flux

h_mnsurfb_eff twomass_xsc TWOMASS H mean surface brightness at the half-light radius. real 4 mag phot.mag.sb

h_msig twomass_sixx2_psc TWOMASS H "default" mag uncertainty real 4 mag

h_msig_10 twomass_xsc TWOMASS H 1-sigma uncertainty in 10 arcsec circular ap. mag. real 4 mag stat.error

h_msig_15 twomass_xsc TWOMASS H 1-sigma uncertainty in 15 arcsec circular ap. mag. real 4 mag stat.error

h_msig_20 twomass_xsc TWOMASS H 1-sigma uncertainty in 20 arcsec circular ap. mag. real 4 mag stat.error

h_msig_25 twomass_xsc TWOMASS H 1-sigma uncertainty in 25 arcsec circular ap. mag. real 4 mag stat.error

h_msig_2mass allwise_sc WISE 2MASS H-band corrected photometric uncertainty of the associated 2MASS PSC source. This column is "null" if there is no associated 2MASS PSC source or if the 2MASS PSC H-band uncertainty entry is "null". float 8 mag

h_msig_2mass wise_allskysc WISE 2MASS H-band corrected photometric uncertainty of the associated 2MASS PSC source.
This column is default if there is no associated 2MASS PSC source or if the 2MASS PSC H-band uncertainty entry is default. real 4 mag -0.9999995e9

h_msig_2mass wise_prelimsc WISE 2MASS H-band corrected photometric uncertainty of the associated 2MASS PSC source
This column is default if there is no associated 2MASS PSC source or if the 2MASS PSC H-band uncertainty entry is default real 4 mag -0.9999995e9

h_msig_30 twomass_xsc TWOMASS H 1-sigma uncertainty in 30 arcsec circular ap. mag. real 4 mag stat.error

h_msig_40 twomass_xsc TWOMASS H 1-sigma uncertainty in 40 arcsec circular ap. mag. real 4 mag stat.error

h_msig_5 twomass_xsc TWOMASS H 1-sigma uncertainty in 5 arcsec circular ap. mag. real 4 mag stat.error

h_msig_50 twomass_xsc TWOMASS H 1-sigma uncertainty in 50 arcsec circular ap. mag. real 4 mag stat.error

h_msig_60 twomass_xsc TWOMASS H 1-sigma uncertainty in 60 arcsec circular ap. mag. real 4 mag stat.error

h_msig_7 twomass_sixx2_xsc TWOMASS H 1-sigma uncertainty in 7 arcsec circular ap. mag real 4 mag

h_msig_7 twomass_xsc TWOMASS H 1-sigma uncertainty in 7 arcsec circular ap. mag. real 4 mag stat.error

h_msig_70 twomass_xsc TWOMASS H 1-sigma uncertainty in 70 arcsec circular ap. mag. real 4 mag stat.error

h_msig_c twomass_xsc TWOMASS H 1-sigma uncertainty in Kron circular mag. real 4 mag stat.error

h_msig_e twomass_xsc TWOMASS H 1-sigma uncertainty in Kron elliptical mag. real 4 mag stat.error

h_msig_ext twomass_sixx2_xsc TWOMASS H 1-sigma uncertainty in mag from fit extrapolation real 4 mag

h_msig_ext twomass_xsc TWOMASS H 1-sigma uncertainty in mag from fit extrapolation. real 4 mag stat.error

h_msig_fc twomass_xsc TWOMASS H 1-sigma uncertainty in fiducial Kron circ. mag. real 4 mag stat.error

h_msig_fe twomass_xsc TWOMASS H 1-sigma uncertainty in fiducial Kron ell. mag. real 4 mag stat.error

h_msig_i20c twomass_xsc TWOMASS H 1-sigma uncertainty in 20mag/sq." iso. circ. mag. real 4 mag stat.error

h_msig_i20e twomass_xsc TWOMASS H 1-sigma uncertainty in 20mag/sq." iso. ell. mag. real 4 mag stat.error

h_msig_i21c twomass_xsc TWOMASS H 1-sigma uncertainty in 21mag/sq." iso. circ. mag. real 4 mag stat.error

h_msig_i21e twomass_xsc TWOMASS H 1-sigma uncertainty in 21mag/sq." iso. ell. mag. real 4 mag stat.error

h_msig_j21fc twomass_xsc TWOMASS H 1-sigma uncertainty in 21mag/sq." iso.fid.circ.mag. real 4 mag stat.error

h_msig_j21fe twomass_xsc TWOMASS H 1-sigma uncertainty in 21mag/sq." iso.fid.ell.mag. real 4 mag stat.error

h_msig_k20fc twomass_xsc TWOMASS H 1-sigma uncertainty in 20mag/sq." iso.fid.circ. mag. real 4 mag stat.error

h_msig_k20fe twomass_sixx2_xsc TWOMASS H 1-sigma uncertainty in 20mag/sq.″ iso.fid.ell.mag real 4 mag

h_msig_k20fe twomass_xsc TWOMASS H 1-sigma uncertainty in 20mag/sq." iso.fid.ell.mag. real 4 mag stat.error

h_msig_stdap twomass_psc TWOMASS Uncertainty in the H-band standard aperture magnitude. real 4 mag phot.flux

h_msig_sys twomass_xsc TWOMASS H 1-sigma uncertainty in system photometry mag. real 4 mag stat.error

h_msigcom twomass_psc TWOMASS Combined, or total photometric uncertainty for the default H-band magnitude. real 4 mag H-band phot.flux

h_msigcom twomass_sixx2_psc TWOMASS combined (total) H band photometric uncertainty real 4 mag

h_msnr10 twomass_scn TWOMASS The estimated H-band magnitude at which SNR=10 is achieved for this scan. real 4 mag phot.flux

h_msnr10 twomass_sixx2_scn TWOMASS H mag at which SNR=10 is achieved, from h_psp and h_zp_ap real 4 mag

h_n_snr10 twomass_scn TWOMASS Number of point sources at H-band with SNR>10 (instrumental mag <=15.1) int 4 meta.number

h_n_snr10 twomass_sixx2_scn TWOMASS number of H point sources with SNR>10 (instrumental m<=15.1) int 4

h_pchi twomass_xsc TWOMASS H chi^2 of fit to rad. profile (LCSB: alpha scale len). real 4 stat.fit.param

h_peak twomass_xsc TWOMASS H peak pixel brightness. real 4 mag phot.mag.sb

h_perc_darea twomass_xsc TWOMASS H 5-sigma to 3-sigma percent area change. smallint 2 FIT_PARAM

h_phi twomass_xsc TWOMASS H angle to 3-sigma major axis (E of N). smallint 2 degrees pos.posAng

h_psfchi twomass_psc TWOMASS Reduced chi-squared goodness-of-fit value for the H-band profile-fit photometry made on the 1.3 s "Read_2" exposures. real 4 stat.fit.param

h_psp twomass_scn TWOMASS H-band photometric sensitivity paramater (PSP). real 4 instr.sensitivity

h_psp twomass_sixx2_scn TWOMASS H photometric sensitivity param: h_shape_avg*(h_fbg_avg^.29) real 4

h_pts_noise twomass_scn TWOMASS Base-10 logarithm of the mode of the noise distribution for all point source detections in the scan, where the noise is estimated from the measured H-band photometric errors and is expressed in units of mJy. real 4 instr.det.noise

h_pts_noise twomass_sixx2_scn TWOMASS log10 of H band modal point src noise estimate real 4 logmJy

h_r_c twomass_xsc TWOMASS H Kron circular aperture radius. real 4 arcsec phys.angSize;src

h_r_e twomass_xsc TWOMASS H Kron elliptical aperture semi-major axis. real 4 arcsec phys.angSize;src

h_r_eff twomass_xsc TWOMASS H half-light (integrated half-flux point) radius. real 4 arcsec phys.angSize;src

h_r_i20c twomass_xsc TWOMASS H 20mag/sq." isophotal circular aperture radius. real 4 arcsec phys.angSize;src

h_r_i20e twomass_xsc TWOMASS H 20mag/sq." isophotal elliptical ap. semi-major axis. real 4 arcsec phys.angSize;src

h_r_i21c twomass_xsc TWOMASS H 21mag/sq." isophotal circular aperture radius. real 4 arcsec phys.angSize;src

h_r_i21e twomass_xsc TWOMASS H 21mag/sq." isophotal elliptical ap. semi-major axis. real 4 arcsec phys.angSize;src

h_resid_ann twomass_xsc TWOMASS H residual annulus background median. real 4 DN meta.code

h_sc_1mm twomass_xsc TWOMASS H 1st moment (score) (LCSB: super blk 2,4,8 SNR). real 4 meta.code

h_sc_2mm twomass_xsc TWOMASS H 2nd moment (score) (LCSB: SNRMAX - super SNR max). real 4 meta.code

h_sc_msh twomass_xsc TWOMASS H median shape score. real 4 meta.code

h_sc_mxdn twomass_xsc TWOMASS H mxdn (score) (LCSB: BSNR - block/smoothed SNR). real 4 meta.code

h_sc_r1 twomass_xsc TWOMASS H r1 (score). real 4 meta.code

h_sc_r23 twomass_xsc TWOMASS H r23 (score) (LCSB: TSNR - integrated SNR for r=15). real 4 meta.code

h_sc_sh twomass_xsc TWOMASS H shape (score). real 4 meta.code

h_sc_vint twomass_xsc TWOMASS H vint (score). real 4 meta.code

h_sc_wsh twomass_xsc TWOMASS H wsh (score) (LCSB: PSNR - peak raw SNR). real 4 meta.code

h_seetrack twomass_xsc TWOMASS H band seetracking score. real 4 meta.code

h_sh0 twomass_xsc TWOMASS H ridge shape (LCSB: BSNR limit). real 4 FIT_PARAM

h_shape_avg twomass_scn TWOMASS H-band average seeing shape for scan. real 4 instr.obsty.seeing

h_shape_avg twomass_sixx2_scn TWOMASS H band average seeing shape for scan real 4

h_shape_rms twomass_scn TWOMASS RMS-error of H-band average seeing shape. real 4 instr.obsty.seeing

h_shape_rms twomass_sixx2_scn TWOMASS rms of H band avg seeing shape for scan real 4

h_sig_sh0 twomass_xsc TWOMASS H ridge shape sigma (LCSB: B2SNR limit). real 4 FIT_PARAM

h_snr twomass_psc TWOMASS H-band "scan" signal-to-noise ratio. real 4 mag instr.det.noise

h_snr twomass_sixx2_psc TWOMASS H band "scan" signal-to-noise ratio real 4

h_subst2 twomass_xsc TWOMASS H residual background #2 (score). real 4 meta.code

h_zp_ap twomass_scn TWOMASS Photometric zero-point for H-band aperture photometry. real 4 mag phot.mag;arith.zp

h_zp_ap twomass_sixx2_scn TWOMASS H band ap. calibration photometric zero-point for scan real 4 mag

h_zperr_ap twomass_scn TWOMASS RMS-error of zero-point for H-band aperture photometry real 4 mag stat.error

h_zperr_ap twomass_sixx2_scn TWOMASS H band ap. calibration rms error of zero-point for scan real 4 mag

ha twomass_scn TWOMASS Hour angle at beginning of scan. float 8 hr pos.posAng

ha twomass_sixx2_scn TWOMASS beginning hour angle of scan data float 8 hr

halfFlux sharksDetection SHARKSv20210222 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux sharksDetection SHARKSv20210421 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux ultravistaDetection ULTRAVISTADR4 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation, not available in SE output {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vhsDetection VHSDR2 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count;em.opt

halfFlux vhsDetection VHSDR3 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vhsDetection VHSDR4 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vhsDetection VHSDR5 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vhsDetection VHSDR6 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vhsDetection VHSv20120926 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vhsDetection VHSv20130417 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vhsDetection VHSv20140409 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vhsDetection VHSv20150108 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vhsDetection VHSv20160114 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vhsDetection VHSv20160507 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vhsDetection VHSv20170630 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vhsDetection VHSv20180419 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vhsDetection VHSv20201209 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vhsDetection VHSv20231101 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vhsDetection VHSv20240731 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vhsDetection, vhsListRemeasurement VHSDR1 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count;em.opt

halfFlux videoDetection VIDEODR2 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation, not available in SE output {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count;em.opt

halfFlux videoDetection VIDEODR3 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation, not available in SE output {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux videoDetection VIDEODR4 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation, not available in SE output {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux videoDetection VIDEODR5 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation, not available in SE output {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux videoDetection VIDEOv20100513 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation, not available in SE output {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count;em.opt

halfFlux videoDetection VIDEOv20111208 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation, not available in SE output {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count;em.opt

halfFlux videoListRemeasurement VIDEOv20100513 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count;em.opt

halfFlux vikingDetection VIKINGDR2 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count;em.opt

halfFlux vikingDetection VIKINGDR3 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vikingDetection VIKINGDR4 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vikingDetection VIKINGv20111019 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count;em.opt

halfFlux vikingDetection VIKINGv20130417 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vikingDetection VIKINGv20140402 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vikingDetection VIKINGv20150421 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vikingDetection VIKINGv20151230 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vikingDetection VIKINGv20160406 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vikingDetection VIKINGv20161202 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vikingDetection VIKINGv20170715 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vikingDetection, vikingListRemeasurement VIKINGv20110714 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count;em.opt

halfFlux vmcDetection VMCDR1 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count;em.opt

halfFlux vmcDetection VMCDR2 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vmcDetection VMCDR3 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vmcDetection VMCDR4 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vmcDetection VMCDR5 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vmcDetection VMCv20110909 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count;em.opt

halfFlux vmcDetection VMCv20120126 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count;em.opt

halfFlux vmcDetection VMCv20121128 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vmcDetection VMCv20130304 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vmcDetection VMCv20130805 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vmcDetection VMCv20140428 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vmcDetection VMCv20140903 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vmcDetection VMCv20150309 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vmcDetection VMCv20151218 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vmcDetection VMCv20160311 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vmcDetection VMCv20160822 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vmcDetection VMCv20170109 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vmcDetection VMCv20170411 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vmcDetection VMCv20171101 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vmcDetection VMCv20180702 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vmcDetection VMCv20181120 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vmcDetection VMCv20191212 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vmcDetection VMCv20210708 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vmcDetection VMCv20230816 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vmcDetection VMCv20240226 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vmcDetection, vmcListRemeasurement VMCv20110816 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count;em.opt

halfFlux vmcdeepDetection VMCDEEPv20230713 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vmcdeepDetection VMCDEEPv20240506 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vvvDetection VVVDR1 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vvvDetection VVVDR2 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vvvDetection, vvvDetectionPawPrints, vvvDetectionTiles VVVDR5 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count

halfFlux vvvDetection, vvvListRemeasurement VVVv20100531 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 phot.count;em.opt

halfFluxErr sharksDetection SHARKSv20210222 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr sharksDetection SHARKSv20210421 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr ultravistaDetection ULTRAVISTADR4 error on Half flux, not available in SE output {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vhsDetection VHSDR2 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vhsDetection VHSDR3 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vhsDetection VHSDR4 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vhsDetection VHSDR5 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vhsDetection VHSDR6 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vhsDetection VHSv20120926 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vhsDetection VHSv20130417 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vhsDetection VHSv20140409 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vhsDetection VHSv20150108 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vhsDetection VHSv20160114 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vhsDetection VHSv20160507 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vhsDetection VHSv20170630 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vhsDetection VHSv20180419 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vhsDetection VHSv20201209 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vhsDetection VHSv20231101 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vhsDetection VHSv20240731 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vhsDetection, vhsListRemeasurement VHSDR1 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr videoDetection VIDEODR2 error on Half flux, not available in SE output {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr videoDetection VIDEODR3 error on Half flux, not available in SE output {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr videoDetection VIDEODR4 error on Half flux, not available in SE output {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr videoDetection VIDEODR5 error on Half flux, not available in SE output {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr videoDetection VIDEOv20100513 error on Half flux, not available in SE output {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr videoDetection VIDEOv20111208 error on Half flux, not available in SE output {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr videoListRemeasurement VIDEOv20100513 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vikingDetection VIKINGDR2 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vikingDetection VIKINGDR3 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vikingDetection VIKINGDR4 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vikingDetection VIKINGv20111019 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vikingDetection VIKINGv20130417 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vikingDetection VIKINGv20140402 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vikingDetection VIKINGv20150421 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vikingDetection VIKINGv20151230 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vikingDetection VIKINGv20160406 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vikingDetection VIKINGv20161202 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vikingDetection VIKINGv20170715 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vikingDetection, vikingListRemeasurement VIKINGv20110714 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vmcDetection VMCDR1 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vmcDetection VMCDR2 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vmcDetection VMCDR3 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vmcDetection VMCDR4 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vmcDetection VMCDR5 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vmcDetection VMCv20110909 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vmcDetection VMCv20120126 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vmcDetection VMCv20121128 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vmcDetection VMCv20130304 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vmcDetection VMCv20130805 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vmcDetection VMCv20140428 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vmcDetection VMCv20140903 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vmcDetection VMCv20150309 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vmcDetection VMCv20151218 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vmcDetection VMCv20160311 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vmcDetection VMCv20160822 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vmcDetection VMCv20170109 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vmcDetection VMCv20170411 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vmcDetection VMCv20171101 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vmcDetection VMCv20180702 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vmcDetection VMCv20181120 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vmcDetection VMCv20191212 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vmcDetection VMCv20210708 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vmcDetection VMCv20230816 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vmcDetection VMCv20240226 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vmcDetection, vmcListRemeasurement VMCv20110816 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vmcdeepDetection VMCDEEPv20230713 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vmcdeepDetection VMCDEEPv20240506 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vvvDetection VVVDR1 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vvvDetection VVVDR2 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vvvDetection, vvvDetectionPawPrints, vvvDetectionTiles VVVDR5 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfFluxErr vvvDetection, vvvListRemeasurement VVVv20100531 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 stat.error

halfMag sharksDetection SHARKSv20210222 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag sharksDetection SHARKSv20210421 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag ultravistaDetection ULTRAVISTADR4 Calibrated magnitude within circular aperture halfRad, not available in SE output real 4 mag phot.mag

halfMag vhsDetection VHSDR2 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vhsDetection VHSDR3 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vhsDetection VHSDR4 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vhsDetection VHSDR5 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vhsDetection VHSDR6 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vhsDetection VHSv20120926 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vhsDetection VHSv20130417 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vhsDetection VHSv20140409 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vhsDetection VHSv20150108 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vhsDetection VHSv20160114 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vhsDetection VHSv20160507 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vhsDetection VHSv20170630 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vhsDetection VHSv20180419 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vhsDetection VHSv20201209 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vhsDetection VHSv20231101 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vhsDetection VHSv20240731 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vhsDetection, vhsListRemeasurement VHSDR1 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag videoDetection VIDEODR2 Calibrated magnitude within circular aperture halfRad, not available in SE output real 4 mag phot.mag

halfMag videoDetection VIDEODR3 Calibrated magnitude within circular aperture halfRad, not available in SE output real 4 mag phot.mag

halfMag videoDetection VIDEODR4 Calibrated magnitude within circular aperture halfRad, not available in SE output real 4 mag phot.mag

halfMag videoDetection VIDEODR5 Calibrated magnitude within circular aperture halfRad, not available in SE output real 4 mag phot.mag

halfMag videoDetection VIDEOv20100513 Calibrated magnitude within circular aperture halfRad, not available in SE output real 4 mag phot.mag

halfMag videoDetection VIDEOv20111208 Calibrated magnitude within circular aperture halfRad, not available in SE output real 4 mag phot.mag

halfMag videoListRemeasurement VIDEOv20100513 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vikingDetection VIKINGDR2 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vikingDetection VIKINGDR3 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vikingDetection VIKINGDR4 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vikingDetection VIKINGv20111019 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vikingDetection VIKINGv20130417 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vikingDetection VIKINGv20140402 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vikingDetection VIKINGv20150421 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vikingDetection VIKINGv20151230 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vikingDetection VIKINGv20160406 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vikingDetection VIKINGv20161202 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vikingDetection VIKINGv20170715 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vikingDetection, vikingListRemeasurement VIKINGv20110714 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vmcDetection VMCDR1 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vmcDetection VMCDR2 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vmcDetection VMCDR3 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vmcDetection VMCDR4 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vmcDetection VMCDR5 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vmcDetection VMCv20110909 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vmcDetection VMCv20120126 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vmcDetection VMCv20121128 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vmcDetection VMCv20130304 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vmcDetection VMCv20130805 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vmcDetection VMCv20140428 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vmcDetection VMCv20140903 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vmcDetection VMCv20150309 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vmcDetection VMCv20151218 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vmcDetection VMCv20160311 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vmcDetection VMCv20160822 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vmcDetection VMCv20170109 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vmcDetection VMCv20170411 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vmcDetection VMCv20171101 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vmcDetection VMCv20180702 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vmcDetection VMCv20181120 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vmcDetection VMCv20191212 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vmcDetection VMCv20210708 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vmcDetection VMCv20230816 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vmcDetection VMCv20240226 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vmcDetection, vmcListRemeasurement VMCv20110816 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vmcdeepDetection VMCDEEPv20230713 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vmcdeepDetection VMCDEEPv20240506 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vvvDetection VVVDR1 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vvvDetection VVVDR2 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vvvDetection, vvvDetectionPawPrints, vvvDetectionTiles VVVDR5 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMag vvvDetection, vvvListRemeasurement VVVv20100531 Calibrated magnitude within circular aperture halfRad real 4 mag phot.mag

halfMagErr sharksDetection SHARKSv20210222 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr sharksDetection SHARKSv20210421 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr ultravistaDetection ULTRAVISTADR4 Calibrated error on Half magnitude, not available in SE output real 4 mag stat.error;phot.mag

halfMagErr vhsDetection VHSDR2 Calibrated error on Half magnitude real 4 mag stat.error

halfMagErr vhsDetection VHSDR3 Calibrated error on Half magnitude real 4 mag stat.error

halfMagErr vhsDetection VHSDR4 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vhsDetection VHSDR5 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vhsDetection VHSDR6 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vhsDetection VHSv20120926 Calibrated error on Half magnitude real 4 mag stat.error

halfMagErr vhsDetection VHSv20130417 Calibrated error on Half magnitude real 4 mag stat.error

halfMagErr vhsDetection VHSv20140409 Calibrated error on Half magnitude real 4 mag stat.error

halfMagErr vhsDetection VHSv20150108 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vhsDetection VHSv20160114 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vhsDetection VHSv20160507 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vhsDetection VHSv20170630 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vhsDetection VHSv20180419 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vhsDetection VHSv20201209 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vhsDetection VHSv20231101 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vhsDetection VHSv20240731 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vhsDetection, vhsListRemeasurement VHSDR1 Calibrated error on Half magnitude real 4 mag stat.error

halfMagErr videoDetection VIDEODR2 Calibrated error on Half magnitude, not available in SE output real 4 mag stat.error

halfMagErr videoDetection VIDEODR3 Calibrated error on Half magnitude, not available in SE output real 4 mag stat.error

halfMagErr videoDetection VIDEODR4 Calibrated error on Half magnitude, not available in SE output real 4 mag stat.error;phot.mag

halfMagErr videoDetection VIDEODR5 Calibrated error on Half magnitude, not available in SE output real 4 mag stat.error;phot.mag

halfMagErr videoDetection VIDEOv20100513 Calibrated error on Half magnitude, not available in SE output real 4 mag stat.error

halfMagErr videoDetection VIDEOv20111208 Calibrated error on Half magnitude, not available in SE output real 4 mag stat.error

halfMagErr videoListRemeasurement VIDEOv20100513 Calibrated error on Half magnitude real 4 mag stat.error

halfMagErr vikingDetection VIKINGDR2 Calibrated error on Half magnitude real 4 mag stat.error

halfMagErr vikingDetection VIKINGDR3 Calibrated error on Half magnitude real 4 mag stat.error

halfMagErr vikingDetection VIKINGDR4 Calibrated error on Half magnitude real 4 mag stat.error

halfMagErr vikingDetection VIKINGv20111019 Calibrated error on Half magnitude real 4 mag stat.error

halfMagErr vikingDetection VIKINGv20130417 Calibrated error on Half magnitude real 4 mag stat.error

halfMagErr vikingDetection VIKINGv20140402 Calibrated error on Half magnitude real 4 mag stat.error

halfMagErr vikingDetection VIKINGv20150421 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vikingDetection VIKINGv20151230 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vikingDetection VIKINGv20160406 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vikingDetection VIKINGv20161202 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vikingDetection VIKINGv20170715 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vikingDetection, vikingListRemeasurement VIKINGv20110714 Calibrated error on Half magnitude real 4 mag stat.error

halfMagErr vmcDetection VMCDR1 Calibrated error on Half magnitude real 4 mag stat.error

halfMagErr vmcDetection VMCDR2 Calibrated error on Half magnitude real 4 mag stat.error

halfMagErr vmcDetection VMCDR3 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vmcDetection VMCDR4 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vmcDetection VMCDR5 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vmcDetection VMCv20110909 Calibrated error on Half magnitude real 4 mag stat.error

halfMagErr vmcDetection VMCv20120126 Calibrated error on Half magnitude real 4 mag stat.error

halfMagErr vmcDetection VMCv20121128 Calibrated error on Half magnitude real 4 mag stat.error

halfMagErr vmcDetection VMCv20130304 Calibrated error on Half magnitude real 4 mag stat.error

halfMagErr vmcDetection VMCv20130805 Calibrated error on Half magnitude real 4 mag stat.error

halfMagErr vmcDetection VMCv20140428 Calibrated error on Half magnitude real 4 mag stat.error

halfMagErr vmcDetection VMCv20140903 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vmcDetection VMCv20150309 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vmcDetection VMCv20151218 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vmcDetection VMCv20160311 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vmcDetection VMCv20160822 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vmcDetection VMCv20170109 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vmcDetection VMCv20170411 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vmcDetection VMCv20171101 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vmcDetection VMCv20180702 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vmcDetection VMCv20181120 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vmcDetection VMCv20191212 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vmcDetection VMCv20210708 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vmcDetection VMCv20230816 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vmcDetection VMCv20240226 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vmcDetection, vmcListRemeasurement VMCv20110816 Calibrated error on Half magnitude real 4 mag stat.error

halfMagErr vmcdeepDetection VMCDEEPv20230713 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vmcdeepDetection VMCDEEPv20240506 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vvvDetection VVVDR1 Calibrated error on Half magnitude real 4 mag stat.error

halfMagErr vvvDetection VVVDR2 Calibrated error on Half magnitude real 4 mag stat.error

halfMagErr vvvDetection, vvvDetectionPawPrints, vvvDetectionTiles VVVDR5 Calibrated error on Half magnitude real 4 mag stat.error;phot.mag

halfMagErr vvvDetection, vvvListRemeasurement VVVv20100531 Calibrated error on Half magnitude real 4 mag stat.error

halfRad sharksDetection SHARKSv20210222 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad sharksDetection SHARKSv20210421 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad ultravistaDetection ULTRAVISTADR4 SExtractor half-light radius (FRAC_RADIUS), calcuated assuming Kron flux is total flux {catalogue TType keyword: Half_radius} real 4 pixels phys.angSize

halfRad ultravistaMapRemeasurement ULTRAVISTADR4 Half-light radius (SE: FRAC_RADIUS, calcuated assuming Kron flux is total flux; CASU: default) {catalogue TType keyword: Half_radius} real 4 pixels phys.angSize

halfRad vhsDetection VHSDR2 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize;src

halfRad vhsDetection VHSDR3 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vhsDetection VHSDR4 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vhsDetection VHSDR5 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vhsDetection VHSDR6 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vhsDetection VHSv20120926 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vhsDetection VHSv20130417 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vhsDetection VHSv20140409 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vhsDetection VHSv20150108 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vhsDetection VHSv20160114 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vhsDetection VHSv20160507 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vhsDetection VHSv20170630 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vhsDetection VHSv20180419 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vhsDetection VHSv20201209 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vhsDetection VHSv20231101 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vhsDetection VHSv20240731 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vhsDetection, vhsListRemeasurement VHSDR1 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize;src

halfRad videoDetection VIDEODR2 SExtractor half-light radius (FRAC_RADIUS), calcuated assuming Kron flux is total flux {catalogue TType keyword: Half_radius} real 4 pixels phys.angSize;src

halfRad videoDetection VIDEODR3 SExtractor half-light radius (FRAC_RADIUS), calcuated assuming Kron flux is total flux {catalogue TType keyword: Half_radius} real 4 pixels phys.angSize

halfRad videoDetection VIDEODR4 SExtractor half-light radius (FRAC_RADIUS), calcuated assuming Kron flux is total flux {catalogue TType keyword: Half_radius} real 4 pixels phys.angSize

halfRad videoDetection VIDEODR5 SExtractor half-light radius (FRAC_RADIUS), calcuated assuming Kron flux is total flux {catalogue TType keyword: Half_radius} real 4 pixels phys.angSize

halfRad videoDetection VIDEOv20100513 SExtractor half-light radius (FRAC_RADIUS), calcuated assuming Kron flux is total flux {catalogue TType keyword: Half_radius} real 4 pixels phys.angSize;src

halfRad videoDetection VIDEOv20111208 SExtractor half-light radius (FRAC_RADIUS), calcuated assuming Kron flux is total flux {catalogue TType keyword: Half_radius} real 4 pixels phys.angSize;src

halfRad videoListRemeasurement VIDEOv20100513 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize;src

halfRad vikingDetection VIKINGDR2 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize;src

halfRad vikingDetection VIKINGDR3 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vikingDetection VIKINGDR4 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vikingDetection VIKINGv20111019 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize;src

halfRad vikingDetection VIKINGv20130417 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vikingDetection VIKINGv20140402 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vikingDetection VIKINGv20150421 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vikingDetection VIKINGv20151230 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vikingDetection VIKINGv20160406 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vikingDetection VIKINGv20161202 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vikingDetection VIKINGv20170715 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vikingDetection, vikingListRemeasurement VIKINGv20110714 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize;src

halfRad vikingMapRemeasurement VIKINGZYSELJv20160909 Half-light radius (SE: FRAC_RADIUS, calcuated assuming Kron flux is total flux; CASU: default) {catalogue TType keyword: Half_radius} real 4 pixels phys.angSize

halfRad vikingMapRemeasurement VIKINGZYSELJv20170124 Half-light radius (SE: FRAC_RADIUS, calcuated assuming Kron flux is total flux; CASU: default) {catalogue TType keyword: Half_radius} real 4 pixels phys.angSize

halfRad vmcDetection VMCDR1 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize;src

halfRad vmcDetection VMCDR2 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vmcDetection VMCDR3 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vmcDetection VMCDR4 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vmcDetection VMCDR5 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vmcDetection VMCv20110909 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize;src

halfRad vmcDetection VMCv20120126 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize;src

halfRad vmcDetection VMCv20121128 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vmcDetection VMCv20130304 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vmcDetection VMCv20130805 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vmcDetection VMCv20140428 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vmcDetection VMCv20140903 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vmcDetection VMCv20150309 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vmcDetection VMCv20151218 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vmcDetection VMCv20160311 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vmcDetection VMCv20160822 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vmcDetection VMCv20170109 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vmcDetection VMCv20170411 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vmcDetection VMCv20171101 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vmcDetection VMCv20180702 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vmcDetection VMCv20181120 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vmcDetection VMCv20191212 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vmcDetection VMCv20210708 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vmcDetection VMCv20230816 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vmcDetection VMCv20240226 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vmcDetection, vmcListRemeasurement VMCv20110816 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize;src

halfRad vmcdeepDetection VMCDEEPv20230713 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vmcdeepDetection VMCDEEPv20240506 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vvvDetection VVVDR1 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vvvDetection VVVDR2 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vvvDetection, vvvDetectionPawPrints, vvvDetectionTiles VVVDR5 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize

halfRad vvvDetection, vvvListRemeasurement VVVv20100531 r_h half-light radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} real 4 pixels -0.9999995e9 phys.angSize;src

hAperJky3 ultravistaSourceRemeasurement ULTRAVISTADR4 Default point source H aperture corrected (2.0 arcsec aperture diameter) calibrated flux
If in doubt use this flux estimator real 4 jansky -0.9999995e9 phot.flux

hAperJky3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Default point source H aperture corrected (2.0 arcsec aperture diameter) calibrated flux
If in doubt use this flux estimator real 4 jansky -0.9999995e9 phot.flux

hAperJky3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Default point source H aperture corrected (2.0 arcsec aperture diameter) calibrated flux
If in doubt use this flux estimator real 4 jansky -0.9999995e9 phot.flux

hAperJky3Err ultravistaSourceRemeasurement ULTRAVISTADR4 Error in default point/extended source H (2.0 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error

hAperJky3Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in default point/extended source H (2.0 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error

hAperJky3Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in default point/extended source H (2.0 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error

hAperJky4 ultravistaSourceRemeasurement ULTRAVISTADR4 Point source H aperture corrected (2.8 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 phot.flux

hAperJky4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Point source H aperture corrected (2.8 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 phot.flux

hAperJky4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Point source H aperture corrected (2.8 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 phot.flux

hAperJky4Err ultravistaSourceRemeasurement ULTRAVISTADR4 Error in point/extended source H (2.8 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error

hAperJky4Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in point/extended source H (2.8 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error

hAperJky4Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in point/extended source H (2.8 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error

hAperJky6 ultravistaSourceRemeasurement ULTRAVISTADR4 Point source H aperture corrected (5.7 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 phot.flux

hAperJky6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Point source H aperture corrected (5.7 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 phot.flux

hAperJky6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Point source H aperture corrected (5.7 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 phot.flux

hAperJky6Err ultravistaSourceRemeasurement ULTRAVISTADR4 Error in point/extended source H (5.7 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error

hAperJky6Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in point/extended source H (5.7 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error

hAperJky6Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in point/extended source H (5.7 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error

hAperJkyNoAperCorr3 ultravistaSourceRemeasurement ULTRAVISTADR4 Default extended source H (2.0 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux
If in doubt use this flux estimator real 4 jansky -0.9999995e9 phot.flux

hAperJkyNoAperCorr3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Default extended source H (2.0 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux
If in doubt use this flux estimator real 4 jansky -0.9999995e9 phot.flux

hAperJkyNoAperCorr3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Default extended source H (2.0 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux
If in doubt use this flux estimator real 4 jansky -0.9999995e9 phot.flux

hAperJkyNoAperCorr4 ultravistaSourceRemeasurement ULTRAVISTADR4 Extended source H (2.8 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux real 4 jansky -0.9999995e9 phot.flux

hAperJkyNoAperCorr4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Extended source H (2.8 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux real 4 jansky -0.9999995e9 phot.flux

hAperJkyNoAperCorr4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Extended source H (2.8 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux real 4 jansky -0.9999995e9 phot.flux

hAperJkyNoAperCorr6 ultravistaSourceRemeasurement ULTRAVISTADR4 Extended source H (5.7 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux real 4 jansky -0.9999995e9 phot.flux

hAperJkyNoAperCorr6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Extended source H (5.7 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux real 4 jansky -0.9999995e9 phot.flux

hAperJkyNoAperCorr6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Extended source H (5.7 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux real 4 jansky -0.9999995e9 phot.flux

hAperLup3 ultravistaSourceRemeasurement ULTRAVISTADR4 Default point source H aperture corrected (2.0 arcsec aperture diameter) luptitude
If in doubt use this flux estimator real 4 lup -0.9999995e9 phot.lup

hAperLup3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Default point source H aperture corrected (2.0 arcsec aperture diameter) luptitude
If in doubt use this flux estimator real 4 lup -0.9999995e9 phot.lup

hAperLup3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Default point source H aperture corrected (2.0 arcsec aperture diameter) luptitude
If in doubt use this flux estimator real 4 lup -0.9999995e9 phot.lup

hAperLup3Err ultravistaSourceRemeasurement ULTRAVISTADR4 Error in default point/extended source H (2.0 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error

hAperLup3Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in default point/extended source H (2.0 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error

hAperLup3Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in default point/extended source H (2.0 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error

hAperLup4 ultravistaSourceRemeasurement ULTRAVISTADR4 Point source H aperture corrected (2.8 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 phot.lup

hAperLup4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Point source H aperture corrected (2.8 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 phot.lup

hAperLup4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Point source H aperture corrected (2.8 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 phot.lup

hAperLup4Err ultravistaSourceRemeasurement ULTRAVISTADR4 Error in point/extended source H (2.8 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error

hAperLup4Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in point/extended source H (2.8 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error

hAperLup4Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in point/extended source H (2.8 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error

hAperLup6 ultravistaSourceRemeasurement ULTRAVISTADR4 Point source H aperture corrected (5.7 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 phot.lup

hAperLup6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Point source H aperture corrected (5.7 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 phot.lup

hAperLup6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Point source H aperture corrected (5.7 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 phot.lup

hAperLup6Err ultravistaSourceRemeasurement ULTRAVISTADR4 Error in point/extended source H (5.7 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error

hAperLup6Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in point/extended source H (5.7 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error

hAperLup6Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in point/extended source H (5.7 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error

hAperLupNoAperCorr3 ultravistaSourceRemeasurement ULTRAVISTADR4 Default extended source H (2.0 arcsec aperture diameter, but no aperture correction applied) aperture luptitude
If in doubt use this flux estimator real 4 lup -0.9999995e9 phot.lup

hAperLupNoAperCorr3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Default extended source H (2.0 arcsec aperture diameter, but no aperture correction applied) aperture luptitude
If in doubt use this flux estimator real 4 lup -0.9999995e9 phot.lup

hAperLupNoAperCorr3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Default extended source H (2.0 arcsec aperture diameter, but no aperture correction applied) aperture luptitude
If in doubt use this flux estimator real 4 lup -0.9999995e9 phot.lup

hAperLupNoAperCorr4 ultravistaSourceRemeasurement ULTRAVISTADR4 Extended source H (2.8 arcsec aperture diameter, but no aperture correction applied) aperture luptitude real 4 lup -0.9999995e9 phot.lup

hAperLupNoAperCorr4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Extended source H (2.8 arcsec aperture diameter, but no aperture correction applied) aperture luptitude real 4 lup -0.9999995e9 phot.lup

hAperLupNoAperCorr4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Extended source H (2.8 arcsec aperture diameter, but no aperture correction applied) aperture luptitude real 4 lup -0.9999995e9 phot.lup

hAperLupNoAperCorr6 ultravistaSourceRemeasurement ULTRAVISTADR4 Extended source H (5.7 arcsec aperture diameter, but no aperture correction applied) aperture luptitude real 4 lup -0.9999995e9 phot.lup

hAperLupNoAperCorr6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Extended source H (5.7 arcsec aperture diameter, but no aperture correction applied) aperture luptitude real 4 lup -0.9999995e9 phot.lup

hAperLupNoAperCorr6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Extended source H (5.7 arcsec aperture diameter, but no aperture correction applied) aperture luptitude real 4 lup -0.9999995e9 phot.lup

hAperMag1 vvvSource VVVDR1 Extended source H aperture corrected mag (0.7 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMag1 vvvSource VVVDR5 Point source H aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag1 vvvSource VVVv20100531 Extended source H aperture corrected mag (0.7 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMag1 vvvSource VVVv20110718 Extended source H aperture corrected mag (0.7 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMag1 vvvSource, vvvSynopticSource VVVDR2 Extended source H aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag1 vvvxSource VVVXDR1 Point source H aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag1Err vvvSource VVVDR1 Error in extended source H mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag1Err vvvSource VVVDR5 Error in point source H mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag1Err vvvSource VVVv20100531 Error in extended source H mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag1Err vvvSource VVVv20110718 Error in extended source H mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag1Err vvvSource, vvvSynopticSource VVVDR2 Error in extended source H mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag1Err vvvxSource VVVXDR1 Error in point source H mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag2 vvvSynopticSource VVVDR1 Extended source H aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag2 vvvSynopticSource VVVDR2 Extended source H aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag2Err vvvSynopticSource VVVDR1 Error in extended source H mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag2Err vvvSynopticSource VVVDR2 Error in extended source H mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag3 ultravistaSource ULTRAVISTADR4 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag3 ultravistaSourceRemeasurement ULTRAVISTADR4 Default point source H aperture corrected (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMag3 vhsSource VHSDR1 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMag3 vhsSource VHSDR2 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMag3 vhsSource VHSDR3 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag3 vhsSource VHSDR4 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag3 vhsSource VHSDR5 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag3 vhsSource VHSDR6 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag3 vhsSource VHSv20120926 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMag3 vhsSource VHSv20130417 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMag3 vhsSource VHSv20140409 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag3 vhsSource VHSv20150108 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag3 vhsSource VHSv20160114 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag3 vhsSource VHSv20160507 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag3 vhsSource VHSv20170630 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag3 vhsSource VHSv20180419 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag3 vhsSource VHSv20201209 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag3 vhsSource VHSv20231101 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag3 vhsSource VHSv20240731 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag3 videoSource VIDEODR2 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMag3 videoSource VIDEODR3 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMag3 videoSource VIDEODR4 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag3 videoSource VIDEODR5 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag3 videoSource VIDEOv20100513 Default point/extended source H mag, no aperture correction applied
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMag3 videoSource VIDEOv20111208 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMag3 vikingSource VIKINGDR2 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMag3 vikingSource VIKINGDR3 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMag3 vikingSource VIKINGDR4 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag3 vikingSource VIKINGv20110714 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMag3 vikingSource VIKINGv20111019 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMag3 vikingSource VIKINGv20130417 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMag3 vikingSource VIKINGv20140402 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag3 vikingSource VIKINGv20150421 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag3 vikingSource VIKINGv20151230 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag3 vikingSource VIKINGv20160406 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag3 vikingSource VIKINGv20161202 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag3 vikingSource VIKINGv20170715 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Default point source H aperture corrected (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMag3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Default point source H aperture corrected (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMag3 vvvSource VVVDR1 Default point/extended source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMag3 vvvSource VVVDR2 Default point/extended source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag3 vvvSource VVVDR5 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag3 vvvSource VVVv20100531 Default point/extended source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMag3 vvvSource VVVv20110718 Default point/extended source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMag3 vvvSynopticSource VVVDR1 Default point/extended source H aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag3 vvvSynopticSource VVVDR2 Default point/extended source H aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag3 vvvVivaCatalogue VVVDR5 H magnitude using aperture corrected mag (2.0 arcsec aperture diameter, from VVVDR4 1st epoch JHKs contemporaneous OB) {catalogue TType keyword: hAperMag3} real 4 mag -9.999995e8

hAperMag3 vvvxSource VVVXDR1 Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag3Err ultravistaSource ULTRAVISTADR4 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag3Err ultravistaSourceRemeasurement ULTRAVISTADR4 Error in default point/extended source H (2.0 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error

hAperMag3Err vhsSource VHSDR1 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag3Err vhsSource VHSDR2 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag3Err vhsSource VHSDR3 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.H

hAperMag3Err vhsSource VHSDR4 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.H;phot.mag

hAperMag3Err vhsSource VHSDR5 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag3Err vhsSource VHSDR6 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag3Err vhsSource VHSv20120926 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag3Err vhsSource VHSv20130417 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag3Err vhsSource VHSv20140409 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.H

hAperMag3Err vhsSource VHSv20150108 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.H;phot.mag

hAperMag3Err vhsSource VHSv20160114 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag3Err vhsSource VHSv20160507 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag3Err vhsSource VHSv20170630 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag3Err vhsSource VHSv20180419 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag3Err vhsSource VHSv20201209 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag3Err vhsSource VHSv20231101 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag3Err vhsSource VHSv20240731 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag3Err videoSource VIDEODR2 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag3Err videoSource VIDEODR3 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag3Err videoSource VIDEODR4 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.H;phot.mag

hAperMag3Err videoSource VIDEODR5 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.H;phot.mag

hAperMag3Err videoSource VIDEOv20100513 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag3Err videoSource VIDEOv20111208 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag3Err vikingSource VIKINGDR2 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag3Err vikingSource VIKINGDR3 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag3Err vikingSource VIKINGDR4 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.H

hAperMag3Err vikingSource VIKINGv20110714 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag3Err vikingSource VIKINGv20111019 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag3Err vikingSource VIKINGv20130417 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag3Err vikingSource VIKINGv20140402 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag3Err vikingSource VIKINGv20150421 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.H;phot.mag

hAperMag3Err vikingSource VIKINGv20151230 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag3Err vikingSource VIKINGv20160406 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag3Err vikingSource VIKINGv20161202 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag3Err vikingSource VIKINGv20170715 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag3Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in default point/extended source H (2.0 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error

hAperMag3Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in default point/extended source H (2.0 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error

hAperMag3Err vvvSource VVVDR2 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag3Err vvvSource VVVDR5 Error in default point source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag3Err vvvSource VVVv20100531 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag3Err vvvSource VVVv20110718 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag3Err vvvSource, vvvSynopticSource VVVDR1 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag3Err vvvVivaCatalogue VVVDR5 Error in default point source H mag, from VVVDR4 {catalogue TType keyword: hAperMag3Err} real 4 mag -9.999995e8

hAperMag3Err vvvxSource VVVXDR1 Error in default point source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag4 ultravistaSource ULTRAVISTADR4 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag4 ultravistaSourceRemeasurement ULTRAVISTADR4 Point source H aperture corrected (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag4 vhsSource VHSDR1 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag4 vhsSource VHSDR2 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag4 vhsSource VHSDR3 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag4 vhsSource VHSDR4 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag4 vhsSource VHSDR5 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag4 vhsSource VHSDR6 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag4 vhsSource VHSv20120926 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag4 vhsSource VHSv20130417 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag4 vhsSource VHSv20140409 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag4 vhsSource VHSv20150108 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag4 vhsSource VHSv20160114 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag4 vhsSource VHSv20160507 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag4 vhsSource VHSv20170630 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag4 vhsSource VHSv20180419 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag4 vhsSource VHSv20201209 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag4 vhsSource VHSv20231101 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag4 vhsSource VHSv20240731 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag4 videoSource VIDEODR2 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag4 videoSource VIDEODR3 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag4 videoSource VIDEODR4 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag4 videoSource VIDEODR5 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag4 videoSource VIDEOv20100513 Extended source H mag, no aperture correction applied real 4 mag -0.9999995e9 phot.mag

hAperMag4 videoSource VIDEOv20111208 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag4 vikingSource VIKINGDR2 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag4 vikingSource VIKINGDR3 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag4 vikingSource VIKINGDR4 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag4 vikingSource VIKINGv20110714 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag4 vikingSource VIKINGv20111019 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag4 vikingSource VIKINGv20130417 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag4 vikingSource VIKINGv20140402 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag4 vikingSource VIKINGv20150421 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag4 vikingSource VIKINGv20151230 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag4 vikingSource VIKINGv20160406 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag4 vikingSource VIKINGv20161202 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag4 vikingSource VIKINGv20170715 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Point source H aperture corrected (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Point source H aperture corrected (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag4 vvvSource VVVDR2 Extended source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag4 vvvSource VVVDR5 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag4 vvvSource VVVv20100531 Extended source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag4 vvvSource VVVv20110718 Extended source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag4 vvvSource, vvvSynopticSource VVVDR1 Extended source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag4 vvvxSource VVVXDR1 Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag4Err ultravistaSource ULTRAVISTADR4 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag4Err ultravistaSourceRemeasurement ULTRAVISTADR4 Error in point/extended source H (2.8 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error

hAperMag4Err vhsSource VHSDR1 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag4Err vhsSource VHSDR2 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag4Err vhsSource VHSDR3 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.H

hAperMag4Err vhsSource VHSDR4 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.H;phot.mag

hAperMag4Err vhsSource VHSDR5 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag4Err vhsSource VHSDR6 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag4Err vhsSource VHSv20120926 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag4Err vhsSource VHSv20130417 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag4Err vhsSource VHSv20140409 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.H

hAperMag4Err vhsSource VHSv20150108 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.H;phot.mag

hAperMag4Err vhsSource VHSv20160114 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag4Err vhsSource VHSv20160507 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag4Err vhsSource VHSv20170630 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag4Err vhsSource VHSv20180419 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag4Err vhsSource VHSv20201209 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag4Err vhsSource VHSv20231101 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag4Err vhsSource VHSv20240731 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag4Err videoSource VIDEODR2 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag4Err videoSource VIDEODR3 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag4Err videoSource VIDEODR4 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.H;phot.mag

hAperMag4Err videoSource VIDEODR5 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.H;phot.mag

hAperMag4Err videoSource VIDEOv20100513 Error in extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag4Err videoSource VIDEOv20111208 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag4Err vikingSource VIKINGDR2 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag4Err vikingSource VIKINGDR3 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag4Err vikingSource VIKINGDR4 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.H

hAperMag4Err vikingSource VIKINGv20110714 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag4Err vikingSource VIKINGv20111019 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag4Err vikingSource VIKINGv20130417 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag4Err vikingSource VIKINGv20140402 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag4Err vikingSource VIKINGv20150421 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.H;phot.mag

hAperMag4Err vikingSource VIKINGv20151230 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag4Err vikingSource VIKINGv20160406 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag4Err vikingSource VIKINGv20161202 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag4Err vikingSource VIKINGv20170715 Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag4Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in point/extended source H (2.8 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error

hAperMag4Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in point/extended source H (2.8 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error

hAperMag4Err vvvSource VVVDR2 Error in extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag4Err vvvSource VVVDR5 Error in point source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag4Err vvvSource VVVv20100531 Error in extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag4Err vvvSource VVVv20110718 Error in extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag4Err vvvSource, vvvSynopticSource VVVDR1 Error in extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag4Err vvvxSource VVVXDR1 Error in point source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag5 vvvSynopticSource VVVDR1 Extended source H aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag5 vvvSynopticSource VVVDR2 Extended source H aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag5Err vvvSynopticSource VVVDR1 Error in extended source H mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag5Err vvvSynopticSource VVVDR2 Error in extended source H mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag6 ultravistaSource ULTRAVISTADR4 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag6 ultravistaSourceRemeasurement ULTRAVISTADR4 Point source H aperture corrected (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag6 vhsSource VHSDR1 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag6 vhsSource VHSDR2 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag6 vhsSource VHSDR3 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag6 vhsSource VHSDR4 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag6 vhsSource VHSDR5 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag6 vhsSource VHSDR6 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag6 vhsSource VHSv20120926 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag6 vhsSource VHSv20130417 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag6 vhsSource VHSv20140409 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag6 vhsSource VHSv20150108 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag6 vhsSource VHSv20160114 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag6 vhsSource VHSv20160507 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag6 vhsSource VHSv20170630 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag6 vhsSource VHSv20180419 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag6 vhsSource VHSv20201209 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag6 vhsSource VHSv20231101 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag6 vhsSource VHSv20240731 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag6 videoSource VIDEODR2 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag6 videoSource VIDEODR3 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag6 videoSource VIDEODR4 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag6 videoSource VIDEODR5 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag6 videoSource VIDEOv20100513 Extended source H mag, no aperture correction applied real 4 mag -0.9999995e9 phot.mag

hAperMag6 videoSource VIDEOv20111208 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag6 vikingSource VIKINGDR2 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag6 vikingSource VIKINGDR3 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag6 vikingSource VIKINGDR4 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag6 vikingSource VIKINGv20110714 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag6 vikingSource VIKINGv20111019 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag6 vikingSource VIKINGv20130417 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag6 vikingSource VIKINGv20140402 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag6 vikingSource VIKINGv20150421 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag6 vikingSource VIKINGv20151230 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag6 vikingSource VIKINGv20160406 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag6 vikingSource VIKINGv20161202 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag6 vikingSource VIKINGv20170715 Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMag6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Point source H aperture corrected (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Point source H aperture corrected (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMag6Err ultravistaSource ULTRAVISTADR4 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag6Err ultravistaSourceRemeasurement ULTRAVISTADR4 Error in point/extended source H (5.7 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error

hAperMag6Err vhsSource VHSDR1 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag6Err vhsSource VHSDR2 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag6Err vhsSource VHSDR3 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.H

hAperMag6Err vhsSource VHSDR4 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.H;phot.mag

hAperMag6Err vhsSource VHSDR5 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag6Err vhsSource VHSDR6 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag6Err vhsSource VHSv20120926 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag6Err vhsSource VHSv20130417 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag6Err vhsSource VHSv20140409 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.H

hAperMag6Err vhsSource VHSv20150108 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.H;phot.mag

hAperMag6Err vhsSource VHSv20160114 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag6Err vhsSource VHSv20160507 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag6Err vhsSource VHSv20170630 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag6Err vhsSource VHSv20180419 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag6Err vhsSource VHSv20201209 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag6Err vhsSource VHSv20231101 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag6Err vhsSource VHSv20240731 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag6Err videoSource VIDEODR2 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag6Err videoSource VIDEODR3 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag6Err videoSource VIDEODR4 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.H;phot.mag

hAperMag6Err videoSource VIDEODR5 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.H;phot.mag

hAperMag6Err videoSource VIDEOv20100513 Error in extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag6Err videoSource VIDEOv20111208 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag6Err vikingSource VIKINGDR2 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag6Err vikingSource VIKINGDR3 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag6Err vikingSource VIKINGDR4 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.H

hAperMag6Err vikingSource VIKINGv20110714 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag6Err vikingSource VIKINGv20111019 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag6Err vikingSource VIKINGv20130417 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag6Err vikingSource VIKINGv20140402 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

hAperMag6Err vikingSource VIKINGv20150421 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.H;phot.mag

hAperMag6Err vikingSource VIKINGv20151230 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag6Err vikingSource VIKINGv20160406 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag6Err vikingSource VIKINGv20161202 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag6Err vikingSource VIKINGv20170715 Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hAperMag6Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in point/extended source H (5.7 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error

hAperMag6Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in point/extended source H (5.7 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error

hAperMagNoAperCorr3 ultravistaSource ULTRAVISTADR4 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr3 ultravistaSourceRemeasurement ULTRAVISTADR4 Default extended source H (2.0 arcsec aperture diameter, but no aperture correction applied) aperture magnitude
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr3 vhsSource VHSDR1 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr3 vhsSource VHSDR2 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr3 vhsSource VHSDR3 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr3 vhsSource VHSDR4 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr3 vhsSource VHSDR5 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr3 vhsSource VHSDR6 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr3 vhsSource VHSv20120926 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr3 vhsSource VHSv20130417 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr3 vhsSource VHSv20140409 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr3 vhsSource VHSv20150108 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr3 vhsSource VHSv20160114 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr3 vhsSource VHSv20160507 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr3 vhsSource VHSv20170630 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr3 vhsSource VHSv20180419 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr3 vhsSource VHSv20201209 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr3 vhsSource VHSv20231101 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr3 vhsSource VHSv20240731 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr3 videoSource VIDEODR2 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr3 videoSource VIDEODR3 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr3 videoSource VIDEODR4 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr3 videoSource VIDEODR5 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr3 videoSource VIDEOv20111208 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr3 vikingSource VIKINGDR2 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr3 vikingSource VIKINGDR3 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr3 vikingSource VIKINGDR4 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr3 vikingSource VIKINGv20110714 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr3 vikingSource VIKINGv20111019 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr3 vikingSource VIKINGv20130417 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr3 vikingSource VIKINGv20140402 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr3 vikingSource VIKINGv20150421 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr3 vikingSource VIKINGv20151230 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr3 vikingSource VIKINGv20160406 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr3 vikingSource VIKINGv20161202 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr3 vikingSource VIKINGv20170715 Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Default extended source H (2.0 arcsec aperture diameter, but no aperture correction applied) aperture magnitude
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Default extended source H (2.0 arcsec aperture diameter, but no aperture correction applied) aperture magnitude
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr4 ultravistaSource ULTRAVISTADR4 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr4 ultravistaSourceRemeasurement ULTRAVISTADR4 Extended source H (2.8 arcsec aperture diameter, but no aperture correction applied) aperture magnitude real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr4 vhsSource VHSDR1 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr4 vhsSource VHSDR2 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr4 vhsSource VHSDR3 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr4 vhsSource VHSDR4 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr4 vhsSource VHSDR5 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr4 vhsSource VHSDR6 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr4 vhsSource VHSv20120926 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr4 vhsSource VHSv20130417 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr4 vhsSource VHSv20140409 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr4 vhsSource VHSv20150108 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr4 vhsSource VHSv20160114 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr4 vhsSource VHSv20160507 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr4 vhsSource VHSv20170630 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr4 vhsSource VHSv20180419 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr4 vhsSource VHSv20201209 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr4 vhsSource VHSv20231101 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr4 vhsSource VHSv20240731 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr4 videoSource VIDEODR2 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr4 videoSource VIDEODR3 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr4 videoSource VIDEODR4 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr4 videoSource VIDEODR5 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr4 videoSource VIDEOv20111208 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr4 vikingSource VIKINGDR2 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr4 vikingSource VIKINGDR3 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr4 vikingSource VIKINGDR4 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr4 vikingSource VIKINGv20110714 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr4 vikingSource VIKINGv20111019 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr4 vikingSource VIKINGv20130417 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr4 vikingSource VIKINGv20140402 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr4 vikingSource VIKINGv20150421 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr4 vikingSource VIKINGv20151230 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr4 vikingSource VIKINGv20160406 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr4 vikingSource VIKINGv20161202 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr4 vikingSource VIKINGv20170715 Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Extended source H (2.8 arcsec aperture diameter, but no aperture correction applied) aperture magnitude real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Extended source H (2.8 arcsec aperture diameter, but no aperture correction applied) aperture magnitude real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr6 ultravistaSource ULTRAVISTADR4 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr6 ultravistaSourceRemeasurement ULTRAVISTADR4 Extended source H (5.7 arcsec aperture diameter, but no aperture correction applied) aperture magnitude real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr6 vhsSource VHSDR1 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr6 vhsSource VHSDR2 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr6 vhsSource VHSDR3 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr6 vhsSource VHSDR4 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr6 vhsSource VHSDR5 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr6 vhsSource VHSDR6 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr6 vhsSource VHSv20120926 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr6 vhsSource VHSv20130417 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr6 vhsSource VHSv20140409 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr6 vhsSource VHSv20150108 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr6 vhsSource VHSv20160114 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr6 vhsSource VHSv20160507 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr6 vhsSource VHSv20170630 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr6 vhsSource VHSv20180419 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr6 vhsSource VHSv20201209 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr6 vhsSource VHSv20231101 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr6 vhsSource VHSv20240731 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr6 videoSource VIDEODR2 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr6 videoSource VIDEODR3 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr6 videoSource VIDEODR4 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr6 videoSource VIDEODR5 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr6 videoSource VIDEOv20111208 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr6 vikingSource VIKINGDR2 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr6 vikingSource VIKINGDR3 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr6 vikingSource VIKINGDR4 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr6 vikingSource VIKINGv20110714 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr6 vikingSource VIKINGv20111019 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr6 vikingSource VIKINGv20130417 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr6 vikingSource VIKINGv20140402 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr6 vikingSource VIKINGv20150421 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr6 vikingSource VIKINGv20151230 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr6 vikingSource VIKINGv20160406 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr6 vikingSource VIKINGv20161202 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr6 vikingSource VIKINGv20170715 Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hAperMagNoAperCorr6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Extended source H (5.7 arcsec aperture diameter, but no aperture correction applied) aperture magnitude real 4 mag -0.9999995e9 phot.mag

hAperMagNoAperCorr6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Extended source H (5.7 arcsec aperture diameter, but no aperture correction applied) aperture magnitude real 4 mag -0.9999995e9 phot.mag

haStratAst ultravistaVarFrameSetInfo ULTRAVISTADR4 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in H band. real 4 -0.9999995e9 stat.fit.param;em.IR.H

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

haStratAst videoVarFrameSetInfo VIDEODR2 Strateva parameter, a, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

haStratAst videoVarFrameSetInfo VIDEODR3 Strateva parameter, a, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.NIR

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

haStratAst videoVarFrameSetInfo VIDEODR4 Strateva parameter, a, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.H

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

haStratAst videoVarFrameSetInfo VIDEODR5 Strateva parameter, a, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.H

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

haStratAst videoVarFrameSetInfo VIDEOv20100513 Strateva parameter, a, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

haStratAst videoVarFrameSetInfo VIDEOv20111208 Strateva parameter, a, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

haStratAst vikingVarFrameSetInfo VIKINGDR2 Strateva parameter, a, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

haStratAst vikingVarFrameSetInfo VIKINGv20110714 Strateva parameter, a, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

haStratAst vikingVarFrameSetInfo VIKINGv20111019 Strateva parameter, a, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

haStratAst vvvVarFrameSetInfo VVVDR5 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in H band. real 4 -0.9999995e9 stat.fit.param;em.IR.H

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

haStratAst vvvVarFrameSetInfo VVVv20100531 Strateva parameter, a, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

haStratPht ultravistaMapLcVarFrameSetInfo ULTRAVISTADR4 Strateva parameter, a, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.H

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

haStratPht ultravistaVarFrameSetInfo ULTRAVISTADR4 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in H band. real 4 -0.9999995e9 stat.fit.param;em.IR.H

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

haStratPht videoVarFrameSetInfo VIDEODR2 Strateva parameter, a, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

haStratPht videoVarFrameSetInfo VIDEODR3 Strateva parameter, a, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.NIR

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

haStratPht videoVarFrameSetInfo VIDEODR4 Strateva parameter, a, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.H

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

haStratPht videoVarFrameSetInfo VIDEODR5 Strateva parameter, a, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.H

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

haStratPht videoVarFrameSetInfo VIDEOv20100513 Strateva parameter, a, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

haStratPht videoVarFrameSetInfo VIDEOv20111208 Strateva parameter, a, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

haStratPht vikingVarFrameSetInfo VIKINGDR2 Strateva parameter, a, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

haStratPht vikingVarFrameSetInfo VIKINGv20110714 Strateva parameter, a, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

haStratPht vikingVarFrameSetInfo VIKINGv20111019 Strateva parameter, a, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

haStratPht vvvVarFrameSetInfo VVVDR5 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in H band. real 4 -0.9999995e9 stat.fit.param;em.IR.H

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

haStratPht vvvVarFrameSetInfo VVVv20100531 Strateva parameter, a, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hAverageConf ultravistaSourceRemeasurement ULTRAVISTADR4 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -0.9999995e9 stat.likelihood;em.IR.NIR

hAverageConf vhsSource VHSDR1 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -99999999 meta.code

hAverageConf vhsSource VHSDR2 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -99999999 meta.code

hAverageConf vhsSource VHSDR3 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -0.9999995e9 stat.likelihood;em.IR.H

hAverageConf vhsSource VHSDR4 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -0.9999995e9 stat.likelihood;em.IR.H

hAverageConf vhsSource VHSDR5 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -0.9999995e9 stat.likelihood;em.IR.H

hAverageConf vhsSource VHSDR6 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -0.9999995e9 stat.likelihood;em.IR.H

hAverageConf vhsSource VHSv20120926 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -99999999 stat.likelihood;em.IR.NIR

hAverageConf vhsSource VHSv20130417 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -0.9999995e9 stat.likelihood;em.IR.NIR

hAverageConf vhsSource VHSv20140409 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -0.9999995e9 stat.likelihood;em.IR.H

hAverageConf vhsSource VHSv20150108 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -0.9999995e9 stat.likelihood;em.IR.H

hAverageConf vhsSource VHSv20160114 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -0.9999995e9 stat.likelihood;em.IR.H

hAverageConf vhsSource VHSv20160507 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -0.9999995e9 stat.likelihood;em.IR.H

hAverageConf vhsSource VHSv20170630 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -0.9999995e9 stat.likelihood;em.IR.H

hAverageConf vhsSource VHSv20180419 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -0.9999995e9 stat.likelihood;em.IR.H

hAverageConf vhsSource VHSv20201209 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -0.9999995e9 stat.likelihood;em.IR.H

hAverageConf vhsSource VHSv20231101 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -0.9999995e9 stat.likelihood;em.IR.H

hAverageConf vhsSource VHSv20240731 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -0.9999995e9 stat.likelihood;em.IR.H

hAverageConf vikingSource VIKINGDR2 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -99999999 meta.code

hAverageConf vikingSource VIKINGDR3 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -99999999 stat.likelihood;em.IR.NIR

hAverageConf vikingSource VIKINGDR4 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -0.9999995e9 stat.likelihood;em.IR.H

hAverageConf vikingSource VIKINGv20110714 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -99999999 meta.code

hAverageConf vikingSource VIKINGv20111019 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -99999999 meta.code

hAverageConf vikingSource VIKINGv20130417 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -0.9999995e9 stat.likelihood;em.IR.NIR

hAverageConf vikingSource VIKINGv20140402 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -0.9999995e9 stat.likelihood;em.IR.NIR

hAverageConf vikingSource VIKINGv20150421 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -0.9999995e9 stat.likelihood;em.IR.H

hAverageConf vikingSource VIKINGv20151230 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -0.9999995e9 stat.likelihood;em.IR.H

hAverageConf vikingSource VIKINGv20160406 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -0.9999995e9 stat.likelihood;em.IR.H

hAverageConf vikingSource VIKINGv20161202 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -0.9999995e9 stat.likelihood;em.IR.H

hAverageConf vikingSource VIKINGv20170715 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -0.9999995e9 stat.likelihood;em.IR.H

hAverageConf vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -0.9999995e9 stat.likelihood;em.IR.NIR

hAverageConf vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -0.9999995e9 stat.likelihood;em.IR.NIR

hAverageConf vvvSource VVVDR2 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -0.9999995e9 stat.likelihood;em.IR.NIR

hAverageConf vvvSource VVVDR5 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -0.9999995e9 stat.likelihood;em.IR.H

hAverageConf vvvSource, vvvSynopticSource VVVDR1 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -99999999 stat.likelihood;em.IR.NIR

hAverageConf vvvxSource VVVXDR1 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -0.9999995e9 stat.likelihood;em.IR.H

hbestAper ultravistaMapLcVariability ULTRAVISTADR4 Best aperture (1-3) for photometric statistics in the H band int 4 -9999

Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)

hbestAper ultravistaVariability ULTRAVISTADR4 Best aperture (1-6) for photometric statistics in the H band int 4 -9999 meta.code.class;em.IR.H

Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)

hbestAper videoVariability VIDEODR2 Best aperture (1-6) for photometric statistics in the H band int 4 -9999

Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)

hbestAper videoVariability VIDEODR3 Best aperture (1-6) for photometric statistics in the H band int 4 -9999 meta.code.class;em.IR.NIR

Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)

hbestAper videoVariability VIDEODR4 Best aperture (1-6) for photometric statistics in the H band int 4 -9999 meta.code.class;em.IR.H

Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)

hbestAper videoVariability VIDEODR5 Best aperture (1-6) for photometric statistics in the H band int 4 -9999 meta.code.class;em.IR.H

Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)

hbestAper videoVariability VIDEOv20100513 Best aperture (1-6) for photometric statistics in the H band int 4 -9999

Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)

hbestAper videoVariability VIDEOv20111208 Best aperture (1-6) for photometric statistics in the H band int 4 -9999

Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)

hbestAper vikingVariability VIKINGDR2 Best aperture (1-6) for photometric statistics in the H band int 4 -9999

Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)

hbestAper vikingVariability VIKINGv20110714 Best aperture (1-6) for photometric statistics in the H band int 4 -9999

Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)

hbestAper vikingVariability VIKINGv20111019 Best aperture (1-6) for photometric statistics in the H band int 4 -9999

Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)

hbestAper vvvVariability VVVDR5 Best aperture (1-6) for photometric statistics in the H band int 4 -9999 meta.code.class;em.IR.H

Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)

hbestAper vvvVariability VVVv20100531 Best aperture (1-6) for photometric statistics in the H band int 4 -9999

Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)

hbStratAst ultravistaVarFrameSetInfo ULTRAVISTADR4 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in H band. real 4 -0.9999995e9 stat.fit.param;em.IR.H

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hbStratAst videoVarFrameSetInfo VIDEODR2 Strateva parameter, b, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hbStratAst videoVarFrameSetInfo VIDEODR3 Strateva parameter, b, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.NIR

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hbStratAst videoVarFrameSetInfo VIDEODR4 Strateva parameter, b, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.H

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hbStratAst videoVarFrameSetInfo VIDEODR5 Strateva parameter, b, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.H

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hbStratAst videoVarFrameSetInfo VIDEOv20100513 Strateva parameter, b, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hbStratAst videoVarFrameSetInfo VIDEOv20111208 Strateva parameter, b, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hbStratAst vikingVarFrameSetInfo VIKINGDR2 Strateva parameter, b, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hbStratAst vikingVarFrameSetInfo VIKINGv20110714 Strateva parameter, b, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hbStratAst vikingVarFrameSetInfo VIKINGv20111019 Strateva parameter, b, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hbStratAst vvvVarFrameSetInfo VVVDR5 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in H band. real 4 -0.9999995e9 stat.fit.param;em.IR.H

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hbStratAst vvvVarFrameSetInfo VVVv20100531 Strateva parameter, b, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hbStratPht ultravistaMapLcVarFrameSetInfo ULTRAVISTADR4 Strateva parameter, b, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.H

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hbStratPht ultravistaVarFrameSetInfo ULTRAVISTADR4 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in H band. real 4 -0.9999995e9 stat.fit.param;em.IR.H

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hbStratPht videoVarFrameSetInfo VIDEODR2 Strateva parameter, b, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hbStratPht videoVarFrameSetInfo VIDEODR3 Strateva parameter, b, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.NIR

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hbStratPht videoVarFrameSetInfo VIDEODR4 Strateva parameter, b, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.H

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hbStratPht videoVarFrameSetInfo VIDEODR5 Strateva parameter, b, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.H

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hbStratPht videoVarFrameSetInfo VIDEOv20100513 Strateva parameter, b, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hbStratPht videoVarFrameSetInfo VIDEOv20111208 Strateva parameter, b, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hbStratPht vikingVarFrameSetInfo VIKINGDR2 Strateva parameter, b, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hbStratPht vikingVarFrameSetInfo VIKINGv20110714 Strateva parameter, b, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hbStratPht vikingVarFrameSetInfo VIKINGv20111019 Strateva parameter, b, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hbStratPht vvvVarFrameSetInfo VVVDR5 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in H band. real 4 -0.9999995e9 stat.fit.param;em.IR.H

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hbStratPht vvvVarFrameSetInfo VVVv20100531 Strateva parameter, b, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hchiSqAst ultravistaVarFrameSetInfo ULTRAVISTADR4 Goodness of fit of Strateva function to astrometric data in H band real 4 -0.9999995e9 stat.fit.goodness;em.IR.H

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hchiSqAst videoVarFrameSetInfo VIDEODR2 Goodness of fit of Strateva function to astrometric data in H band real 4 -0.9999995e9

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hchiSqAst videoVarFrameSetInfo VIDEODR3 Goodness of fit of Strateva function to astrometric data in H band real 4 -0.9999995e9 stat.fit.goodness;em.IR.NIR

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hchiSqAst videoVarFrameSetInfo VIDEODR4 Goodness of fit of Strateva function to astrometric data in H band real 4 -0.9999995e9 stat.fit.goodness;em.IR.H

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hchiSqAst videoVarFrameSetInfo VIDEODR5 Goodness of fit of Strateva function to astrometric data in H band real 4 -0.9999995e9 stat.fit.goodness;em.IR.H

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hchiSqAst videoVarFrameSetInfo VIDEOv20100513 Goodness of fit of Strateva function to astrometric data in H band real 4 -0.9999995e9

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hchiSqAst videoVarFrameSetInfo VIDEOv20111208 Goodness of fit of Strateva function to astrometric data in H band real 4 -0.9999995e9

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hchiSqAst vikingVarFrameSetInfo VIKINGDR2 Goodness of fit of Strateva function to astrometric data in H band real 4 -0.9999995e9

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hchiSqAst vikingVarFrameSetInfo VIKINGv20110714 Goodness of fit of Strateva function to astrometric data in H band real 4 -0.9999995e9

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hchiSqAst vikingVarFrameSetInfo VIKINGv20111019 Goodness of fit of Strateva function to astrometric data in H band real 4 -0.9999995e9

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hchiSqAst vvvVarFrameSetInfo VVVDR5 Goodness of fit of Strateva function to astrometric data in H band real 4 -0.9999995e9 stat.fit.goodness;em.IR.H

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hchiSqAst vvvVarFrameSetInfo VVVv20100531 Goodness of fit of Strateva function to astrometric data in H band real 4 -0.9999995e9

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hchiSqpd ultravistaMapLcVariability ULTRAVISTADR4 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hchiSqpd ultravistaVariability ULTRAVISTADR4 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hchiSqpd videoVariability VIDEODR2 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hchiSqpd videoVariability VIDEODR3 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hchiSqpd videoVariability VIDEODR4 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hchiSqpd videoVariability VIDEODR5 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hchiSqpd videoVariability VIDEOv20100513 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hchiSqpd videoVariability VIDEOv20111208 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hchiSqpd vikingVariability VIKINGDR2 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hchiSqpd vikingVariability VIKINGv20110714 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hchiSqpd vikingVariability VIKINGv20111019 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hchiSqpd vvvVariability VVVDR5 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hchiSqpd vvvVariability VVVv20100531 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hchiSqPht ultravistaMapLcVarFrameSetInfo, ultravistaVarFrameSetInfo ULTRAVISTADR4 Goodness of fit of Strateva function to photometric data in H band real 4 -0.9999995e9 stat.fit.goodness;em.IR.H

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hchiSqPht videoVarFrameSetInfo VIDEODR2 Goodness of fit of Strateva function to photometric data in H band real 4 -0.9999995e9

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hchiSqPht videoVarFrameSetInfo VIDEODR3 Goodness of fit of Strateva function to photometric data in H band real 4 -0.9999995e9 stat.fit.goodness;em.IR.NIR

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hchiSqPht videoVarFrameSetInfo VIDEODR4 Goodness of fit of Strateva function to photometric data in H band real 4 -0.9999995e9 stat.fit.goodness;em.IR.H

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hchiSqPht videoVarFrameSetInfo VIDEODR5 Goodness of fit of Strateva function to photometric data in H band real 4 -0.9999995e9 stat.fit.goodness;em.IR.H

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hchiSqPht videoVarFrameSetInfo VIDEOv20100513 Goodness of fit of Strateva function to photometric data in H band real 4 -0.9999995e9

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hchiSqPht videoVarFrameSetInfo VIDEOv20111208 Goodness of fit of Strateva function to photometric data in H band real 4 -0.9999995e9

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hchiSqPht vikingVarFrameSetInfo VIKINGDR2 Goodness of fit of Strateva function to photometric data in H band real 4 -0.9999995e9

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hchiSqPht vikingVarFrameSetInfo VIKINGv20110714 Goodness of fit of Strateva function to photometric data in H band real 4 -0.9999995e9

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hchiSqPht vikingVarFrameSetInfo VIKINGv20111019 Goodness of fit of Strateva function to photometric data in H band real 4 -0.9999995e9

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hchiSqPht vvvVarFrameSetInfo VVVDR5 Goodness of fit of Strateva function to photometric data in H band real 4 -0.9999995e9 stat.fit.goodness;em.IR.H

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hchiSqPht vvvVarFrameSetInfo VVVv20100531 Goodness of fit of Strateva function to photometric data in H band real 4 -0.9999995e9

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

Hclass vvvParallaxCatalogue, vvvProperMotionCatalogue VVVDR5 VVV DR4 H morphological classification. 1 = galaxy,0 = noise,-1 = stellar,-2 = probably stellar,-3 = probable galaxy,-7 = bad pixel within 2" aperture,-9 = saturated {catalogue TType keyword: Hclass} int 4 -99999999

hClass ultravistaSource ULTRAVISTADR4 discrete image classification flag in H smallint 2 -9999 src.class;em.IR.H

hClass ultravistaSourceRemeasurement ULTRAVISTADR4 discrete image classification flag in H smallint 2 -9999 src.class

hClass vhsSource VHSDR2 discrete image classification flag in H smallint 2 -9999 src.class

hClass vhsSource VHSDR3 discrete image classification flag in H smallint 2 -9999 src.class;em.IR.H

hClass vhsSource VHSDR4 discrete image classification flag in H smallint 2 -9999 src.class;em.IR.H

hClass vhsSource VHSDR5 discrete image classification flag in H smallint 2 -9999 src.class;em.IR.H

hClass vhsSource VHSDR6 discrete image classification flag in H smallint 2 -9999 src.class;em.IR.H

hClass vhsSource VHSv20120926 discrete image classification flag in H smallint 2 -9999 src.class

hClass vhsSource VHSv20130417 discrete image classification flag in H smallint 2 -9999 src.class

hClass vhsSource VHSv20140409 discrete image classification flag in H smallint 2 -9999 src.class;em.IR.H

hClass vhsSource VHSv20150108 discrete image classification flag in H smallint 2 -9999 src.class;em.IR.H

hClass vhsSource VHSv20160114 discrete image classification flag in H smallint 2 -9999 src.class;em.IR.H

hClass vhsSource VHSv20160507 discrete image classification flag in H smallint 2 -9999 src.class;em.IR.H

hClass vhsSource VHSv20170630 discrete image classification flag in H smallint 2 -9999 src.class;em.IR.H

hClass vhsSource VHSv20180419 discrete image classification flag in H smallint 2 -9999 src.class;em.IR.H

hClass vhsSource VHSv20201209 discrete image classification flag in H smallint 2 -9999 src.class;em.IR.H

hClass vhsSource VHSv20231101 discrete image classification flag in H smallint 2 -9999 src.class;em.IR.H

hClass vhsSource VHSv20240731 discrete image classification flag in H smallint 2 -9999 src.class;em.IR.H

hClass vhsSource, vhsSourceRemeasurement VHSDR1 discrete image classification flag in H smallint 2 -9999 src.class

hClass videoSource VIDEODR2 discrete image classification flag in H smallint 2 -9999 src.class

hClass videoSource VIDEODR3 discrete image classification flag in H smallint 2 -9999 src.class

hClass videoSource VIDEODR4 discrete image classification flag in H smallint 2 -9999 src.class;em.IR.H

hClass videoSource VIDEODR5 discrete image classification flag in H smallint 2 -9999 src.class;em.IR.H

hClass videoSource VIDEOv20111208 discrete image classification flag in H smallint 2 -9999 src.class

hClass videoSource, videoSourceRemeasurement VIDEOv20100513 discrete image classification flag in H smallint 2 -9999 src.class

hClass vikingSource VIKINGDR2 discrete image classification flag in H smallint 2 -9999 src.class

hClass vikingSource VIKINGDR3 discrete image classification flag in H smallint 2 -9999 src.class

hClass vikingSource VIKINGDR4 discrete image classification flag in H smallint 2 -9999 src.class;em.IR.H

hClass vikingSource VIKINGv20111019 discrete image classification flag in H smallint 2 -9999 src.class

hClass vikingSource VIKINGv20130417 discrete image classification flag in H smallint 2 -9999 src.class

hClass vikingSource VIKINGv20140402 discrete image classification flag in H smallint 2 -9999 src.class

hClass vikingSource VIKINGv20150421 discrete image classification flag in H smallint 2 -9999 src.class;em.IR.H

hClass vikingSource VIKINGv20151230 discrete image classification flag in H smallint 2 -9999 src.class;em.IR.H

hClass vikingSource VIKINGv20160406 discrete image classification flag in H smallint 2 -9999 src.class;em.IR.H

hClass vikingSource VIKINGv20161202 discrete image classification flag in H smallint 2 -9999 src.class;em.IR.H

hClass vikingSource VIKINGv20170715 discrete image classification flag in H smallint 2 -9999 src.class;em.IR.H

hClass vikingSource, vikingSourceRemeasurement VIKINGv20110714 discrete image classification flag in H smallint 2 -9999 src.class

hClass vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 discrete image classification flag in H smallint 2 -9999 src.class

hClass vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 discrete image classification flag in H smallint 2 -9999 src.class

hClass vvvSource VVVDR2 discrete image classification flag in H smallint 2 -9999 src.class

hClass vvvSource VVVDR5 discrete image classification flag in H smallint 2 -9999 src.class;em.IR.H

hClass vvvSource VVVv20110718 discrete image classification flag in H smallint 2 -9999 src.class

hClass vvvSource, vvvSourceRemeasurement VVVv20100531 discrete image classification flag in H smallint 2 -9999 src.class

hClass vvvSource, vvvSynopticSource VVVDR1 discrete image classification flag in H smallint 2 -9999 src.class

hClass vvvxSource VVVXDR1 discrete image classification flag in H smallint 2 -9999 src.class;em.IR.H

hClassStat ultravistaSource ULTRAVISTADR4 S-Extractor classification statistic in H real 4 -0.9999995e9 stat;em.IR.H

hClassStat ultravistaSourceRemeasurement ULTRAVISTADR4 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat

hClassStat vhsSource VHSDR2 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat

hClassStat vhsSource VHSDR3 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat;em.IR.H

hClassStat vhsSource VHSDR4 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat;em.IR.H

hClassStat vhsSource VHSDR5 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat;em.IR.H

hClassStat vhsSource VHSDR6 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat;em.IR.H

hClassStat vhsSource VHSv20120926 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat

hClassStat vhsSource VHSv20130417 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat

hClassStat vhsSource VHSv20140409 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat;em.IR.H

hClassStat vhsSource VHSv20150108 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat;em.IR.H

hClassStat vhsSource VHSv20160114 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat;em.IR.H

hClassStat vhsSource VHSv20160507 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat;em.IR.H

hClassStat vhsSource VHSv20170630 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat;em.IR.H

hClassStat vhsSource VHSv20180419 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat;em.IR.H

hClassStat vhsSource VHSv20201209 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat;em.IR.H

hClassStat vhsSource VHSv20231101 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat;em.IR.H

hClassStat vhsSource VHSv20240731 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat;em.IR.H

hClassStat vhsSource, vhsSourceRemeasurement VHSDR1 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat

hClassStat videoSource VIDEODR2 S-Extractor classification statistic in H real 4 -0.9999995e9 stat

hClassStat videoSource VIDEODR3 S-Extractor classification statistic in H real 4 -0.9999995e9 stat

hClassStat videoSource VIDEODR4 S-Extractor classification statistic in H real 4 -0.9999995e9 stat;em.IR.H

hClassStat videoSource VIDEODR5 S-Extractor classification statistic in H real 4 -0.9999995e9 stat;em.IR.H

hClassStat videoSource VIDEOv20100513 S-Extractor classification statistic in H real 4 -0.9999995e9 stat

hClassStat videoSource VIDEOv20111208 S-Extractor classification statistic in H real 4 -0.9999995e9 stat

hClassStat videoSourceRemeasurement VIDEOv20100513 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat

hClassStat vikingSource VIKINGDR2 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat

hClassStat vikingSource VIKINGDR3 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat

hClassStat vikingSource VIKINGDR4 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat;em.IR.H

hClassStat vikingSource VIKINGv20111019 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat

hClassStat vikingSource VIKINGv20130417 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat

hClassStat vikingSource VIKINGv20140402 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat

hClassStat vikingSource VIKINGv20150421 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat;em.IR.H

hClassStat vikingSource VIKINGv20151230 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat;em.IR.H

hClassStat vikingSource VIKINGv20160406 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat;em.IR.H

hClassStat vikingSource VIKINGv20161202 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat;em.IR.H

hClassStat vikingSource VIKINGv20170715 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat;em.IR.H

hClassStat vikingSource, vikingSourceRemeasurement VIKINGv20110714 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat

hClassStat vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat

hClassStat vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat

hClassStat vvvSource VVVDR1 S-Extractor classification statistic in H real 4 -0.9999995e9 stat

hClassStat vvvSource VVVDR2 S-Extractor classification statistic in H real 4 -0.9999995e9 stat

hClassStat vvvSource VVVDR5 S-Extractor classification statistic in H real 4 -0.9999995e9 stat;em.IR.H

hClassStat vvvSource VVVv20100531 S-Extractor classification statistic in H real 4 -0.9999995e9 stat

hClassStat vvvSource VVVv20110718 S-Extractor classification statistic in H real 4 -0.9999995e9 stat

hClassStat vvvSourceRemeasurement VVVv20100531 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat

hClassStat vvvSourceRemeasurement VVVv20110718 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat

hClassStat vvvSynopticSource VVVDR1 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat

hClassStat vvvSynopticSource VVVDR2 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 stat

hClassStat vvvxSource VVVXDR1 S-Extractor classification statistic in H real 4 -0.9999995e9 stat;em.IR.H

hCorr twompzPhotoz TWOMPZ H 20mag/sq." isophotal fiducial ell. ap. magnitude with Galactic dust correction {image primary HDU keyword: Hcorr} real 4 mag -0.9999995e9 phot.mag;em.IR.H

hCorrErr twompzPhotoz TWOMPZ H 1-sigma uncertainty in 20mag/sq." aperture {image primary HDU keyword: h_msig_k20fe} real 4 mag -0.9999995e9

hcStratAst ultravistaVarFrameSetInfo ULTRAVISTADR4 Parameter, c2 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in H band. real 4 -0.9999995e9 stat.fit.param;em.IR.H

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hcStratAst videoVarFrameSetInfo VIDEODR2 Strateva parameter, c, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hcStratAst videoVarFrameSetInfo VIDEODR3 Strateva parameter, c, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.NIR

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hcStratAst videoVarFrameSetInfo VIDEODR4 Strateva parameter, c, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.H

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hcStratAst videoVarFrameSetInfo VIDEODR5 Strateva parameter, c, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.H

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hcStratAst videoVarFrameSetInfo VIDEOv20100513 Strateva parameter, c, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hcStratAst videoVarFrameSetInfo VIDEOv20111208 Strateva parameter, c, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hcStratAst vikingVarFrameSetInfo VIKINGDR2 Strateva parameter, c, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hcStratAst vikingVarFrameSetInfo VIKINGv20110714 Strateva parameter, c, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hcStratAst vikingVarFrameSetInfo VIKINGv20111019 Strateva parameter, c, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hcStratAst vvvVarFrameSetInfo VVVDR5 Parameter, c2 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in H band. real 4 -0.9999995e9 stat.fit.param;em.IR.H

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hcStratAst vvvVarFrameSetInfo VVVv20100531 Strateva parameter, c, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hcStratPht ultravistaMapLcVarFrameSetInfo ULTRAVISTADR4 Strateva parameter, c, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.H

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hcStratPht ultravistaVarFrameSetInfo ULTRAVISTADR4 Parameter, c2 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in H band. real 4 -0.9999995e9 stat.fit.param;em.IR.H

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hcStratPht videoVarFrameSetInfo VIDEODR2 Strateva parameter, c, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hcStratPht videoVarFrameSetInfo VIDEODR3 Strateva parameter, c, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.NIR

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hcStratPht videoVarFrameSetInfo VIDEODR4 Strateva parameter, c, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.H

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hcStratPht videoVarFrameSetInfo VIDEODR5 Strateva parameter, c, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.H

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hcStratPht videoVarFrameSetInfo VIDEOv20100513 Strateva parameter, c, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hcStratPht videoVarFrameSetInfo VIDEOv20111208 Strateva parameter, c, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hcStratPht vikingVarFrameSetInfo VIKINGDR2 Strateva parameter, c, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hcStratPht vikingVarFrameSetInfo VIKINGv20110714 Strateva parameter, c, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hcStratPht vikingVarFrameSetInfo VIKINGv20111019 Strateva parameter, c, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hcStratPht vvvVarFrameSetInfo VVVDR5 Parameter, c2 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in H band. real 4 -0.9999995e9 stat.fit.param;em.IR.H

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hcStratPht vvvVarFrameSetInfo VVVv20100531 Strateva parameter, c, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hDeblend vhsSourceRemeasurement VHSDR1 placeholder flag indicating parent/child relation in H int 4 -99999999 meta.code

hDeblend videoSource, videoSourceRemeasurement VIDEOv20100513 placeholder flag indicating parent/child relation in H int 4 -99999999 meta.code

hDeblend vikingSourceRemeasurement VIKINGv20110714 placeholder flag indicating parent/child relation in H int 4 -99999999 meta.code

hDeblend vikingSourceRemeasurement VIKINGv20111019 placeholder flag indicating parent/child relation in H int 4 -99999999 meta.code

hDeblend vvvSource VVVv20110718 placeholder flag indicating parent/child relation in H int 4 -99999999 meta.code

hDeblend vvvSource, vvvSourceRemeasurement VVVv20100531 placeholder flag indicating parent/child relation in H int 4 -99999999 meta.code

HEALPix ravedr5Source RAVE Hierarchical Equal-Area iso-Latitude Pixelisation value (N_side = 4096) bigint 8 meta.code

HeightLSG vvvVivaCatalogue VVVDR5 Height of FreqLSG considering LSG method {catalogue TType keyword: HeightLSG} float 8 ?? -9.999995e8

HeightPDM vvvVivaCatalogue VVVDR5 Height of FreqPDM considering PDM method {catalogue TType keyword: HeightPDM} float 8 ?? -9.999995e8

HeightPKfi2 vvvVivaCatalogue VVVDR5 Height of FreqPKfi2 using PK method {catalogue TType keyword: HeightPKfi2} float 8 ?? -9.999995e8

HeightPLfi2 vvvVivaCatalogue VVVDR5 Height of FreqPLfi2 considering PL method {catalogue TType keyword: HeightPLfi2} float 8 ?? -9.999995e8

HeightSTR vvvVivaCatalogue VVVDR5 Height of FreqSTR considering STR method {catalogue TType keyword: HeightSTR} float 8 ?? -9.999995e8

Hell vvvParallaxCatalogue, vvvProperMotionCatalogue VVVDR5 Ellipticity of the DR4 H detection. {catalogue TType keyword: Hell} real 4 -999999500.0

hEll ultravistaSource ULTRAVISTADR4 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity;em.IR.H

hEll ultravistaSourceRemeasurement ULTRAVISTADR4 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticty

hEll vhsSource VHSDR2 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity

hEll vhsSource VHSDR3 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity;em.IR.H

hEll vhsSource VHSDR4 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity;em.IR.H

hEll vhsSource VHSDR5 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity;em.IR.H

hEll vhsSource VHSDR6 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity;em.IR.H

hEll vhsSource VHSv20120926 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity

hEll vhsSource VHSv20130417 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity

hEll vhsSource VHSv20140409 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity;em.IR.H

hEll vhsSource VHSv20150108 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity;em.IR.H

hEll vhsSource VHSv20160114 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity;em.IR.H

hEll vhsSource VHSv20160507 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity;em.IR.H

hEll vhsSource VHSv20170630 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity;em.IR.H

hEll vhsSource VHSv20180419 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity;em.IR.H

hEll vhsSource VHSv20201209 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity;em.IR.H

hEll vhsSource VHSv20231101 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity;em.IR.H

hEll vhsSource VHSv20240731 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity;em.IR.H

hEll vhsSource, vhsSourceRemeasurement VHSDR1 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity

hEll videoSource VIDEODR2 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity

hEll videoSource VIDEODR3 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity

hEll videoSource VIDEODR4 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity;em.IR.H

hEll videoSource VIDEODR5 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity;em.IR.H

hEll videoSource VIDEOv20111208 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity

hEll videoSource, videoSourceRemeasurement VIDEOv20100513 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity

hEll vikingSource VIKINGDR2 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity

hEll vikingSource VIKINGDR3 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity

hEll vikingSource VIKINGDR4 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity;em.IR.H

hEll vikingSource VIKINGv20111019 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity

hEll vikingSource VIKINGv20130417 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity

hEll vikingSource VIKINGv20140402 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity

hEll vikingSource VIKINGv20150421 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity;em.IR.H

hEll vikingSource VIKINGv20151230 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity;em.IR.H

hEll vikingSource VIKINGv20160406 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity;em.IR.H

hEll vikingSource VIKINGv20161202 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity;em.IR.H

hEll vikingSource VIKINGv20170715 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity;em.IR.H

hEll vikingSource, vikingSourceRemeasurement VIKINGv20110714 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity

hEll vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity

hEll vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity

hEll vvvSource VVVDR2 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity

hEll vvvSource VVVDR5 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity;em.IR.H

hEll vvvSource VVVv20110718 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity

hEll vvvSource, vvvSourceRemeasurement VVVv20100531 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity

hEll vvvSource, vvvSynopticSource VVVDR1 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity

hEll vvvxSource VVVXDR1 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 src.ellipticity;em.IR.H

hemis twomass_psc TWOMASS Hemisphere code for the TWOMASS Observatory from which this source was observed. varchar 1 meta.code;obs

hemis twomass_scn TWOMASS Observatory from which data were obtained: "n" = north = Mt. Hopkins, "s" = south = Cerro Tololo. varchar 1 meta.code;obs

hemis twomass_sixx2_scn TWOMASS hemisphere (N/S) of observation varchar 1

hemis twomass_xsc TWOMASS hemisphere (N/S) of observation. "n" = North/Mt. Hopkins; "s" = South/CTIO. varchar 1 meta.code;obs

heNum ultravistaMergeLog, ultravistaRemeasMergeLog ULTRAVISTADR4 the extension number of this H frame tinyint 1 meta.number;em.IR.H

heNum vhsMergeLog VHSDR1 the extension number of this H frame tinyint 1 meta.number

heNum vhsMergeLog VHSDR2 the extension number of this H frame tinyint 1 meta.number

heNum vhsMergeLog VHSDR3 the extension number of this H frame tinyint 1 meta.number;em.IR.H

heNum vhsMergeLog VHSDR4 the extension number of this H frame tinyint 1 meta.number;em.IR.H

heNum vhsMergeLog VHSDR5 the extension number of this H frame tinyint 1 meta.number;em.IR.H

heNum vhsMergeLog VHSDR6 the extension number of this H frame tinyint 1 meta.number;em.IR.H

heNum vhsMergeLog VHSv20120926 the extension number of this H frame tinyint 1 meta.number

heNum vhsMergeLog VHSv20130417 the extension number of this H frame tinyint 1 meta.number

heNum vhsMergeLog VHSv20140409 the extension number of this H frame tinyint 1 meta.number;em.IR.H

heNum vhsMergeLog VHSv20150108 the extension number of this H frame tinyint 1 meta.number;em.IR.H

heNum vhsMergeLog VHSv20160114 the extension number of this H frame tinyint 1 meta.number;em.IR.H

heNum vhsMergeLog VHSv20160507 the extension number of this H frame tinyint 1 meta.number;em.IR.H

heNum vhsMergeLog VHSv20170630 the extension number of this H frame tinyint 1 meta.number;em.IR.H

heNum vhsMergeLog VHSv20180419 the extension number of this H frame tinyint 1 meta.number;em.IR.H

heNum vhsMergeLog VHSv20201209 the extension number of this H frame tinyint 1 meta.id;em.IR.H

heNum vhsMergeLog VHSv20231101 the extension number of this H frame tinyint 1 meta.id;em.IR.H

heNum vhsMergeLog VHSv20240731 the extension number of this H frame tinyint 1 meta.id;em.IR.H

heNum videoMergeLog VIDEODR2 the extension number of this H frame tinyint 1 meta.number

heNum videoMergeLog VIDEODR3 the extension number of this H frame tinyint 1 meta.number

heNum videoMergeLog VIDEODR4 the extension number of this H frame tinyint 1 meta.number;em.IR.H

heNum videoMergeLog VIDEODR5 the extension number of this H frame tinyint 1 meta.number;em.IR.H

heNum videoMergeLog VIDEOv20100513 the extension number of this H frame tinyint 1 meta.number

heNum videoMergeLog VIDEOv20111208 the extension number of this H frame tinyint 1 meta.number

heNum vikingMergeLog VIKINGDR2 the extension number of this H frame tinyint 1 meta.number

heNum vikingMergeLog VIKINGDR3 the extension number of this H frame tinyint 1 meta.number

heNum vikingMergeLog VIKINGDR4 the extension number of this H frame tinyint 1 meta.number;em.IR.H

heNum vikingMergeLog VIKINGv20110714 the extension number of this H frame tinyint 1 meta.number

heNum vikingMergeLog VIKINGv20111019 the extension number of this H frame tinyint 1 meta.number

heNum vikingMergeLog VIKINGv20130417 the extension number of this H frame tinyint 1 meta.number

heNum vikingMergeLog VIKINGv20140402 the extension number of this H frame tinyint 1 meta.number

heNum vikingMergeLog VIKINGv20150421 the extension number of this H frame tinyint 1 meta.number;em.IR.H

heNum vikingMergeLog VIKINGv20151230 the extension number of this H frame tinyint 1 meta.number;em.IR.H

heNum vikingMergeLog VIKINGv20160406 the extension number of this H frame tinyint 1 meta.number;em.IR.H

heNum vikingMergeLog VIKINGv20161202 the extension number of this H frame tinyint 1 meta.number;em.IR.H

heNum vikingMergeLog VIKINGv20170715 the extension number of this H frame tinyint 1 meta.number;em.IR.H

heNum vikingZY_selJ_RemeasMergeLog VIKINGZYSELJv20160909 the extension number of this H frame tinyint 1 meta.number

heNum vikingZY_selJ_RemeasMergeLog VIKINGZYSELJv20170124 the extension number of this H frame tinyint 1 meta.number

heNum vvvMergeLog VVVDR2 the extension number of this H frame tinyint 1 meta.number

heNum vvvMergeLog VVVDR5 the extension number of this H frame tinyint 1 meta.number;em.IR.H

heNum vvvMergeLog VVVv20100531 the extension number of this H frame tinyint 1 meta.number

heNum vvvMergeLog VVVv20110718 the extension number of this H frame tinyint 1 meta.number

heNum vvvMergeLog, vvvSynopticMergeLog VVVDR1 the extension number of this H frame tinyint 1 meta.number

heNum vvvxMergeLog VVVXDR1 the extension number of this H frame tinyint 1 meta.id;em.IR.H

hErrBits ultravistaSource ULTRAVISTADR4 processing warning/error bitwise flags in H int 4 -99999999 meta.code;em.IR.H

This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows:

Bit Flag Meaning

1 The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected).

2 The object was originally blended with another

4 At least one pixel is saturated (or very close to)

8 The object is truncated (too close to an image boundary)

16 Object's aperture data are incomplete or corrupted

32 Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters.

64 Memory overflow occurred during deblending

128 Memory overflow occurred during extraction

hErrBits ultravistaSourceRemeasurement ULTRAVISTADR4 processing warning/error bitwise flags in H int 4 -99999999 meta.code

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vhsSource VHSDR1 processing warning/error bitwise flags in H int 4 -99999999 meta.code

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vhsSource VHSDR2 processing warning/error bitwise flags in H int 4 -99999999 meta.code

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vhsSource VHSDR3 processing warning/error bitwise flags in H int 4 -99999999 meta.code;em.IR.H

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vhsSource VHSDR4 processing warning/error bitwise flags in H int 4 -99999999 meta.code;em.IR.H

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vhsSource VHSDR5 processing warning/error bitwise flags in H int 4 -99999999 meta.code;em.IR.H

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vhsSource VHSDR6 processing warning/error bitwise flags in H int 4 -99999999 meta.code;em.IR.H

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vhsSource VHSv20120926 processing warning/error bitwise flags in H int 4 -99999999 meta.code

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vhsSource VHSv20130417 processing warning/error bitwise flags in H int 4 -99999999 meta.code

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vhsSource VHSv20140409 processing warning/error bitwise flags in H int 4 -99999999 meta.code;em.IR.H

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vhsSource VHSv20150108 processing warning/error bitwise flags in H int 4 -99999999 meta.code;em.IR.H

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vhsSource VHSv20160114 processing warning/error bitwise flags in H int 4 -99999999 meta.code;em.IR.H

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vhsSource VHSv20160507 processing warning/error bitwise flags in H int 4 -99999999 meta.code;em.IR.H

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vhsSource VHSv20170630 processing warning/error bitwise flags in H int 4 -99999999 meta.code;em.IR.H

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vhsSource VHSv20180419 processing warning/error bitwise flags in H int 4 -99999999 meta.code;em.IR.H

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vhsSource VHSv20201209 processing warning/error bitwise flags in H int 4 -99999999 meta.code;em.IR.H

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vhsSource VHSv20231101 processing warning/error bitwise flags in H int 4 -99999999 meta.code;em.IR.H

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vhsSource VHSv20240731 processing warning/error bitwise flags in H int 4 -99999999 meta.code;em.IR.H

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vhsSourceRemeasurement VHSDR1 processing warning/error bitwise flags in H int 4 -99999999 meta.code

hErrBits videoSource VIDEODR2 processing warning/error bitwise flags in H int 4 -99999999 meta.code

This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows:

Bit Flag Meaning

1 The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected).

2 The object was originally blended with another

4 At least one pixel is saturated (or very close to)

8 The object is truncated (too close to an image boundary)

16 Object's aperture data are incomplete or corrupted

32 Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters.

64 Memory overflow occurred during deblending

128 Memory overflow occurred during extraction

hErrBits videoSource VIDEODR3 processing warning/error bitwise flags in H int 4 -99999999 meta.code

This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows:

Bit Flag Meaning

1 The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected).

2 The object was originally blended with another

4 At least one pixel is saturated (or very close to)

8 The object is truncated (too close to an image boundary)

16 Object's aperture data are incomplete or corrupted

32 Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters.

64 Memory overflow occurred during deblending

128 Memory overflow occurred during extraction

hErrBits videoSource VIDEODR4 processing warning/error bitwise flags in H int 4 -99999999 meta.code;em.IR.H

This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows:

Bit Flag Meaning

1 The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected).

2 The object was originally blended with another

4 At least one pixel is saturated (or very close to)

8 The object is truncated (too close to an image boundary)

16 Object's aperture data are incomplete or corrupted

32 Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters.

64 Memory overflow occurred during deblending

128 Memory overflow occurred during extraction

hErrBits videoSource VIDEODR5 processing warning/error bitwise flags in H int 4 -99999999 meta.code;em.IR.H

This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows:

Bit Flag Meaning

1 The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected).

2 The object was originally blended with another

4 At least one pixel is saturated (or very close to)

8 The object is truncated (too close to an image boundary)

16 Object's aperture data are incomplete or corrupted

32 Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters.

64 Memory overflow occurred during deblending

128 Memory overflow occurred during extraction

hErrBits videoSource VIDEOv20100513 processing warning/error bitwise flags in H int 4 -99999999 meta.code

This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows:

Bit Flag Meaning

1 The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected).

2 The object was originally blended with another

4 At least one pixel is saturated (or very close to)

8 The object is truncated (too close to an image boundary)

16 Object's aperture data are incomplete or corrupted

32 Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters.

64 Memory overflow occurred during deblending

128 Memory overflow occurred during extraction

hErrBits videoSource VIDEOv20111208 processing warning/error bitwise flags in H int 4 -99999999 meta.code

This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows:

Bit Flag Meaning

1 The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected).

2 The object was originally blended with another

4 At least one pixel is saturated (or very close to)

8 The object is truncated (too close to an image boundary)

16 Object's aperture data are incomplete or corrupted

32 Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters.

64 Memory overflow occurred during deblending

128 Memory overflow occurred during extraction

hErrBits videoSourceRemeasurement VIDEOv20100513 processing warning/error bitwise flags in H int 4 -99999999 meta.code

hErrBits vikingSource VIKINGDR2 processing warning/error bitwise flags in H int 4 -99999999 meta.code

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vikingSource VIKINGDR3 processing warning/error bitwise flags in H int 4 -99999999 meta.code

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vikingSource VIKINGDR4 processing warning/error bitwise flags in H int 4 -99999999 meta.code;em.IR.H

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vikingSource VIKINGv20110714 processing warning/error bitwise flags in H int 4 -99999999 meta.code

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vikingSource VIKINGv20111019 processing warning/error bitwise flags in H int 4 -99999999 meta.code

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vikingSource VIKINGv20130417 processing warning/error bitwise flags in H int 4 -99999999 meta.code

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vikingSource VIKINGv20140402 processing warning/error bitwise flags in H int 4 -99999999 meta.code

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vikingSource VIKINGv20150421 processing warning/error bitwise flags in H int 4 -99999999 meta.code;em.IR.H

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vikingSource VIKINGv20151230 processing warning/error bitwise flags in H int 4 -99999999 meta.code;em.IR.H

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vikingSource VIKINGv20160406 processing warning/error bitwise flags in H int 4 -99999999 meta.code;em.IR.H

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vikingSource VIKINGv20161202 processing warning/error bitwise flags in H int 4 -99999999 meta.code;em.IR.H

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vikingSource VIKINGv20170715 processing warning/error bitwise flags in H int 4 -99999999 meta.code;em.IR.H

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vikingSourceRemeasurement VIKINGv20110714 processing warning/error bitwise flags in H int 4 -99999999 meta.code

hErrBits vikingSourceRemeasurement VIKINGv20111019 processing warning/error bitwise flags in H int 4 -99999999 meta.code

hErrBits vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 processing warning/error bitwise flags in H int 4 -99999999 meta.code

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 processing warning/error bitwise flags in H int 4 -99999999 meta.code

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vvvSource VVVDR2 processing warning/error bitwise flags in H int 4 -99999999 meta.code

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vvvSource VVVDR5 processing warning/error bitwise flags in H int 4 -99999999 meta.code;em.IR.H

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vvvSource VVVv20100531 processing warning/error bitwise flags in H int 4 -99999999 meta.code

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vvvSource VVVv20110718 processing warning/error bitwise flags in H int 4 -99999999 meta.code

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vvvSource, vvvSynopticSource VVVDR1 processing warning/error bitwise flags in H int 4 -99999999 meta.code

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vvvSourceRemeasurement VVVv20100531 processing warning/error bitwise flags in H int 4 -99999999 meta.code

hErrBits vvvSourceRemeasurement VVVv20110718 processing warning/error bitwise flags in H int 4 -99999999 meta.code

hErrBits vvvxSource VVVXDR1 processing warning/error bitwise flags in H int 4 -99999999 meta.code;em.IR.H

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hEta ultravistaSource ULTRAVISTADR4 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vhsSource VHSDR1 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vhsSource VHSDR2 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vhsSource VHSDR3 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vhsSource VHSDR4 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vhsSource VHSDR5 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vhsSource VHSDR6 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vhsSource VHSv20120926 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vhsSource VHSv20130417 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vhsSource VHSv20140409 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vhsSource VHSv20150108 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vhsSource VHSv20160114 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vhsSource VHSv20160507 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vhsSource VHSv20170630 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vhsSource VHSv20180419 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vhsSource VHSv20201209 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vhsSource VHSv20231101 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vhsSource VHSv20240731 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta videoSource VIDEODR2 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta videoSource VIDEODR3 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta videoSource VIDEODR4 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta videoSource VIDEODR5 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta videoSource VIDEOv20100513 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta videoSource VIDEOv20111208 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vikingSource VIKINGDR2 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vikingSource VIKINGDR3 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vikingSource VIKINGDR4 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vikingSource VIKINGv20110714 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vikingSource VIKINGv20111019 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vikingSource VIKINGv20130417 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vikingSource VIKINGv20140402 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vikingSource VIKINGv20150421 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vikingSource VIKINGv20151230 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vikingSource VIKINGv20160406 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vikingSource VIKINGv20161202 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vikingSource VIKINGv20170715 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vvvSource VVVDR2 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vvvSource VVVDR5 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vvvSource VVVv20100531 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vvvSource VVVv20110718 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vvvSource, vvvSynopticSource VVVDR1 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hEta vvvxSource VVVXDR1 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hexpML ultravistaMapLcVarFrameSetInfo, ultravistaVarFrameSetInfo ULTRAVISTADR4 Expected magnitude limit of frameSet in this in H band. real 4 mag -0.9999995e9 phot.mag;em.IR.H;stat.max

hexpML videoVarFrameSetInfo VIDEODR2 Expected magnitude limit of frameSet in this in H band. real 4 -0.9999995e9

hexpML videoVarFrameSetInfo VIDEODR3 Expected magnitude limit of frameSet in this in H band. real 4 -0.9999995e9 phot.mag;stat.max;em.IR.NIR

hexpML videoVarFrameSetInfo VIDEODR4 Expected magnitude limit of frameSet in this in H band. real 4 mag -0.9999995e9 phot.mag;em.IR.H;stat.max

hexpML videoVarFrameSetInfo VIDEODR5 Expected magnitude limit of frameSet in this in H band. real 4 mag -0.9999995e9 phot.mag;em.IR.H;stat.max

hexpML videoVarFrameSetInfo VIDEOv20100513 Expected magnitude limit of frameSet in this in H band. real 4 -0.9999995e9

hexpML videoVarFrameSetInfo VIDEOv20111208 Expected magnitude limit of frameSet in this in H band. real 4 -0.9999995e9

hexpML vikingVarFrameSetInfo VIKINGDR2 Expected magnitude limit of frameSet in this in H band. real 4 -0.9999995e9

hexpML vikingVarFrameSetInfo VIKINGv20110714 Expected magnitude limit of frameSet in this in H band. real 4 -0.9999995e9

hexpML vikingVarFrameSetInfo VIKINGv20111019 Expected magnitude limit of frameSet in this in H band. real 4 -0.9999995e9

hexpML vvvVarFrameSetInfo VVVDR5 Expected magnitude limit of frameSet in this in H band. real 4 mag -0.9999995e9 phot.mag;em.IR.H;stat.max

hexpML vvvVarFrameSetInfo VVVv20100531 Expected magnitude limit of frameSet in this in H band. real 4 -0.9999995e9

hExpRms ultravistaMapLcVariability ULTRAVISTADR4 Rms calculated from polynomial fit to modal RMS as a function of magnitude in H band real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hExpRms ultravistaVariability ULTRAVISTADR4 Rms calculated from polynomial fit to modal RMS as a function of magnitude in H band real 4 mag -0.9999995e9 stat.error;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hExpRms videoVariability VIDEODR2 Rms calculated from polynomial fit to modal RMS as a function of magnitude in H band real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hExpRms videoVariability VIDEODR3 Rms calculated from polynomial fit to modal RMS as a function of magnitude in H band real 4 mag -0.9999995e9 stat.error;em.IR.NIR

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hExpRms videoVariability VIDEODR4 Rms calculated from polynomial fit to modal RMS as a function of magnitude in H band real 4 mag -0.9999995e9 stat.error;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hExpRms videoVariability VIDEODR5 Rms calculated from polynomial fit to modal RMS as a function of magnitude in H band real 4 mag -0.9999995e9 stat.error;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hExpRms videoVariability VIDEOv20100513 Rms calculated from polynomial fit to modal RMS as a function of magnitude in H band real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hExpRms videoVariability VIDEOv20111208 Rms calculated from polynomial fit to modal RMS as a function of magnitude in H band real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hExpRms vikingVariability VIKINGDR2 Rms calculated from polynomial fit to modal RMS as a function of magnitude in H band real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hExpRms vikingVariability VIKINGv20110714 Rms calculated from polynomial fit to modal RMS as a function of magnitude in H band real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hExpRms vikingVariability VIKINGv20111019 Rms calculated from polynomial fit to modal RMS as a function of magnitude in H band real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hExpRms vvvVariability VVVDR5 Rms calculated from polynomial fit to modal RMS as a function of magnitude in H band real 4 mag -0.9999995e9 stat.error;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hExpRms vvvVariability VVVv20100531 Rms calculated from polynomial fit to modal RMS as a function of magnitude in H band real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hGausig ultravistaSource ULTRAVISTADR4 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param;em.IR.H

hGausig ultravistaSourceRemeasurement ULTRAVISTADR4 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param

hGausig vhsSource VHSDR2 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param

hGausig vhsSource VHSDR3 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param;em.IR.H

hGausig vhsSource VHSDR4 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param;em.IR.H

hGausig vhsSource VHSDR5 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param;em.IR.H

hGausig vhsSource VHSDR6 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param;em.IR.H

hGausig vhsSource VHSv20120926 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param

hGausig vhsSource VHSv20130417 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param

hGausig vhsSource VHSv20140409 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param;em.IR.H

hGausig vhsSource VHSv20150108 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param;em.IR.H

hGausig vhsSource VHSv20160114 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param;em.IR.H

hGausig vhsSource VHSv20160507 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param;em.IR.H

hGausig vhsSource VHSv20170630 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param;em.IR.H

hGausig vhsSource VHSv20180419 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param;em.IR.H

hGausig vhsSource VHSv20201209 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param;em.IR.H

hGausig vhsSource VHSv20231101 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param;em.IR.H

hGausig vhsSource VHSv20240731 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param;em.IR.H

hGausig vhsSource, vhsSourceRemeasurement VHSDR1 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param

hGausig videoSource VIDEODR2 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param

hGausig videoSource VIDEODR3 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param

hGausig videoSource VIDEODR4 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param;em.IR.H

hGausig videoSource VIDEODR5 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param;em.IR.H

hGausig videoSource VIDEOv20111208 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param

hGausig videoSource, videoSourceRemeasurement VIDEOv20100513 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param

hGausig vikingSource VIKINGDR2 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param

hGausig vikingSource VIKINGDR3 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param

hGausig vikingSource VIKINGDR4 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param;em.IR.H

hGausig vikingSource VIKINGv20111019 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param

hGausig vikingSource VIKINGv20130417 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param

hGausig vikingSource VIKINGv20140402 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param

hGausig vikingSource VIKINGv20150421 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param;em.IR.H

hGausig vikingSource VIKINGv20151230 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param;em.IR.H

hGausig vikingSource VIKINGv20160406 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param;em.IR.H

hGausig vikingSource VIKINGv20161202 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param;em.IR.H

hGausig vikingSource VIKINGv20170715 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param;em.IR.H

hGausig vikingSource, vikingSourceRemeasurement VIKINGv20110714 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param

hGausig vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param

hGausig vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param

hGausig vvvSource VVVDR2 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param

hGausig vvvSource VVVDR5 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param;em.IR.H

hGausig vvvSource VVVv20110718 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param

hGausig vvvSource, vvvSourceRemeasurement VVVv20100531 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param

hGausig vvvSource, vvvSynopticSource VVVDR1 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param

hGausig vvvxSource VVVXDR1 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 src.morph.param;em.IR.H

hgl twomass_scn TWOMASS Special flag indicating whether or not this scan has a single-frame H-band electronic glitch. smallint 2 meta.code

hgl twomass_sixx2_scn TWOMASS single-frame H-band glitch flag (0:not found|1:found) smallint 2

hHalfRad ultravistaSource ULTRAVISTADR4 SExtractor half-light radius in H band real 4 pixels -0.9999995e9 phys.angSize;em.IR.H

hHalfRad videoSource VIDEODR4 SExtractor half-light radius in H band real 4 pixels -0.9999995e9 phys.angSize;em.IR.H

hHalfRad videoSource VIDEODR5 SExtractor half-light radius in H band real 4 pixels -0.9999995e9 phys.angSize;em.IR.H

hHlCorSMjRadAs ultravistaSource ULTRAVISTADR4 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize;em.IR.H

hHlCorSMjRadAs ultravistaSourceRemeasurement ULTRAVISTADR4 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize

hHlCorSMjRadAs vhsSource VHSDR1 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize;src

hHlCorSMjRadAs vhsSource VHSDR2 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize;src

hHlCorSMjRadAs vhsSource VHSDR3 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize;em.IR.H

hHlCorSMjRadAs vhsSource VHSDR4 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize;em.IR.H

hHlCorSMjRadAs vhsSource VHSDR5 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize;em.IR.H

hHlCorSMjRadAs vhsSource VHSDR6 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize;em.IR.H

hHlCorSMjRadAs vhsSource VHSv20120926 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize

hHlCorSMjRadAs vhsSource VHSv20130417 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize

hHlCorSMjRadAs vhsSource VHSv20140409 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize;em.IR.H

hHlCorSMjRadAs vhsSource VHSv20150108 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize;em.IR.H

hHlCorSMjRadAs vhsSource VHSv20160114 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize;em.IR.H

hHlCorSMjRadAs vhsSource VHSv20160507 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize;em.IR.H

hHlCorSMjRadAs vhsSource VHSv20170630 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize;em.IR.H

hHlCorSMjRadAs vhsSource VHSv20180419 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize;em.IR.H

hHlCorSMjRadAs vhsSource VHSv20201209 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize;em.IR.H

hHlCorSMjRadAs vhsSource VHSv20231101 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize;em.IR.H

hHlCorSMjRadAs vhsSource VHSv20240731 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize;em.IR.H

hHlCorSMjRadAs videoSource VIDEODR2 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize;src

hHlCorSMjRadAs videoSource VIDEODR3 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize

hHlCorSMjRadAs videoSource VIDEODR4 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize;em.IR.H

hHlCorSMjRadAs videoSource VIDEODR5 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize;em.IR.H

hHlCorSMjRadAs videoSource VIDEOv20100513 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize;src

hHlCorSMjRadAs videoSource VIDEOv20111208 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize;src

hHlCorSMjRadAs vikingSource VIKINGDR2 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize;src

hHlCorSMjRadAs vikingSource VIKINGDR3 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize

hHlCorSMjRadAs vikingSource VIKINGDR4 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize;em.IR.H

hHlCorSMjRadAs vikingSource VIKINGv20110714 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize;src

hHlCorSMjRadAs vikingSource VIKINGv20111019 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize;src

hHlCorSMjRadAs vikingSource VIKINGv20130417 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize

hHlCorSMjRadAs vikingSource VIKINGv20140402 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize

hHlCorSMjRadAs vikingSource VIKINGv20150421 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize;em.IR.H

hHlCorSMjRadAs vikingSource VIKINGv20151230 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize;em.IR.H

hHlCorSMjRadAs vikingSource VIKINGv20160406 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize;em.IR.H

hHlCorSMjRadAs vikingSource VIKINGv20161202 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize;em.IR.H

hHlCorSMjRadAs vikingSource VIKINGv20170715 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 phys.angSize;em.IR.H

HIGH_BACKGROUND xmm3dr4 XMM The flag is set to 1 (= True) if this detection comes from a field which, during manual screening, was considered to have a high background level which notably impacted on source detection. bit 1

hIntRms ultravistaMapLcVariability ULTRAVISTADR4 Intrinsic rms in H-band real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hIntRms ultravistaVariability ULTRAVISTADR4 Intrinsic rms in H-band real 4 mag -0.9999995e9 stat.error;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hIntRms videoVariability VIDEODR2 Intrinsic rms in H-band real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hIntRms videoVariability VIDEODR3 Intrinsic rms in H-band real 4 mag -0.9999995e9 stat.error;em.IR.NIR

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hIntRms videoVariability VIDEODR4 Intrinsic rms in H-band real 4 mag -0.9999995e9 stat.error;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hIntRms videoVariability VIDEODR5 Intrinsic rms in H-band real 4 mag -0.9999995e9 stat.error;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hIntRms videoVariability VIDEOv20100513 Intrinsic rms in H-band real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hIntRms videoVariability VIDEOv20111208 Intrinsic rms in H-band real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hIntRms vikingVariability VIKINGDR2 Intrinsic rms in H-band real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hIntRms vikingVariability VIKINGv20110714 Intrinsic rms in H-band real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hIntRms vikingVariability VIKINGv20111019 Intrinsic rms in H-band real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hIntRms vvvVariability VVVDR5 Intrinsic rms in H-band real 4 mag -0.9999995e9 stat.error;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hIntRms vvvVariability VVVv20100531 Intrinsic rms in H-band real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hip hipparcos_new_reduction GAIADR1 Hipparcos identifier int 4 meta.main;meta.id

hip tgas_source GAIADR1 Hipparcos identifier int 4 id.cross

hip tycho2 GAIADR1 Hipparcos number varchar 16 meta.id.cross

hip_tyc_oid gaia_hip_tycho2_match GAIADR1 Initial Gaia Source List identifier for Hipparcos/Tycho2 bigint 8 id.cross

hisDefAst ultravistaVarFrameSetInfo ULTRAVISTADR4 Use a default model for the astrometric noise in H band. tinyint 1 0 meta.code;em.IR.H

hisDefAst videoVarFrameSetInfo VIDEODR2 Use a default model for the astrometric noise in H band. tinyint 1 0

hisDefAst videoVarFrameSetInfo VIDEODR3 Use a default model for the astrometric noise in H band. tinyint 1 0 meta.code;em.IR.NIR

hisDefAst videoVarFrameSetInfo VIDEODR4 Use a default model for the astrometric noise in H band. tinyint 1 0 meta.code;em.IR.H

hisDefAst videoVarFrameSetInfo VIDEODR5 Use a default model for the astrometric noise in H band. tinyint 1 0 meta.code;em.IR.H

hisDefAst videoVarFrameSetInfo VIDEOv20111208 Use a default model for the astrometric noise in H band. tinyint 1 0

hisDefAst vikingVarFrameSetInfo VIKINGDR2 Use a default model for the astrometric noise in H band. tinyint 1 0

hisDefAst vikingVarFrameSetInfo VIKINGv20111019 Use a default model for the astrometric noise in H band. tinyint 1 0

hisDefAst vvvVarFrameSetInfo VVVDR5 Use a default model for the astrometric noise in H band. tinyint 1 0 meta.code;em.IR.H

hisDefPht ultravistaMapLcVarFrameSetInfo, ultravistaVarFrameSetInfo ULTRAVISTADR4 Use a default model for the photometric noise in H band. tinyint 1 0 meta.code;em.IR.H

hisDefPht videoVarFrameSetInfo VIDEODR2 Use a default model for the photometric noise in H band. tinyint 1 0

hisDefPht videoVarFrameSetInfo VIDEODR3 Use a default model for the photometric noise in H band. tinyint 1 0 meta.code;em.IR.NIR

hisDefPht videoVarFrameSetInfo VIDEODR4 Use a default model for the photometric noise in H band. tinyint 1 0 meta.code;em.IR.H

hisDefPht videoVarFrameSetInfo VIDEODR5 Use a default model for the photometric noise in H band. tinyint 1 0 meta.code;em.IR.H

hisDefPht videoVarFrameSetInfo VIDEOv20111208 Use a default model for the photometric noise in H band. tinyint 1 0

hisDefPht vikingVarFrameSetInfo VIKINGDR2 Use a default model for the photometric noise in H band. tinyint 1 0

hisDefPht vikingVarFrameSetInfo VIKINGv20111019 Use a default model for the photometric noise in H band. tinyint 1 0

hisDefPht vvvVarFrameSetInfo VVVDR5 Use a default model for the photometric noise in H band. tinyint 1 0 meta.code;em.IR.H

hIsMeas ultravistaSourceRemeasurement ULTRAVISTADR4 Is pass band H measured? 0 no, 1 yes tinyint 1 0 meta.code

hIsMeas vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Is pass band H measured? 0 no, 1 yes tinyint 1 0 meta.code

hIsMeas vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Is pass band H measured? 0 no, 1 yes tinyint 1 0 meta.code

hKronJky ultravistaSourceRemeasurement ULTRAVISTADR4 Extended source H calibrated flux (Kron) real 4 jansky -0.9999995e9 phot.flux

hKronJkyErr ultravistaSourceRemeasurement ULTRAVISTADR4 Error in extended source H calibrated flux (Kron) real 4 janksy -0.9999995e9 stat.error

hKronLup ultravistaSourceRemeasurement ULTRAVISTADR4 Extended source H luptitude (Kron) real 4 lup -0.9999995e9 phot.lup

hKronLupErr ultravistaSourceRemeasurement ULTRAVISTADR4 Error in extended source H luptitude (Kron) real 4 lup -0.9999995e9 stat.error

hKronMag ultravistaSource ULTRAVISTADR4 Extended source H mag (Kron - SExtractor MAG_AUTO) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hKronMag ultravistaSourceRemeasurement ULTRAVISTADR4 Extended source H magnitude (Kron) real 4 mag -0.9999995e9 phot.mag

hKronMag videoSource VIDEODR4 Extended source H mag (Kron - SExtractor MAG_AUTO) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hKronMag videoSource VIDEODR5 Extended source H mag (Kron - SExtractor MAG_AUTO) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hKronMagErr ultravistaSource ULTRAVISTADR4 Extended source H mag error (Kron - SExtractor MAG_AUTO) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hKronMagErr ultravistaSourceRemeasurement ULTRAVISTADR4 Error in extended source H magnitude (Kron) real 4 mag -0.9999995e9 stat.error

hKronMagErr videoSource VIDEODR4 Extended source H mag error (Kron - SExtractor MAG_AUTO) real 4 mag -0.9999995e9 stat.error;em.IR.H;phot.mag

hKronMagErr videoSource VIDEODR5 Extended source H mag error (Kron - SExtractor MAG_AUTO) real 4 mag -0.9999995e9 stat.error;em.IR.H;phot.mag

hlCircRadAs sharksDetection SHARKSv20210222 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs sharksDetection SHARKSv20210421 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs ultravistaDetection ULTRAVISTADR4 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs ultravistaMapRemeasurement ULTRAVISTADR4 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total (CASU: default) real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vhsDetection VHSDR1 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize;src

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vhsDetection VHSDR2 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize;src

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vhsDetection VHSDR3 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vhsDetection VHSDR4 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vhsDetection VHSDR5 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vhsDetection VHSDR6 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vhsDetection VHSv20120926 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vhsDetection VHSv20130417 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vhsDetection VHSv20140409 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vhsDetection VHSv20150108 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vhsDetection VHSv20160114 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vhsDetection VHSv20160507 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vhsDetection VHSv20170630 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vhsDetection VHSv20180419 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vhsDetection VHSv20201209 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vhsDetection VHSv20231101 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vhsDetection VHSv20240731 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vhsListRemeasurement VHSDR1 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total flux real 4 arcsec -0.9999995e9 phys.angSize;src

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs videoDetection VIDEODR2 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize;src

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs videoDetection VIDEODR3 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs videoDetection VIDEODR4 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs videoDetection VIDEODR5 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs videoDetection VIDEOv20100513 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize;src

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs videoDetection VIDEOv20111208 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize;src

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs videoListRemeasurement VIDEOv20100513 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total flux real 4 arcsec -0.9999995e9 phys.angSize;src

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vikingDetection VIKINGDR2 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize;src

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vikingDetection VIKINGDR3 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vikingDetection VIKINGDR4 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vikingDetection VIKINGv20110714 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize;src

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vikingDetection VIKINGv20111019 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize;src

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vikingDetection VIKINGv20130417 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vikingDetection VIKINGv20140402 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vikingDetection VIKINGv20150421 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vikingDetection VIKINGv20151230 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vikingDetection VIKINGv20160406 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vikingDetection VIKINGv20161202 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vikingDetection VIKINGv20170715 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vikingListRemeasurement VIKINGv20110714 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total flux real 4 arcsec -0.9999995e9 phys.angSize;src

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vikingListRemeasurement VIKINGv20111019 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total flux real 4 arcsec -0.9999995e9 phys.angSize;src

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vikingMapRemeasurement VIKINGZYSELJv20160909 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total (CASU: default) real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vikingMapRemeasurement VIKINGZYSELJv20170124 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total (CASU: default) real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vmcdeepDetection VMCDEEPv20230713 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadAs vmcdeepDetection VMCDEEPv20240506 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs sharksDetection SHARKSv20210222 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs sharksDetection SHARKSv20210421 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs ultravistaDetection ULTRAVISTADR4 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs ultravistaMapRemeasurement ULTRAVISTADR4 Error in hlCircRadAs (CASU: default) real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs vhsDetection VHSDR2 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize;src

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs vhsDetection VHSDR3 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs vhsDetection VHSDR4 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs vhsDetection VHSDR5 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs vhsDetection VHSDR6 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs vhsDetection VHSv20120926 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs vhsDetection VHSv20130417 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs vhsDetection VHSv20140409 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs vhsDetection VHSv20150108 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs vhsDetection VHSv20160114 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs vhsDetection VHSv20160507 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs vhsDetection VHSv20170630 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs vhsDetection VHSv20180419 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs vhsDetection VHSv20201209 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs vhsDetection VHSv20231101 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs vhsDetection VHSv20240731 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs vhsDetection, vhsListRemeasurement VHSDR1 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize;src

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs videoDetection VIDEODR2 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize;src

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs videoDetection VIDEODR3 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs videoDetection VIDEODR4 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs videoDetection VIDEODR5 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs videoDetection VIDEOv20111208 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize;src

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs videoDetection, videoListRemeasurement VIDEOv20100513 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize;src

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs vikingDetection VIKINGDR2 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize;src

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs vikingDetection VIKINGDR3 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs vikingDetection VIKINGDR4 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs vikingDetection VIKINGv20111019 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize;src

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs vikingDetection VIKINGv20130417 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs vikingDetection VIKINGv20140402 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs vikingDetection VIKINGv20150421 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs vikingDetection VIKINGv20151230 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs vikingDetection VIKINGv20160406 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs vikingDetection VIKINGv20161202 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs vikingDetection VIKINGv20170715 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs vikingDetection, vikingListRemeasurement VIKINGv20110714 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize;src

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs vikingMapRemeasurement VIKINGZYSELJv20160909 Error in hlCircRadAs (CASU: default) real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs vikingMapRemeasurement VIKINGZYSELJv20170124 Error in hlCircRadAs (CASU: default) real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs vmcdeepDetection VMCDEEPv20230713 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCircRadErrAs vmcdeepDetection VMCDEEPv20240506 Error in hlCircRadAs real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMjRadAs sharksDetection SHARKSv20210222 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMjRadAs sharksDetection SHARKSv20210421 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMjRadAs ultravistaDetection ULTRAVISTADR4 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMjRadAs ultravistaMapRemeasurement ULTRAVISTADR4 Seeing corrected Half-light semi-major axis (CASU: default) real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMjRadAs vhsDetection VHSDR1 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9

hlCorSMjRadAs vhsDetection VHSDR2 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9

hlCorSMjRadAs vhsDetection VHSDR3 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMjRadAs vhsDetection VHSDR4 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMjRadAs vhsDetection VHSDR5 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMjRadAs vhsDetection VHSDR6 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMjRadAs vhsDetection VHSv20120926 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMjRadAs vhsDetection VHSv20130417 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMjRadAs vhsDetection VHSv20140409 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMjRadAs vhsDetection VHSv20150108 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMjRadAs vhsDetection VHSv20160114 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMjRadAs vhsDetection VHSv20160507 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMjRadAs vhsDetection VHSv20170630 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMjRadAs vhsDetection VHSv20180419 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMjRadAs vhsDetection VHSv20201209 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMjRadAs vhsDetection VHSv20231101 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMjRadAs vhsDetection VHSv20240731 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMjRadAs vhsListRemeasurement VHSDR1 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMjRadAs videoDetection VIDEODR2 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9

hlCorSMjRadAs videoDetection VIDEODR3 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMjRadAs videoDetection VIDEODR4 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMjRadAs videoDetection VIDEODR5 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMjRadAs videoDetection VIDEOv20100513 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9

hlCorSMjRadAs videoDetection VIDEOv20111208 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9

hlCorSMjRadAs videoListRemeasurement VIDEOv20100513 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMjRadAs vikingDetection VIKINGDR2 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9

hlCorSMjRadAs vikingDetection VIKINGDR3 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMjRadAs vikingDetection VIKINGDR4 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMjRadAs vikingDetection VIKINGv20110714 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9

hlCorSMjRadAs vikingDetection VIKINGv20111019 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9

hlCorSMjRadAs vikingDetection VIKINGv20130417 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMjRadAs vikingDetection VIKINGv20140402 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMjRadAs vikingDetection VIKINGv20150421 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMjRadAs vikingDetection VIKINGv20151230 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMjRadAs vikingDetection VIKINGv20160406 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMjRadAs vikingDetection VIKINGv20161202 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMjRadAs vikingDetection VIKINGv20170715 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMjRadAs vikingListRemeasurement VIKINGv20110714 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMjRadAs vikingListRemeasurement VIKINGv20111019 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMjRadAs vikingMapRemeasurement VIKINGZYSELJv20160909 Seeing corrected Half-light semi-major axis (CASU: default) real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMjRadAs vikingMapRemeasurement VIKINGZYSELJv20170124 Seeing corrected Half-light semi-major axis (CASU: default) real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMjRadAs vmcdeepDetection VMCDEEPv20230713 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMjRadAs vmcdeepDetection VMCDEEPv20240506 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMnRadAs sharksDetection SHARKSv20210222 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs sharksDetection SHARKSv20210421 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs ultravistaDetection ULTRAVISTADR4 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs ultravistaMapRemeasurement ULTRAVISTADR4 Seeing corrected Half-light semi-minor axis (CASU: default) real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs vhsDetection VHSDR2 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs vhsDetection VHSDR3 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs vhsDetection VHSDR4 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs vhsDetection VHSDR5 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs vhsDetection VHSDR6 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs vhsDetection VHSv20120926 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs vhsDetection VHSv20130417 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs vhsDetection VHSv20140409 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs vhsDetection VHSv20150108 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs vhsDetection VHSv20160114 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs vhsDetection VHSv20160507 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs vhsDetection VHSv20170630 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs vhsDetection VHSv20180419 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs vhsDetection VHSv20201209 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs vhsDetection VHSv20231101 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs vhsDetection VHSv20240731 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs vhsDetection, vhsListRemeasurement VHSDR1 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs videoDetection VIDEODR2 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs videoDetection VIDEODR3 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs videoDetection VIDEODR4 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs videoDetection VIDEODR5 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs videoDetection VIDEOv20111208 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs videoDetection, videoListRemeasurement VIDEOv20100513 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs vikingDetection VIKINGDR2 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs vikingDetection VIKINGDR3 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs vikingDetection VIKINGDR4 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs vikingDetection VIKINGv20111019 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs vikingDetection VIKINGv20130417 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs vikingDetection VIKINGv20140402 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs vikingDetection VIKINGv20150421 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs vikingDetection VIKINGv20151230 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs vikingDetection VIKINGv20160406 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs vikingDetection VIKINGv20161202 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs vikingDetection VIKINGv20170715 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs vikingDetection, vikingListRemeasurement VIKINGv20110714 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs vikingMapRemeasurement VIKINGZYSELJv20160909 Seeing corrected Half-light semi-minor axis (CASU: default) real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs vikingMapRemeasurement VIKINGZYSELJv20170124 Seeing corrected Half-light semi-minor axis (CASU: default) real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs vmcdeepDetection VMCDEEPv20230713 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlCorSMnRadAs vmcdeepDetection VMCDEEPv20240506 Seeing corrected Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs sharksDetection SHARKSv20210222 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs sharksDetection SHARKSv20210421 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs ultravistaDetection ULTRAVISTADR4 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs ultravistaMapRemeasurement ULTRAVISTADR4 Geometric half-light radius (CASU: default) real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs vhsDetection VHSDR2 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize;src

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs vhsDetection VHSDR3 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs vhsDetection VHSDR4 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs vhsDetection VHSDR5 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs vhsDetection VHSDR6 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs vhsDetection VHSv20120926 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs vhsDetection VHSv20130417 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs vhsDetection VHSv20140409 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs vhsDetection VHSv20150108 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs vhsDetection VHSv20160114 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs vhsDetection VHSv20160507 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs vhsDetection VHSv20170630 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs vhsDetection VHSv20180419 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs vhsDetection VHSv20201209 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs vhsDetection VHSv20231101 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs vhsDetection VHSv20240731 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs vhsDetection, vhsListRemeasurement VHSDR1 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize;src

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs videoDetection VIDEODR2 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize;src

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs videoDetection VIDEODR3 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs videoDetection VIDEODR4 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs videoDetection VIDEODR5 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs videoDetection VIDEOv20111208 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize;src

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs videoDetection, videoListRemeasurement VIDEOv20100513 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize;src

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs vikingDetection VIKINGDR2 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize;src

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs vikingDetection VIKINGDR3 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs vikingDetection VIKINGDR4 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs vikingDetection VIKINGv20111019 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize;src

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs vikingDetection VIKINGv20130417 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs vikingDetection VIKINGv20140402 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs vikingDetection VIKINGv20150421 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs vikingDetection VIKINGv20151230 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs vikingDetection VIKINGv20160406 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs vikingDetection VIKINGv20161202 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs vikingDetection VIKINGv20170715 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs vikingDetection, vikingListRemeasurement VIKINGv20110714 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize;src

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs vikingMapRemeasurement VIKINGZYSELJv20160909 Geometric half-light radius (CASU: default) real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs vikingMapRemeasurement VIKINGZYSELJv20170124 Geometric half-light radius (CASU: default) real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs vmcdeepDetection VMCDEEPv20230713 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlGeoRadAs vmcdeepDetection VMCDEEPv20240506 Geometric half-light radius real 4 arcsec -0.9999995e9 phys.angSize

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

HLRADIUS mgcBrightSpec MGC Semi-major axis of half-light ellipse real 4 pixel

hlSMjRadAs sharksDetection SHARKSv20210222 Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs sharksDetection SHARKSv20210421 Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs ultravistaDetection ULTRAVISTADR4 Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs ultravistaMapRemeasurement ULTRAVISTADR4 Half-light semi-major axis (CASU: default) real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs vhsDetection VHSDR2 Half-light semi-major axis real 4 arcsec -0.9999995e9

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs vhsDetection VHSDR3 Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs vhsDetection VHSDR4 Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs vhsDetection VHSDR5 Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs vhsDetection VHSDR6 Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs vhsDetection VHSv20120926 Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs vhsDetection VHSv20130417 Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs vhsDetection VHSv20140409 Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs vhsDetection VHSv20150108 Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs vhsDetection VHSv20160114 Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs vhsDetection VHSv20160507 Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs vhsDetection VHSv20170630 Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs vhsDetection VHSv20180419 Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs vhsDetection VHSv20201209 Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs vhsDetection VHSv20231101 Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs vhsDetection VHSv20240731 Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs vhsDetection, vhsListRemeasurement VHSDR1 Half-light semi-major axis real 4 arcsec -0.9999995e9

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs videoDetection VIDEODR2 Half-light semi-major axis real 4 arcsec -0.9999995e9

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs videoDetection VIDEODR3 Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs videoDetection VIDEODR4 Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs videoDetection VIDEODR5 Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs videoDetection VIDEOv20111208 Half-light semi-major axis real 4 arcsec -0.9999995e9

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs videoDetection, videoListRemeasurement VIDEOv20100513 Half-light semi-major axis real 4 arcsec -0.9999995e9

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs vikingDetection VIKINGDR2 Half-light semi-major axis real 4 arcsec -0.9999995e9

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs vikingDetection VIKINGDR3 Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs vikingDetection VIKINGDR4 Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs vikingDetection VIKINGv20111019 Half-light semi-major axis real 4 arcsec -0.9999995e9

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs vikingDetection VIKINGv20130417 Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs vikingDetection VIKINGv20140402 Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs vikingDetection VIKINGv20150421 Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs vikingDetection VIKINGv20151230 Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs vikingDetection VIKINGv20160406 Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs vikingDetection VIKINGv20161202 Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs vikingDetection VIKINGv20170715 Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs vikingDetection, vikingListRemeasurement VIKINGv20110714 Half-light semi-major axis real 4 arcsec -0.9999995e9

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs vikingMapRemeasurement VIKINGZYSELJv20160909 Half-light semi-major axis (CASU: default) real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs vikingMapRemeasurement VIKINGZYSELJv20170124 Half-light semi-major axis (CASU: default) real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs vmcdeepDetection VMCDEEPv20230713 Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMjRadAs vmcdeepDetection VMCDEEPv20240506 Half-light semi-major axis real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs sharksDetection SHARKSv20210222 Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs sharksDetection SHARKSv20210421 Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs ultravistaDetection ULTRAVISTADR4 Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs ultravistaMapRemeasurement ULTRAVISTADR4 Half-light semi-minor axis (CASU: default) real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs vhsDetection VHSDR2 Half-light semi-minor axis real 4 arcsec -0.9999995e9

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs vhsDetection VHSDR3 Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs vhsDetection VHSDR4 Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs vhsDetection VHSDR5 Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs vhsDetection VHSDR6 Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs vhsDetection VHSv20120926 Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs vhsDetection VHSv20130417 Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs vhsDetection VHSv20140409 Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs vhsDetection VHSv20150108 Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs vhsDetection VHSv20160114 Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs vhsDetection VHSv20160507 Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs vhsDetection VHSv20170630 Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs vhsDetection VHSv20180419 Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs vhsDetection VHSv20201209 Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs vhsDetection VHSv20231101 Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs vhsDetection VHSv20240731 Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs vhsDetection, vhsListRemeasurement VHSDR1 Half-light semi-minor axis real 4 arcsec -0.9999995e9

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs videoDetection VIDEODR2 Half-light semi-minor axis real 4 arcsec -0.9999995e9

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs videoDetection VIDEODR3 Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs videoDetection VIDEODR4 Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs videoDetection VIDEODR5 Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs videoDetection VIDEOv20111208 Half-light semi-minor axis real 4 arcsec -0.9999995e9

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs videoDetection, videoListRemeasurement VIDEOv20100513 Half-light semi-minor axis real 4 arcsec -0.9999995e9

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs vikingDetection VIKINGDR2 Half-light semi-minor axis real 4 arcsec -0.9999995e9

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs vikingDetection VIKINGDR3 Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs vikingDetection VIKINGDR4 Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs vikingDetection VIKINGv20111019 Half-light semi-minor axis real 4 arcsec -0.9999995e9

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs vikingDetection VIKINGv20130417 Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs vikingDetection VIKINGv20140402 Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs vikingDetection VIKINGv20150421 Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs vikingDetection VIKINGv20151230 Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs vikingDetection VIKINGv20160406 Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs vikingDetection VIKINGv20161202 Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs vikingDetection VIKINGv20170715 Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs vikingDetection, vikingListRemeasurement VIKINGv20110714 Half-light semi-minor axis real 4 arcsec -0.9999995e9

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs vikingMapRemeasurement VIKINGZYSELJv20160909 Half-light semi-minor axis (CASU: default) real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs vikingMapRemeasurement VIKINGZYSELJv20170124 Half-light semi-minor axis (CASU: default) real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs vmcdeepDetection VMCDEEPv20230713 Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

hlSMnRadAs vmcdeepDetection VMCDEEPv20240506 Half-light semi-minor axis real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1-ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature.

Hmag mcps_lmcSource, mcps_smcSource MCPS The H band magnitude (from 2MASS) (0.00 if star not detected.) real 4 mag

Hmag vvvParallaxCatalogue, vvvProperMotionCatalogue VVVDR5 VVV DR4 H photometry {catalogue TType keyword: Hmag} real 4 mag -999999500.0

hMag ukirtFSstars VIDEOv20100513 H band total magnitude on the MKO(UFTI) system real 4 mag phot.mag

hMag ukirtFSstars VIKINGv20110714 H band total magnitude on the MKO(UFTI) system real 4 mag phot.mag

hMag ukirtFSstars VVVv20100531 H band total magnitude on the MKO(UFTI) system real 4 mag phot.mag

hMag vhsSourceRemeasurement VHSDR1 H mag (as appropriate for this merged source) real 4 mag -0.9999995e9 phot.mag

hMag videoSourceRemeasurement VIDEOv20100513 H mag (as appropriate for this merged source) real 4 mag -0.9999995e9 phot.mag

hMag vikingSourceRemeasurement VIKINGv20110714 H mag (as appropriate for this merged source) real 4 mag -0.9999995e9 phot.mag

hMag vikingSourceRemeasurement VIKINGv20111019 H mag (as appropriate for this merged source) real 4 mag -0.9999995e9 phot.mag

hMag vvvSourceRemeasurement VVVv20100531 H mag (as appropriate for this merged source) real 4 mag -0.9999995e9 phot.mag

hMag vvvSourceRemeasurement VVVv20110718 H mag (as appropriate for this merged source) real 4 mag -0.9999995e9 phot.mag

Hmag2MASS spitzer_smcSource SPITZER The 2MASS H band magnitude. real 4 mag

Hmag_2MASS ravedr5Source RAVE H selected default magnitude from 2MASS real 4 mag magnitude phot.mag;em.IR.H

hMagErr ukirtFSstars VIDEOv20100513 H band magnitude error real 4 mag stat.error

hMagErr ukirtFSstars VIKINGv20110714 H band magnitude error real 4 mag stat.error

hMagErr ukirtFSstars VVVv20100531 H band magnitude error real 4 mag stat.error

hMagErr vhsSourceRemeasurement VHSDR1 Error in H mag real 4 mag -0.9999995e9 stat.error

hMagErr videoSourceRemeasurement VIDEOv20100513 Error in H mag real 4 mag -0.9999995e9 stat.error

hMagErr vikingSourceRemeasurement VIKINGv20110714 Error in H mag real 4 mag -0.9999995e9 stat.error

hMagErr vikingSourceRemeasurement VIKINGv20111019 Error in H mag real 4 mag -0.9999995e9 stat.error

hMagErr vvvSourceRemeasurement VVVv20100531 Error in H mag real 4 mag -0.9999995e9 stat.error

hMagErr vvvSourceRemeasurement VVVv20110718 Error in H mag real 4 mag -0.9999995e9 stat.error

hMagMAD ultravistaMapLcVariability ULTRAVISTADR4 Median Absolute Deviation of H magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMagMAD ultravistaVariability ULTRAVISTADR4 Median Absolute Deviation of H magnitude real 4 mag -0.9999995e9 stat.err;em.IR.H;phot.mag

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMagMAD videoVariability VIDEODR2 Median Absolute Deviation of H magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMagMAD videoVariability VIDEODR3 Median Absolute Deviation of H magnitude real 4 mag -0.9999995e9 stat.error;em.IR.NIR

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMagMAD videoVariability VIDEODR4 Median Absolute Deviation of H magnitude real 4 mag -0.9999995e9 stat.err;em.IR.H;phot.mag

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMagMAD videoVariability VIDEODR5 Median Absolute Deviation of H magnitude real 4 mag -0.9999995e9 stat.err;em.IR.H;phot.mag

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMagMAD videoVariability VIDEOv20100513 Median Absolute Deviation of H magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMagMAD videoVariability VIDEOv20111208 Median Absolute Deviation of H magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMagMAD vikingVariability VIKINGDR2 Median Absolute Deviation of H magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMagMAD vikingVariability VIKINGv20110714 Median Absolute Deviation of H magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMagMAD vikingVariability VIKINGv20111019 Median Absolute Deviation of H magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMagMAD vvvVariability VVVDR5 Median Absolute Deviation of H magnitude real 4 mag -0.9999995e9 stat.err;em.IR.H;phot.mag

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMagMAD vvvVariability VVVv20100531 Median Absolute Deviation of H magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMagRms ultravistaMapLcVariability ULTRAVISTADR4 rms of H magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMagRms ultravistaVariability ULTRAVISTADR4 rms of H magnitude real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMagRms videoVariability VIDEODR2 rms of H magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMagRms videoVariability VIDEODR3 rms of H magnitude real 4 mag -0.9999995e9 stat.error;em.IR.NIR

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMagRms videoVariability VIDEODR4 rms of H magnitude real 4 mag -0.9999995e9 stat.error;em.IR.H;phot.mag

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMagRms videoVariability VIDEODR5 rms of H magnitude real 4 mag -0.9999995e9 stat.error;em.IR.H;phot.mag

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMagRms videoVariability VIDEOv20100513 rms of H magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMagRms videoVariability VIDEOv20111208 rms of H magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMagRms vikingVariability VIKINGDR2 rms of H magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMagRms vikingVariability VIKINGv20110714 rms of H magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMagRms vikingVariability VIKINGv20111019 rms of H magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMagRms vvvVariability VVVDR5 rms of H magnitude real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMagRms vvvVariability VVVv20100531 rms of H magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hmaxCadence ultravistaMapLcVariability ULTRAVISTADR4 maximum gap between observations real 4 days -0.9999995e9

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hmaxCadence ultravistaVariability ULTRAVISTADR4 maximum gap between observations real 4 days -0.9999995e9 time.interval;obs;stat.max

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hmaxCadence videoVariability VIDEODR2 maximum gap between observations real 4 days -0.9999995e9

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hmaxCadence videoVariability VIDEODR3 maximum gap between observations real 4 days -0.9999995e9 time.interval;obs;stat.max

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hmaxCadence videoVariability VIDEODR4 maximum gap between observations real 4 days -0.9999995e9 time.interval;obs;stat.max

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hmaxCadence videoVariability VIDEODR5 maximum gap between observations real 4 days -0.9999995e9 time.interval;obs;stat.max

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hmaxCadence videoVariability VIDEOv20100513 maximum gap between observations real 4 days -0.9999995e9

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hmaxCadence videoVariability VIDEOv20111208 maximum gap between observations real 4 days -0.9999995e9

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hmaxCadence vikingVariability VIKINGDR2 maximum gap between observations real 4 days -0.9999995e9

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hmaxCadence vikingVariability VIKINGv20110714 maximum gap between observations real 4 days -0.9999995e9

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hmaxCadence vikingVariability VIKINGv20111019 maximum gap between observations real 4 days -0.9999995e9

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hmaxCadence vvvVariability VVVDR5 maximum gap between observations real 4 days -0.9999995e9 time.interval;obs;stat.max

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hmaxCadence vvvVariability VVVv20100531 maximum gap between observations real 4 days -0.9999995e9

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hMaxMag ultravistaMapLcVariability ULTRAVISTADR4 Maximum magnitude in H band, of good detections real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMaxMag ultravistaVariability ULTRAVISTADR4 Maximum magnitude in H band, of good detections real 4 mag -0.9999995e9 phot.mag;em.IR.H;stat.max

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMaxMag videoVariability VIDEODR2 Maximum magnitude in H band, of good detections real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMaxMag videoVariability VIDEODR3 Maximum magnitude in H band, of good detections real 4 -0.9999995e9 phot.mag;stat.max;em.IR.NIR

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMaxMag videoVariability VIDEODR4 Maximum magnitude in H band, of good detections real 4 mag -0.9999995e9 phot.mag;em.IR.H;stat.max

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMaxMag videoVariability VIDEODR5 Maximum magnitude in H band, of good detections real 4 mag -0.9999995e9 phot.mag;em.IR.H;stat.max

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMaxMag videoVariability VIDEOv20100513 Maximum magnitude in H band, of good detections real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMaxMag videoVariability VIDEOv20111208 Maximum magnitude in H band, of good detections real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMaxMag vikingVariability VIKINGDR2 Maximum magnitude in H band, of good detections real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMaxMag vikingVariability VIKINGv20110714 Maximum magnitude in H band, of good detections real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMaxMag vikingVariability VIKINGv20111019 Maximum magnitude in H band, of good detections real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMaxMag vvvVariability VVVDR5 Maximum magnitude in H band, of good detections real 4 mag -0.9999995e9 phot.mag;em.IR.H;stat.max

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMaxMag vvvVariability VVVv20100531 Maximum magnitude in H band, of good detections real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hmeanMag ultravistaMapLcVariability ULTRAVISTADR4 Mean H magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hmeanMag ultravistaVariability ULTRAVISTADR4 Mean H magnitude real 4 mag -0.9999995e9 phot.mag;em.IR.H;stat.mean;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hmeanMag videoVariability VIDEODR2 Mean H magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hmeanMag videoVariability VIDEODR3 Mean H magnitude real 4 mag -0.9999995e9 phot.mag;stat.mean;em.IR.NIR

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hmeanMag videoVariability VIDEODR4 Mean H magnitude real 4 mag -0.9999995e9 phot.mag;em.IR.H;stat.mean;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hmeanMag videoVariability VIDEODR5 Mean H magnitude real 4 mag -0.9999995e9 phot.mag;em.IR.H;stat.mean;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hmeanMag videoVariability VIDEOv20100513 Mean H magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hmeanMag videoVariability VIDEOv20111208 Mean H magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hmeanMag vikingVariability VIKINGDR2 Mean H magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hmeanMag vikingVariability VIKINGv20110714 Mean H magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hmeanMag vikingVariability VIKINGv20111019 Mean H magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hmeanMag vvvVariability VVVDR5 Mean H magnitude real 4 mag -0.9999995e9 phot.mag;em.IR.H;stat.mean;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hmeanMag vvvVariability VVVv20100531 Mean H magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

Hmeas vvvProperMotionCatalogue VVVDR5 Is there a Z band measurment for this frame tinyint 1

hmedCadence ultravistaMapLcVariability ULTRAVISTADR4 median gap between observations real 4 days -0.9999995e9

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hmedCadence ultravistaVariability ULTRAVISTADR4 median gap between observations real 4 days -0.9999995e9 time.interval;obs;stat.median

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hmedCadence videoVariability VIDEODR2 median gap between observations real 4 days -0.9999995e9

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hmedCadence videoVariability VIDEODR3 median gap between observations real 4 days -0.9999995e9 time.interval;obs;stat.median

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hmedCadence videoVariability VIDEODR4 median gap between observations real 4 days -0.9999995e9 time.interval;obs;stat.median

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hmedCadence videoVariability VIDEODR5 median gap between observations real 4 days -0.9999995e9 time.interval;obs;stat.median

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hmedCadence videoVariability VIDEOv20100513 median gap between observations real 4 days -0.9999995e9

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hmedCadence videoVariability VIDEOv20111208 median gap between observations real 4 days -0.9999995e9

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hmedCadence vikingVariability VIKINGDR2 median gap between observations real 4 days -0.9999995e9

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hmedCadence vikingVariability VIKINGv20110714 median gap between observations real 4 days -0.9999995e9

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hmedCadence vikingVariability VIKINGv20111019 median gap between observations real 4 days -0.9999995e9

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hmedCadence vvvVariability VVVDR5 median gap between observations real 4 days -0.9999995e9 time.interval;obs;stat.median

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hmedCadence vvvVariability VVVv20100531 median gap between observations real 4 days -0.9999995e9

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hmedianMag ultravistaMapLcVariability ULTRAVISTADR4 Median H magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hmedianMag ultravistaVariability ULTRAVISTADR4 Median H magnitude real 4 mag -0.9999995e9 phot.mag;em.IR.H;stat.median;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hmedianMag videoVariability VIDEODR2 Median H magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hmedianMag videoVariability VIDEODR3 Median H magnitude real 4 mag -0.9999995e9 phot.mag;stat.median;em.IR.NIR

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hmedianMag videoVariability VIDEODR4 Median H magnitude real 4 mag -0.9999995e9 phot.mag;em.IR.H;stat.median;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hmedianMag videoVariability VIDEODR5 Median H magnitude real 4 mag -0.9999995e9 phot.mag;em.IR.H;stat.median;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hmedianMag videoVariability VIDEOv20100513 Median H magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hmedianMag videoVariability VIDEOv20111208 Median H magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hmedianMag vikingVariability VIKINGDR2 Median H magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hmedianMag vikingVariability VIKINGv20110714 Median H magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hmedianMag vikingVariability VIKINGv20111019 Median H magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hmedianMag vvvVariability VVVDR5 Median H magnitude real 4 mag -0.9999995e9 phot.mag;em.IR.H;stat.median;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hmedianMag vvvVariability VVVv20100531 Median H magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hmfID ultravistaMergeLog, ultravistaRemeasMergeLog ULTRAVISTADR4 the UID of the relevant H multiframe bigint 8 meta.id;obs.field;em.IR.H

hmfID vhsMergeLog VHSDR1 the UID of the relevant H multiframe bigint 8 obs.field

hmfID vhsMergeLog VHSDR2 the UID of the relevant H multiframe bigint 8 obs.field

hmfID vhsMergeLog VHSDR3 the UID of the relevant H multiframe bigint 8 meta.id;obs.field;em.IR.H

hmfID vhsMergeLog VHSDR4 the UID of the relevant H multiframe bigint 8 meta.id;obs.field;em.IR.H

hmfID vhsMergeLog VHSDR5 the UID of the relevant H multiframe bigint 8 meta.id;obs.field;em.IR.H

hmfID vhsMergeLog VHSDR6 the UID of the relevant H multiframe bigint 8 meta.id;obs.field;em.IR.H

hmfID vhsMergeLog VHSv20120926 the UID of the relevant H multiframe bigint 8 meta.id;obs.field

hmfID vhsMergeLog VHSv20130417 the UID of the relevant H multiframe bigint 8 meta.id;obs.field

hmfID vhsMergeLog VHSv20140409 the UID of the relevant H multiframe bigint 8 meta.id;obs.field;em.IR.H

hmfID vhsMergeLog VHSv20150108 the UID of the relevant H multiframe bigint 8 meta.id;obs.field;em.IR.H

hmfID vhsMergeLog VHSv20160114 the UID of the relevant H multiframe bigint 8 meta.id;obs.field;em.IR.H

hmfID vhsMergeLog VHSv20160507 the UID of the relevant H multiframe bigint 8 meta.id;obs.field;em.IR.H

hmfID vhsMergeLog VHSv20170630 the UID of the relevant H multiframe bigint 8 meta.id;obs.field;em.IR.H

hmfID vhsMergeLog VHSv20180419 the UID of the relevant H multiframe bigint 8 meta.id;obs.field;em.IR.H

hmfID vhsMergeLog VHSv20201209 the UID of the relevant H multiframe bigint 8 meta.id;obs.field;em.IR.H

hmfID vhsMergeLog VHSv20231101 the UID of the relevant H multiframe bigint 8 meta.id;obs.field;em.IR.H

hmfID vhsMergeLog VHSv20240731 the UID of the relevant H multiframe bigint 8 meta.id;obs.field;em.IR.H

hmfID videoMergeLog VIDEODR2 the UID of the relevant H multiframe bigint 8 obs.field

hmfID videoMergeLog VIDEODR3 the UID of the relevant H multiframe bigint 8 meta.id;obs.field

hmfID videoMergeLog VIDEODR4 the UID of the relevant H multiframe bigint 8 meta.id;obs.field;em.IR.H

hmfID videoMergeLog VIDEODR5 the UID of the relevant H multiframe bigint 8 meta.id;obs.field;em.IR.H

hmfID videoMergeLog VIDEOv20100513 the UID of the relevant H multiframe bigint 8 obs.field

hmfID videoMergeLog VIDEOv20111208 the UID of the relevant H multiframe bigint 8 obs.field

hmfID vikingMergeLog VIKINGDR2 the UID of the relevant H multiframe bigint 8 obs.field

hmfID vikingMergeLog VIKINGDR3 the UID of the relevant H multiframe bigint 8 meta.id;obs.field

hmfID vikingMergeLog VIKINGDR4 the UID of the relevant H multiframe bigint 8 meta.id;obs.field;em.IR.H

hmfID vikingMergeLog VIKINGv20110714 the UID of the relevant H multiframe bigint 8 obs.field

hmfID vikingMergeLog VIKINGv20111019 the UID of the relevant H multiframe bigint 8 obs.field

hmfID vikingMergeLog VIKINGv20130417 the UID of the relevant H multiframe bigint 8 meta.id;obs.field

hmfID vikingMergeLog VIKINGv20140402 the UID of the relevant H multiframe bigint 8 meta.id;obs.field

hmfID vikingMergeLog VIKINGv20150421 the UID of the relevant H multiframe bigint 8 meta.id;obs.field;em.IR.H

hmfID vikingMergeLog VIKINGv20151230 the UID of the relevant H multiframe bigint 8 meta.id;obs.field;em.IR.H

hmfID vikingMergeLog VIKINGv20160406 the UID of the relevant H multiframe bigint 8 meta.id;obs.field;em.IR.H

hmfID vikingMergeLog VIKINGv20161202 the UID of the relevant H multiframe bigint 8 meta.id;obs.field;em.IR.H

hmfID vikingMergeLog VIKINGv20170715 the UID of the relevant H multiframe bigint 8 meta.id;obs.field;em.IR.H

hmfID vikingZY_selJ_RemeasMergeLog VIKINGZYSELJv20160909 the UID of the relevant H multiframe bigint 8 obs.field

hmfID vikingZY_selJ_RemeasMergeLog VIKINGZYSELJv20170124 the UID of the relevant H multiframe bigint 8 obs.field

hmfID vvvMergeLog VVVDR2 the UID of the relevant H multiframe bigint 8 meta.id;obs.field

hmfID vvvMergeLog VVVDR5 the UID of the relevant H multiframe bigint 8 meta.id;obs.field;em.IR.H

hmfID vvvMergeLog VVVv20100531 the UID of the relevant H multiframe bigint 8 obs.field

hmfID vvvMergeLog VVVv20110718 the UID of the relevant H multiframe bigint 8 obs.field

hmfID vvvMergeLog, vvvSynopticMergeLog VVVDR1 the UID of the relevant H multiframe bigint 8 meta.id;obs.field

hmfID vvvxMergeLog VVVXDR1 the UID of the relevant H multiframe bigint 8 meta.id;obs.field;em.IR.H

hminCadence ultravistaMapLcVariability ULTRAVISTADR4 minimum gap between observations real 4 days -0.9999995e9

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hminCadence ultravistaVariability ULTRAVISTADR4 minimum gap between observations real 4 days -0.9999995e9 time.interval;obs;stat.min

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hminCadence videoVariability VIDEODR2 minimum gap between observations real 4 days -0.9999995e9

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hminCadence videoVariability VIDEODR3 minimum gap between observations real 4 days -0.9999995e9 time.interval;obs;stat.min

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hminCadence videoVariability VIDEODR4 minimum gap between observations real 4 days -0.9999995e9 time.interval;obs;stat.min

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hminCadence videoVariability VIDEODR5 minimum gap between observations real 4 days -0.9999995e9 time.interval;obs;stat.min

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hminCadence videoVariability VIDEOv20100513 minimum gap between observations real 4 days -0.9999995e9

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hminCadence videoVariability VIDEOv20111208 minimum gap between observations real 4 days -0.9999995e9

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hminCadence vikingVariability VIKINGDR2 minimum gap between observations real 4 days -0.9999995e9

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hminCadence vikingVariability VIKINGv20110714 minimum gap between observations real 4 days -0.9999995e9

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hminCadence vikingVariability VIKINGv20111019 minimum gap between observations real 4 days -0.9999995e9

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hminCadence vvvVariability VVVDR5 minimum gap between observations real 4 days -0.9999995e9 time.interval;obs;stat.min

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hminCadence vvvVariability VVVv20100531 minimum gap between observations real 4 days -0.9999995e9

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hMinMag ultravistaMapLcVariability ULTRAVISTADR4 Minimum magnitude in H band, of good detections real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMinMag ultravistaVariability ULTRAVISTADR4 Minimum magnitude in H band, of good detections real 4 mag -0.9999995e9 phot.mag;em.IR.H;stat.min

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMinMag videoVariability VIDEODR2 Minimum magnitude in H band, of good detections real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMinMag videoVariability VIDEODR3 Minimum magnitude in H band, of good detections real 4 -0.9999995e9 phot.mag;stat.min;em.IR.NIR

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMinMag videoVariability VIDEODR4 Minimum magnitude in H band, of good detections real 4 mag -0.9999995e9 phot.mag;em.IR.H;stat.min

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMinMag videoVariability VIDEODR5 Minimum magnitude in H band, of good detections real 4 mag -0.9999995e9 phot.mag;em.IR.H;stat.min

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMinMag videoVariability VIDEOv20100513 Minimum magnitude in H band, of good detections real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMinMag videoVariability VIDEOv20111208 Minimum magnitude in H band, of good detections real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMinMag vikingVariability VIKINGDR2 Minimum magnitude in H band, of good detections real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMinMag vikingVariability VIKINGv20110714 Minimum magnitude in H band, of good detections real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMinMag vikingVariability VIKINGv20111019 Minimum magnitude in H band, of good detections real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMinMag vvvVariability VVVDR5 Minimum magnitude in H band, of good detections real 4 mag -0.9999995e9 phot.mag;em.IR.H;stat.min

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMinMag vvvVariability VVVv20100531 Minimum magnitude in H band, of good detections real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMjd ultravistaSource ULTRAVISTADR4 Modified Julian Day in H band float 8 days -0.9999995e9 time.epoch;em.IR.H

hMjd ultravistaSourceRemeasurement ULTRAVISTADR4 Modified Julian Day in H band float 8 days -0.9999995e9 time.epoch

hMjd vhsSource VHSDR5 Modified Julian Day in H band float 8 days -0.9999995e9 time.epoch

hMjd vhsSource VHSDR6 Modified Julian Day in H band float 8 days -0.9999995e9 time.epoch;em.IR.H

hMjd vhsSource VHSv20160114 Modified Julian Day in H band float 8 days -0.9999995e9 time.epoch

hMjd vhsSource VHSv20160507 Modified Julian Day in H band float 8 days -0.9999995e9 time.epoch

hMjd vhsSource VHSv20170630 Modified Julian Day in H band float 8 days -0.9999995e9 time.epoch

hMjd vhsSource VHSv20180419 Modified Julian Day in H band float 8 days -0.9999995e9 time.epoch;em.IR.H

hMjd vhsSource VHSv20201209 Modified Julian Day in H band float 8 days -0.9999995e9 time.epoch;em.IR.H

hMjd vhsSource VHSv20231101 Modified Julian Day in H band float 8 days -0.9999995e9 time.epoch;em.IR.H

hMjd vhsSource VHSv20240731 Modified Julian Day in H band float 8 days -0.9999995e9 time.epoch;em.IR.H

hMjd vikingSource VIKINGv20151230 Modified Julian Day in H band float 8 days -0.9999995e9 time.epoch

hMjd vikingSource VIKINGv20160406 Modified Julian Day in H band float 8 days -0.9999995e9 time.epoch

hMjd vikingSource VIKINGv20161202 Modified Julian Day in H band float 8 days -0.9999995e9 time.epoch

hMjd vikingSource VIKINGv20170715 Modified Julian Day in H band float 8 days -0.9999995e9 time.epoch

hMjd vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Modified Julian Day in H band float 8 days -0.9999995e9 time.epoch

hMjd vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Modified Julian Day in H band float 8 days -0.9999995e9 time.epoch

hMjd vvvSource VVVDR5 Modified Julian Day in H band float 8 days -0.9999995e9 time.epoch;em.IR.H

hMjd vvvSynopticSource VVVDR1 Modified Julian Day in H band float 8 days -0.9999995e9 time.epoch

hMjd vvvSynopticSource VVVDR2 Modified Julian Day in H band float 8 days -0.9999995e9 time.epoch

hMjd vvvxSource VVVXDR1 Modified Julian Day in H band float 8 days -0.9999995e9 time.epoch;em.IR.H

hmks vhsSourceRemeasurement VHSDR1 Default colour H-Ks (using appropriate mags) real 4 mag PHOT_COLOR

hmks videoSourceRemeasurement VIDEOv20100513 Default colour H-Ks (using appropriate mags) real 4 mag PHOT_COLOR

hmks vikingSourceRemeasurement VIKINGv20110714 Default colour H-Ks (using appropriate mags) real 4 mag PHOT_COLOR

hmks vikingSourceRemeasurement VIKINGv20111019 Default colour H-Ks (using appropriate mags) real 4 mag PHOT_COLOR

hmks vvvSourceRemeasurement VVVv20100531 Default colour H-Ks (using appropriate mags) real 4 mag PHOT_COLOR

hmks vvvSourceRemeasurement VVVv20110718 Default colour H-Ks (using appropriate mags) real 4 mag PHOT_COLOR

hmks_1Pnt vvvxSource VVVXDR1 Point source colour H-Ks_1 (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmks_1PntErr vvvxSource VVVXDR1 Error on point source colour H-Ks_1 real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmks_2Pnt vvvxSource VVVXDR1 Point source colour H-Ks_2 (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmks_2PntErr vvvxSource VVVXDR1 Error on point source colour H-Ks_2 real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksErr vhsSourceRemeasurement VHSDR1 Error on colour H-Ks real 4 mag stat.error

hmksErr videoSourceRemeasurement VIDEOv20100513 Error on colour H-Ks real 4 mag stat.error

hmksErr vikingSourceRemeasurement VIKINGv20110714 Error on colour H-Ks real 4 mag stat.error

hmksErr vikingSourceRemeasurement VIKINGv20111019 Error on colour H-Ks real 4 mag stat.error

hmksErr vvvSourceRemeasurement VVVv20100531 Error on colour H-Ks real 4 mag stat.error

hmksErr vvvSourceRemeasurement VVVv20110718 Error on colour H-Ks real 4 mag stat.error

hmksExt ultravistaSource ULTRAVISTADR4 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt ultravistaSourceRemeasurement ULTRAVISTADR4 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt vhsSource VHSDR1 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt vhsSource VHSDR2 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt vhsSource VHSDR3 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt vhsSource VHSDR4 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt vhsSource VHSDR5 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt vhsSource VHSDR6 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt vhsSource VHSv20120926 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt vhsSource VHSv20130417 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt vhsSource VHSv20140409 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt vhsSource VHSv20150108 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt vhsSource VHSv20160114 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt vhsSource VHSv20160507 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt vhsSource VHSv20170630 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt vhsSource VHSv20180419 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt vhsSource VHSv20201209 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt vhsSource VHSv20231101 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt vhsSource VHSv20240731 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt videoSource VIDEODR2 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt videoSource VIDEODR3 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt videoSource VIDEODR4 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt videoSource VIDEODR5 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt videoSource VIDEOv20100513 Extended source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt videoSource VIDEOv20111208 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt vikingSource VIKINGDR2 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt vikingSource VIKINGDR3 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt vikingSource VIKINGDR4 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt vikingSource VIKINGv20110714 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt vikingSource VIKINGv20111019 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt vikingSource VIKINGv20130417 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt vikingSource VIKINGv20140402 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt vikingSource VIKINGv20150421 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt vikingSource VIKINGv20151230 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt vikingSource VIKINGv20160406 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt vikingSource VIKINGv20161202 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt vikingSource VIKINGv20170715 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt vvvSource VVVv20100531 Extended source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr ultravistaSource ULTRAVISTADR4 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr ultravistaSourceRemeasurement ULTRAVISTADR4 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr vhsSource VHSDR1 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr vhsSource VHSDR2 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr vhsSource VHSDR3 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr vhsSource VHSDR4 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr vhsSource VHSDR5 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr vhsSource VHSDR6 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr vhsSource VHSv20120926 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr vhsSource VHSv20130417 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr vhsSource VHSv20140409 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr vhsSource VHSv20150108 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr vhsSource VHSv20160114 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr vhsSource VHSv20160507 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr vhsSource VHSv20170630 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr vhsSource VHSv20180419 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr vhsSource VHSv20201209 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr vhsSource VHSv20231101 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr vhsSource VHSv20240731 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr videoSource VIDEODR2 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr videoSource VIDEODR3 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr videoSource VIDEODR4 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr videoSource VIDEODR5 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr videoSource VIDEOv20100513 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr videoSource VIDEOv20111208 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr vikingSource VIKINGDR2 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr vikingSource VIKINGDR3 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr vikingSource VIKINGDR4 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr vikingSource VIKINGv20110714 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr vikingSource VIKINGv20111019 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr vikingSource VIKINGv20130417 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr vikingSource VIKINGv20140402 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr vikingSource VIKINGv20150421 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr vikingSource VIKINGv20151230 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr vikingSource VIKINGv20160406 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr vikingSource VIKINGv20161202 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr vikingSource VIKINGv20170715 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr vvvSource VVVv20100531 Error on extended source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtJky ultravistaSourceRemeasurement ULTRAVISTADR4 Extended source colour calibrated flux Ks/H (using aperJkyNoAperCorr3) real 4 jansky -0.9999995e9 phot.color

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtJky vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Extended source colour calibrated flux Ks/H (using aperJkyNoAperCorr3) real 4 jansky -0.9999995e9 phot.color

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtJky vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Extended source colour calibrated flux Ks/H (using aperJkyNoAperCorr3) real 4 jansky -0.9999995e9 phot.color

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtJkyErr ultravistaSourceRemeasurement ULTRAVISTADR4 Error on extended source colour calibrated flux Ks/H real 4 jansky -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtJkyErr vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error on extended source colour calibrated flux Ks/H real 4 jansky -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtJkyErr vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error on extended source colour calibrated flux Ks/H real 4 jansky -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtLup ultravistaSourceRemeasurement ULTRAVISTADR4 Extended source colour luptitudeH-Ks (using aperLupNoAperCorr3) real 4 lup -0.9999995e9 phot.color

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtLup vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Extended source colour luptitudeH-Ks (using aperLupNoAperCorr3) real 4 lup -0.9999995e9 phot.color

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtLup vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Extended source colour luptitudeH-Ks (using aperLupNoAperCorr3) real 4 lup -0.9999995e9 phot.color

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtLupErr ultravistaSourceRemeasurement ULTRAVISTADR4 Error on extended source colour luptitude H-Ks real 4 lup -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtLupErr vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error on extended source colour luptitude H-Ks real 4 lup -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtLupErr vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error on extended source colour luptitude H-Ks real 4 lup -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt ultravistaSource ULTRAVISTADR4 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt ultravistaSourceRemeasurement ULTRAVISTADR4 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vhsSource VHSDR1 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vhsSource VHSDR2 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vhsSource VHSDR3 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vhsSource VHSDR4 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vhsSource VHSDR5 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vhsSource VHSDR6 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vhsSource VHSv20120926 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vhsSource VHSv20130417 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vhsSource VHSv20140409 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vhsSource VHSv20150108 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vhsSource VHSv20160114 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vhsSource VHSv20160507 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vhsSource VHSv20170630 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vhsSource VHSv20180419 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vhsSource VHSv20201209 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vhsSource VHSv20231101 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vhsSource VHSv20240731 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt videoSource VIDEODR2 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt videoSource VIDEODR3 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt videoSource VIDEODR4 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt videoSource VIDEODR5 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt videoSource VIDEOv20100513 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt videoSource VIDEOv20111208 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vikingSource VIKINGDR2 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vikingSource VIKINGDR3 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vikingSource VIKINGDR4 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vikingSource VIKINGv20110714 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vikingSource VIKINGv20111019 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vikingSource VIKINGv20130417 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vikingSource VIKINGv20140402 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vikingSource VIKINGv20150421 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vikingSource VIKINGv20151230 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vikingSource VIKINGv20160406 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vikingSource VIKINGv20161202 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vikingSource VIKINGv20170715 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vvvPsfDophotZYJHKsSource VVVDR5 Point source colour H-Ks (using PsfMag) real 4 mag -0.9999995e9 phot.color

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vvvSource VVVDR2 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vvvSource VVVDR5 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vvvSource VVVv20100531 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vvvSource VVVv20110718 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vvvSource, vvvSynopticSource VVVDR1 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt vvvxSource VVVXDR1 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr ultravistaSource ULTRAVISTADR4 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr ultravistaSourceRemeasurement ULTRAVISTADR4 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vhsSource VHSDR1 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vhsSource VHSDR2 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vhsSource VHSDR3 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vhsSource VHSDR4 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vhsSource VHSDR5 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vhsSource VHSDR6 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vhsSource VHSv20120926 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vhsSource VHSv20130417 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vhsSource VHSv20140409 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vhsSource VHSv20150108 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vhsSource VHSv20160114 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vhsSource VHSv20160507 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vhsSource VHSv20170630 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vhsSource VHSv20180419 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vhsSource VHSv20201209 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vhsSource VHSv20231101 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vhsSource VHSv20240731 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr videoSource VIDEODR2 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr videoSource VIDEODR3 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr videoSource VIDEODR4 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr videoSource VIDEODR5 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr videoSource VIDEOv20100513 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr videoSource VIDEOv20111208 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vikingSource VIKINGDR2 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vikingSource VIKINGDR3 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vikingSource VIKINGDR4 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vikingSource VIKINGv20110714 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vikingSource VIKINGv20111019 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vikingSource VIKINGv20130417 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vikingSource VIKINGv20140402 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vikingSource VIKINGv20150421 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vikingSource VIKINGv20151230 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vikingSource VIKINGv20160406 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vikingSource VIKINGv20161202 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vikingSource VIKINGv20170715 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vvvPsfDophotZYJHKsSource VVVDR5 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vvvSource VVVDR2 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vvvSource VVVDR5 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vvvSource VVVv20100531 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vvvSource VVVv20110718 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vvvSource, vvvSynopticSource VVVDR1 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr vvvxSource VVVXDR1 Error on point source colour H-Ks real 4 mag -0.9999995e9 stat.error;em.IR.H;em.IR.K

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntJky ultravistaSourceRemeasurement ULTRAVISTADR4 Point source colour calibrated flux Ks/H (using aperJky3) real 4 jansky -0.9999995e9 phot.color

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntJky vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Point source colour calibrated flux Ks/H (using aperJky3) real 4 jansky -0.9999995e9 phot.color

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntJky vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Point source colour calibrated flux Ks/H (using aperJky3) real 4 jansky -0.9999995e9 phot.color

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntJkyErr ultravistaSourceRemeasurement ULTRAVISTADR4 Error on point source colour calibrated flux Ks/H real 4 jansky -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntJkyErr vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error on point source colour calibrated flux Ks/H real 4 jansky -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntJkyErr vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error on point source colour calibrated flux Ks/H real 4 jansky -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntLup ultravistaSourceRemeasurement ULTRAVISTADR4 Point source colour luptitude H-Ks (using aperLup3) real 4 lup -0.9999995e9 phot.color

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntLup vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Point source colour luptitude H-Ks (using aperLup3) real 4 lup -0.9999995e9 phot.color

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntLup vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Point source colour luptitude H-Ks (using aperLup3) real 4 lup -0.9999995e9 phot.color

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntLupErr ultravistaSourceRemeasurement ULTRAVISTADR4 Error on point source colour luptitude H-Ks real 4 lup -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntLupErr vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error on point source colour luptitude H-Ks real 4 lup -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntLupErr vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error on point source colour luptitude H-Ks real 4 lup -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hndof ultravistaMapLcVariability ULTRAVISTADR4 Number of degrees of freedom for chisquare smallint 2 -9999

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hndof ultravistaVariability ULTRAVISTADR4 Number of degrees of freedom for chisquare smallint 2 -9999 stat.fit.dof;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hndof videoVariability VIDEODR2 Number of degrees of freedom for chisquare smallint 2 -9999

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hndof videoVariability VIDEODR3 Number of degrees of freedom for chisquare smallint 2 -9999 stat.fit.dof

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hndof videoVariability VIDEODR4 Number of degrees of freedom for chisquare smallint 2 -9999 stat.fit.dof;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hndof videoVariability VIDEODR5 Number of degrees of freedom for chisquare smallint 2 -9999 stat.fit.dof;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hndof videoVariability VIDEOv20100513 Number of degrees of freedom for chisquare smallint 2 -9999

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hndof videoVariability VIDEOv20111208 Number of degrees of freedom for chisquare smallint 2 -9999

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hndof vikingVariability VIKINGDR2 Number of degrees of freedom for chisquare smallint 2 -9999

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hndof vikingVariability VIKINGv20110714 Number of degrees of freedom for chisquare smallint 2 -9999

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hndof vikingVariability VIKINGv20111019 Number of degrees of freedom for chisquare smallint 2 -9999

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hndof vvvVariability VVVDR5 Number of degrees of freedom for chisquare smallint 2 -9999 stat.fit.dof;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hndof vvvVariability VVVv20100531 Number of degrees of freedom for chisquare smallint 2 -9999

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hnDofAst ultravistaVarFrameSetInfo ULTRAVISTADR4 Number of degrees of freedom of astrometric fit in H band. smallint 2 -9999 stat.fit.dof;stat.param;em.IR.H

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hnDofAst videoVarFrameSetInfo VIDEODR2 Number of degrees of freedom of astrometric fit in H band. smallint 2 -9999

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hnDofAst videoVarFrameSetInfo VIDEODR3 Number of degrees of freedom of astrometric fit in H band. smallint 2 -9999 stat.fit.dof;stat.param;em.IR.NIR

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hnDofAst videoVarFrameSetInfo VIDEODR4 Number of degrees of freedom of astrometric fit in H band. smallint 2 -9999 stat.fit.dof;stat.param;em.IR.H

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hnDofAst videoVarFrameSetInfo VIDEODR5 Number of degrees of freedom of astrometric fit in H band. smallint 2 -9999 stat.fit.dof;stat.param;em.IR.H

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hnDofAst videoVarFrameSetInfo VIDEOv20100513 Number of degrees of freedom of astrometric fit in H band. smallint 2 -9999

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hnDofAst videoVarFrameSetInfo VIDEOv20111208 Number of degrees of freedom of astrometric fit in H band. smallint 2 -9999

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hnDofAst vikingVarFrameSetInfo VIKINGDR2 Number of degrees of freedom of astrometric fit in H band. smallint 2 -9999

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hnDofAst vikingVarFrameSetInfo VIKINGv20110714 Number of degrees of freedom of astrometric fit in H band. smallint 2 -9999

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hnDofAst vikingVarFrameSetInfo VIKINGv20111019 Number of degrees of freedom of astrometric fit in H band. smallint 2 -9999

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hnDofAst vvvVarFrameSetInfo VVVDR5 Number of degrees of freedom of astrometric fit in H band. smallint 2 -9999 stat.fit.dof;stat.param;em.IR.H

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hnDofAst vvvVarFrameSetInfo VVVv20100531 Number of degrees of freedom of astrometric fit in H band. smallint 2 -9999

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hnDofPht ultravistaMapLcVarFrameSetInfo, ultravistaVarFrameSetInfo ULTRAVISTADR4 Number of degrees of freedom of photometric fit in H band. smallint 2 -9999 stat.fit.dof;stat.param;em.IR.H

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hnDofPht videoVarFrameSetInfo VIDEODR2 Number of degrees of freedom of photometric fit in H band. smallint 2 -9999

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hnDofPht videoVarFrameSetInfo VIDEODR3 Number of degrees of freedom of photometric fit in H band. smallint 2 -9999 stat.fit.dof;stat.param;em.IR.NIR

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hnDofPht videoVarFrameSetInfo VIDEODR4 Number of degrees of freedom of photometric fit in H band. smallint 2 -9999 stat.fit.dof;stat.param;em.IR.H

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hnDofPht videoVarFrameSetInfo VIDEODR5 Number of degrees of freedom of photometric fit in H band. smallint 2 -9999 stat.fit.dof;stat.param;em.IR.H

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hnDofPht videoVarFrameSetInfo VIDEOv20100513 Number of degrees of freedom of photometric fit in H band. smallint 2 -9999

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hnDofPht videoVarFrameSetInfo VIDEOv20111208 Number of degrees of freedom of photometric fit in H band. smallint 2 -9999

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hnDofPht vikingVarFrameSetInfo VIKINGDR2 Number of degrees of freedom of photometric fit in H band. smallint 2 -9999

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hnDofPht vikingVarFrameSetInfo VIKINGv20110714 Number of degrees of freedom of photometric fit in H band. smallint 2 -9999

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hnDofPht vikingVarFrameSetInfo VIKINGv20111019 Number of degrees of freedom of photometric fit in H band. smallint 2 -9999

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hnDofPht vvvVarFrameSetInfo VVVDR5 Number of degrees of freedom of photometric fit in H band. smallint 2 -9999 stat.fit.dof;stat.param;em.IR.H

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hnDofPht vvvVarFrameSetInfo VVVv20100531 Number of degrees of freedom of photometric fit in H band. smallint 2 -9999

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hnFlaggedObs ultravistaVariability ULTRAVISTADR4 Number of detections in H band flagged as potentially spurious by ultravistaDetection.ppErrBits int 4 0 meta.number;em.IR.H

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnFlaggedObs videoVariability VIDEODR2 Number of detections in H band flagged as potentially spurious by videoDetection.ppErrBits int 4 0

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnFlaggedObs videoVariability VIDEODR3 Number of detections in H band flagged as potentially spurious by videoDetection.ppErrBits int 4 0 meta.number

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnFlaggedObs videoVariability VIDEODR4 Number of detections in H band flagged as potentially spurious by videoDetection.ppErrBits int 4 0 meta.number;em.IR.H

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnFlaggedObs videoVariability VIDEODR5 Number of detections in H band flagged as potentially spurious by videoDetection.ppErrBits int 4 0 meta.number;em.IR.H

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnFlaggedObs videoVariability VIDEOv20100513 Number of detections in H band flagged as potentially spurious by videoDetection.ppErrBits int 4 0

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnFlaggedObs videoVariability VIDEOv20111208 Number of detections in H band flagged as potentially spurious by videoDetection.ppErrBits int 4 0

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnFlaggedObs vikingVariability VIKINGDR2 Number of detections in H band flagged as potentially spurious by vikingDetection.ppErrBits int 4 0

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnFlaggedObs vikingVariability VIKINGv20110714 Number of detections in H band flagged as potentially spurious by vikingDetection.ppErrBits int 4 0

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnFlaggedObs vikingVariability VIKINGv20111019 Number of detections in H band flagged as potentially spurious by vikingDetection.ppErrBits int 4 0

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnFlaggedObs vvvVariability VVVDR5 Number of detections in H band flagged as potentially spurious by vvvDetection.ppErrBits int 4 0 meta.number;em.IR.H

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnFlaggedObs vvvVariability VVVv20100531 Number of detections in H band flagged as potentially spurious by vvvDetection.ppErrBits int 4 0

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnGoodObs ultravistaVariability ULTRAVISTADR4 Number of good detections in H band int 4 0 meta.number;em.IR.H

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnGoodObs videoVariability VIDEODR2 Number of good detections in H band int 4 0

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnGoodObs videoVariability VIDEODR3 Number of good detections in H band int 4 0 meta.number;em.IR.NIR

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnGoodObs videoVariability VIDEODR4 Number of good detections in H band int 4 0 meta.number;em.IR.H

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnGoodObs videoVariability VIDEODR5 Number of good detections in H band int 4 0 meta.number;em.IR.H

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnGoodObs videoVariability VIDEOv20100513 Number of good detections in H band int 4 0

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnGoodObs videoVariability VIDEOv20111208 Number of good detections in H band int 4 0

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnGoodObs vikingVariability VIKINGDR2 Number of good detections in H band int 4 0

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnGoodObs vikingVariability VIKINGv20110714 Number of good detections in H band int 4 0

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnGoodObs vikingVariability VIKINGv20111019 Number of good detections in H band int 4 0

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnGoodObs vvvVariability VVVDR5 Number of good detections in H band int 4 0 meta.number;em.IR.H

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnGoodObs vvvVariability VVVv20100531 Number of good detections in H band int 4 0

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hNgt3sig ultravistaMapLcVariability ULTRAVISTADR4 Number of good detections in H-band that are more than 3 sigma deviations (hAperMagN < (hMeanMag-3*hMagRms) smallint 2 -9999

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hNgt3sig ultravistaVariability ULTRAVISTADR4 Number of good detections in H-band that are more than 3 sigma deviations (hAperMagN < (hMeanMag-3*hMagRms) smallint 2 -9999 meta.number;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hNgt3sig videoVariability VIDEODR2 Number of good detections in H-band that are more than 3 sigma deviations smallint 2 -9999

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hNgt3sig videoVariability VIDEODR3 Number of good detections in H-band that are more than 3 sigma deviations smallint 2 -9999 meta.number;em.IR.NIR

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hNgt3sig videoVariability VIDEODR4 Number of good detections in H-band that are more than 3 sigma deviations smallint 2 -9999 meta.number;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hNgt3sig videoVariability VIDEODR5 Number of good detections in H-band that are more than 3 sigma deviations smallint 2 -9999 meta.number;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hNgt3sig videoVariability VIDEOv20100513 Number of good detections in H-band that are more than 3 sigma deviations smallint 2 -9999

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hNgt3sig videoVariability VIDEOv20111208 Number of good detections in H-band that are more than 3 sigma deviations smallint 2 -9999

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hNgt3sig vikingVariability VIKINGDR2 Number of good detections in H-band that are more than 3 sigma deviations smallint 2 -9999

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hNgt3sig vikingVariability VIKINGv20110714 Number of good detections in H-band that are more than 3 sigma deviations smallint 2 -9999

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hNgt3sig vikingVariability VIKINGv20111019 Number of good detections in H-band that are more than 3 sigma deviations smallint 2 -9999

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hNgt3sig vvvVariability VVVDR5 Number of good detections in H-band that are more than 3 sigma deviations (hAperMagN < (hMeanMag-3*hMagRms) smallint 2 -9999 meta.number;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hNgt3sig vvvVariability VVVv20100531 Number of good detections in H-band that are more than 3 sigma deviations smallint 2 -9999

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hnMissingObs ultravistaVariability ULTRAVISTADR4 Number of H band frames that this object should have been detected on and was not int 4 0 meta.number;em.IR.H

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnMissingObs videoVariability VIDEODR2 Number of H band frames that this object should have been detected on and was not int 4 0

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnMissingObs videoVariability VIDEODR3 Number of H band frames that this object should have been detected on and was not int 4 0 meta.number;em.IR.NIR

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnMissingObs videoVariability VIDEODR4 Number of H band frames that this object should have been detected on and was not int 4 0 meta.number;em.IR.H

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnMissingObs videoVariability VIDEODR5 Number of H band frames that this object should have been detected on and was not int 4 0 meta.number;em.IR.H

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnMissingObs videoVariability VIDEOv20100513 Number of H band frames that this object should have been detected on and was not int 4 0

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnMissingObs videoVariability VIDEOv20111208 Number of H band frames that this object should have been detected on and was not int 4 0

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnMissingObs vikingVariability VIKINGDR2 Number of H band frames that this object should have been detected on and was not int 4 0

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnMissingObs vikingVariability VIKINGv20110714 Number of H band frames that this object should have been detected on and was not int 4 0

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnMissingObs vikingVariability VIKINGv20111019 Number of H band frames that this object should have been detected on and was not int 4 0

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnMissingObs vvvVariability VVVDR5 Number of H band frames that this object should have been detected on and was not int 4 0 meta.number;em.IR.H

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnMissingObs vvvVariability VVVv20100531 Number of H band frames that this object should have been detected on and was not int 4 0

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnNegFlagObs ultravistaMapLcVariability ULTRAVISTADR4 Number of flagged negative measurements in H band by ultravistaMapRemeasurement.ppErrBits int 4 0

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnNegObs ultravistaMapLcVariability ULTRAVISTADR4 Number of unflagged negative measurements H band int 4 0

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnPosFlagObs ultravistaMapLcVariability ULTRAVISTADR4 Number of flagged positive measurements in H band by ultravistaMapRemeasurement.ppErrBits int 4 0

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hnPosObs ultravistaMapLcVariability ULTRAVISTADR4 Number of unflagged positive measurements in H band int 4 0

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hp_mag hipparcos_new_reduction GAIADR1 Hipparcos magnitude float 8 mag em.opt;phot.mag

hPA ultravistaSource ULTRAVISTADR4 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng;em.IR.H

hPA ultravistaSourceRemeasurement ULTRAVISTADR4 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng

hPA vhsSource VHSDR2 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng

hPA vhsSource VHSDR3 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng;em.IR.H

hPA vhsSource VHSDR4 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng;em.IR.H

hPA vhsSource VHSDR5 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng;em.IR.H

hPA vhsSource VHSDR6 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng;em.IR.H

hPA vhsSource VHSv20120926 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng

hPA vhsSource VHSv20130417 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng

hPA vhsSource VHSv20140409 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng;em.IR.H

hPA vhsSource VHSv20150108 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng;em.IR.H

hPA vhsSource VHSv20160114 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng;em.IR.H

hPA vhsSource VHSv20160507 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng;em.IR.H

hPA vhsSource VHSv20170630 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng;em.IR.H

hPA vhsSource VHSv20180419 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng;em.IR.H

hPA vhsSource VHSv20201209 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng;em.IR.H

hPA vhsSource VHSv20231101 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng;em.IR.H

hPA vhsSource VHSv20240731 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng;em.IR.H

hPA vhsSource, vhsSourceRemeasurement VHSDR1 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng

hPA videoSource VIDEODR2 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng

hPA videoSource VIDEODR3 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng

hPA videoSource VIDEODR4 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng;em.IR.H

hPA videoSource VIDEODR5 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng;em.IR.H

hPA videoSource VIDEOv20111208 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng

hPA videoSource, videoSourceRemeasurement VIDEOv20100513 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng

hPA vikingSource VIKINGDR2 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng

hPA vikingSource VIKINGDR3 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng

hPA vikingSource VIKINGDR4 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng;em.IR.H

hPA vikingSource VIKINGv20111019 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng

hPA vikingSource VIKINGv20130417 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng

hPA vikingSource VIKINGv20140402 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng

hPA vikingSource VIKINGv20150421 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng;em.IR.H

hPA vikingSource VIKINGv20151230 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng;em.IR.H

hPA vikingSource VIKINGv20160406 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng;em.IR.H

hPA vikingSource VIKINGv20161202 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng;em.IR.H

hPA vikingSource VIKINGv20170715 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng;em.IR.H

hPA vikingSource, vikingSourceRemeasurement VIKINGv20110714 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng

hPA vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng

hPA vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng

hPA vvvSource VVVDR2 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng

hPA vvvSource VVVDR5 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng;em.IR.H

hPA vvvSource VVVv20110718 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng

hPA vvvSource, vvvSourceRemeasurement VVVv20100531 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng

hPA vvvSource, vvvSynopticSource VVVDR1 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng

hPA vvvxSource VVVXDR1 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 pos.posAng;em.IR.H

hPetroJky ultravistaSourceRemeasurement ULTRAVISTADR4 Extended source H calibrated flux (Petrosian) real 4 jansky -0.9999995e9 phot.flux

hPetroJkyErr ultravistaSourceRemeasurement ULTRAVISTADR4 Error in extended source H calibrated flux (Petrosian) real 4 jansky -0.9999995e9 stat.error

hPetroLup ultravistaSourceRemeasurement ULTRAVISTADR4 Extended source H luptitude (Petrosian) real 4 lup -0.9999995e9 phot.lup

hPetroLupErr ultravistaSourceRemeasurement ULTRAVISTADR4 Error in extended source H luptitude (Petrosian) real 4 lup -0.9999995e9 stat.error

hPetroMag ultravistaSource ULTRAVISTADR4 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPetroMag ultravistaSourceRemeasurement ULTRAVISTADR4 Extended source H magnitude (Petrosian) real 4 mag -0.9999995e9 phot.mag

hPetroMag vhsSource VHSDR1 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag

hPetroMag vhsSource VHSDR2 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag

hPetroMag vhsSource VHSDR3 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPetroMag vhsSource VHSDR4 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPetroMag vhsSource VHSDR5 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPetroMag vhsSource VHSDR6 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPetroMag vhsSource VHSv20120926 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag

hPetroMag vhsSource VHSv20130417 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag

hPetroMag vhsSource VHSv20140409 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPetroMag vhsSource VHSv20150108 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPetroMag vhsSource VHSv20160114 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPetroMag vhsSource VHSv20160507 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPetroMag vhsSource VHSv20170630 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPetroMag vhsSource VHSv20180419 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPetroMag vhsSource VHSv20201209 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPetroMag vhsSource VHSv20231101 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPetroMag vhsSource VHSv20240731 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPetroMag videoSource VIDEODR2 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag

hPetroMag videoSource VIDEODR3 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag

hPetroMag videoSource VIDEODR4 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPetroMag videoSource VIDEODR5 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPetroMag videoSource VIDEOv20100513 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag

hPetroMag videoSource VIDEOv20111208 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag

hPetroMag vikingSource VIKINGDR2 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag

hPetroMag vikingSource VIKINGDR3 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag

hPetroMag vikingSource VIKINGDR4 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPetroMag vikingSource VIKINGv20110714 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag

hPetroMag vikingSource VIKINGv20111019 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag

hPetroMag vikingSource VIKINGv20130417 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag

hPetroMag vikingSource VIKINGv20140402 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPetroMag vikingSource VIKINGv20150421 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPetroMag vikingSource VIKINGv20151230 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPetroMag vikingSource VIKINGv20160406 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPetroMag vikingSource VIKINGv20161202 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPetroMag vikingSource VIKINGv20170715 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPetroMagErr ultravistaSource ULTRAVISTADR4 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hPetroMagErr ultravistaSourceRemeasurement ULTRAVISTADR4 Error in extended source H magnitude (Petrosian) real 4 mag -0.9999995e9 stat.error

hPetroMagErr vhsSource VHSDR1 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error

hPetroMagErr vhsSource VHSDR2 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error

hPetroMagErr vhsSource VHSDR3 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error;em.IR.H

hPetroMagErr vhsSource VHSDR4 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error;em.IR.H;phot.mag

hPetroMagErr vhsSource VHSDR5 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hPetroMagErr vhsSource VHSDR6 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hPetroMagErr vhsSource VHSv20120926 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error

hPetroMagErr vhsSource VHSv20130417 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error

hPetroMagErr vhsSource VHSv20140409 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error;em.IR.H

hPetroMagErr vhsSource VHSv20150108 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error;em.IR.H;phot.mag

hPetroMagErr vhsSource VHSv20160114 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hPetroMagErr vhsSource VHSv20160507 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hPetroMagErr vhsSource VHSv20170630 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hPetroMagErr vhsSource VHSv20180419 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hPetroMagErr vhsSource VHSv20201209 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hPetroMagErr vhsSource VHSv20231101 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hPetroMagErr vhsSource VHSv20240731 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hPetroMagErr videoSource VIDEODR2 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error

hPetroMagErr videoSource VIDEODR3 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error

hPetroMagErr videoSource VIDEODR4 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error;em.IR.H;phot.mag

hPetroMagErr videoSource VIDEODR5 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error;em.IR.H;phot.mag

hPetroMagErr videoSource VIDEOv20100513 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error

hPetroMagErr videoSource VIDEOv20111208 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error

hPetroMagErr vikingSource VIKINGDR2 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error

hPetroMagErr vikingSource VIKINGDR3 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error

hPetroMagErr vikingSource VIKINGDR4 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error;em.IR.H

hPetroMagErr vikingSource VIKINGv20110714 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error

hPetroMagErr vikingSource VIKINGv20111019 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error

hPetroMagErr vikingSource VIKINGv20130417 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error

hPetroMagErr vikingSource VIKINGv20140402 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error

hPetroMagErr vikingSource VIKINGv20150421 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error;em.IR.H;phot.mag

hPetroMagErr vikingSource VIKINGv20151230 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hPetroMagErr vikingSource VIKINGv20160406 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hPetroMagErr vikingSource VIKINGv20161202 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hPetroMagErr vikingSource VIKINGv20170715 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hppErrBits ultravistaSource ULTRAVISTADR4 additional WFAU post-processing error bits in H int 4 0 meta.code;em.IR.H

hppErrBits ultravistaSourceRemeasurement ULTRAVISTADR4 additional WFAU post-processing error bits in H int 4 0 meta.code

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues

1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits vhsSource VHSDR1 additional WFAU post-processing error bits in H int 4 0 meta.code

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues

1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits vhsSource VHSDR2 additional WFAU post-processing error bits in H int 4 0 meta.code

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues

1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits vhsSource VHSDR3 additional WFAU post-processing error bits in H int 4 0 meta.code;em.IR.H

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues

1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits vhsSource VHSDR4 additional WFAU post-processing error bits in H int 4 0 meta.code;em.IR.H

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues

1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits vhsSource VHSDR5 additional WFAU post-processing error bits in H int 4 0 meta.code;em.IR.H

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues

1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits vhsSource VHSDR6 additional WFAU post-processing error bits in H int 4 0 meta.code;em.IR.H

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues

1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits vhsSource VHSv20120926 additional WFAU post-processing error bits in H int 4 0 meta.code

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues

1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits vhsSource VHSv20130417 additional WFAU post-processing error bits in H int 4 0 meta.code

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues

1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits vhsSource VHSv20140409 additional WFAU post-processing error bits in H int 4 0 meta.code;em.IR.H

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues

1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits vhsSource VHSv20150108 additional WFAU post-processing error bits in H int 4 0 meta.code;em.IR.H

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues

1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits vhsSource VHSv20160114 additional WFAU post-processing error bits in H int 4 0 meta.code;em.IR.H

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues

1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits vhsSource VHSv20160507 additional WFAU post-processing error bits in H int 4 0 meta.code;em.IR.H

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues

1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits vhsSource VHSv20170630 additional WFAU post-processing error bits in H int 4 0 meta.code;em.IR.H

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues

1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits vhsSource VHSv20180419 additional WFAU post-processing error bits in H int 4 0 meta.code;em.IR.H

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues

1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits vhsSource VHSv20201209 additional WFAU post-processing error bits in H int 4 0 meta.code;em.IR.H

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues

1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits vhsSource VHSv20231101 additional WFAU post-processing error bits in H int 4 0 meta.code;em.IR.H

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues

1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits vhsSource VHSv20240731 additional WFAU post-processing error bits in H int 4 0 meta.code;em.IR.H

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues

1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits vhsSourceRemeasurement VHSDR1 additional WFAU post-processing error bits in H int 4 0 meta.code

hppErrBits videoSource VIDEODR2 additional WFAU post-processing error bits in H int 4 0 meta.code

hppErrBits videoSource VIDEODR3 additional WFAU post-processing error bits in H int 4 0 meta.code

hppErrBits videoSource VIDEODR4 additional WFAU post-processing error bits in H int 4 0 meta.code;em.IR.H

hppErrBits videoSource VIDEODR5 additional WFAU post-processing error bits in H int 4 0 meta.code;em.IR.H

hppErrBits videoSource VIDEOv20111208 additional WFAU post-processing error bits in H int 4 0 meta.code

hppErrBits videoSource, videoSourceRemeasurement VIDEOv20100513 additional WFAU post-processing error bits in H int 4 0 meta.code

hppErrBits vikingSource VIKINGDR2 additional WFAU post-processing error bits in H int 4 0 meta.code

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues

1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits vikingSource VIKINGDR3 additional WFAU post-processing error bits in H int 4 0 meta.code

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues

1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits vikingSource VIKINGDR4 additional WFAU post-processing error bits in H int 4 0 meta.code;em.IR.H

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues

1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits vikingSource VIKINGv20110714 additional WFAU post-processing error bits in H int 4 0 meta.code

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues

1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits vikingSource VIKINGv20111019 additional WFAU post-processing error bits in H int 4 0 meta.code

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues

1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits vikingSource VIKINGv20130417 additional WFAU post-processing error bits in H int 4 0 meta.code

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues

1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits vikingSource VIKINGv20140402 additional WFAU post-processing error bits in H int 4 0 meta.code

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues

1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits vikingSource VIKINGv20150421 additional WFAU post-processing error bits in H int 4 0 meta.code;em.IR.H

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues

1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits vikingSource VIKINGv20151230 additional WFAU post-processing error bits in H int 4 0 meta.code;em.IR.H

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues

1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits vikingSource VIKINGv20160406 additional WFAU post-processing error bits in H int 4 0 meta.code;em.IR.H

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues

1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits vikingSource VIKINGv20161202 additional WFAU post-processing error bits in H int 4 0 meta.code;em.IR.H

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues

1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits vikingSource VIKINGv20170715 additional WFAU post-processing error bits in H int 4 0 meta.code;em.IR.H

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues

1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits vikingSourceRemeasurement VIKINGv20110714 additional WFAU post-processing error bits in H int 4 0 meta.code

hppErrBits vikingSourceRemeasurement VIKINGv20111019 additional WFAU post-processing error bits in H int 4 0 meta.code

hppErrBits vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 additional WFAU post-processing error bits in H int 4 0 meta.code

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues

1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 additional WFAU post-processing error bits in H int 4 0 meta.code

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues

1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits vvvSource VVVDR1 additional WFAU post-processing error bits in H int 4 0 meta.code

hppErrBits vvvSource VVVDR2 additional WFAU post-processing error bits in H int 4 0 meta.code

hppErrBits vvvSource VVVDR5 additional WFAU post-processing error bits in H int 4 0 meta.code;em.IR.H

hppErrBits vvvSource VVVv20110718 additional WFAU post-processing error bits in H int 4 0 meta.code

hppErrBits vvvSource, vvvSourceRemeasurement VVVv20100531 additional WFAU post-processing error bits in H int 4 0 meta.code

hppErrBits vvvSynopticSource VVVDR1 additional WFAU post-processing error bits in H int 4 0 meta.code

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues

1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits vvvSynopticSource VVVDR2 additional WFAU post-processing error bits in H int 4 0 meta.code

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues

1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits vvvxSource VVVXDR1 additional WFAU post-processing error bits in H int 4 0 meta.code;em.IR.H

hprobVar ultravistaMapLcVariability ULTRAVISTADR4 Probability of variable from chi-square (and other data) real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hprobVar ultravistaVariability ULTRAVISTADR4 Probability of variable from chi-square (and other data) real 4 -0.9999995e9 stat.probability;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hprobVar videoVariability VIDEODR2 Probability of variable from chi-square (and other data) real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hprobVar videoVariability VIDEODR3 Probability of variable from chi-square (and other data) real 4 -0.9999995e9 stat.probability

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hprobVar videoVariability VIDEODR4 Probability of variable from chi-square (and other data) real 4 -0.9999995e9 stat.probability;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hprobVar videoVariability VIDEODR5 Probability of variable from chi-square (and other data) real 4 -0.9999995e9 stat.probability;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hprobVar videoVariability VIDEOv20100513 Probability of variable from chi-square (and other data) real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hprobVar videoVariability VIDEOv20111208 Probability of variable from chi-square (and other data) real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hprobVar vikingVariability VIKINGDR2 Probability of variable from chi-square (and other data) real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hprobVar vikingVariability VIKINGv20110714 Probability of variable from chi-square (and other data) real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hprobVar vikingVariability VIKINGv20111019 Probability of variable from chi-square (and other data) real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hprobVar vvvVariability VVVDR5 Probability of variable from chi-square (and other data) real 4 -0.9999995e9 stat.probability;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hprobVar vvvVariability VVVv20100531 Probability of variable from chi-square (and other data) real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hPsfMag vhsSource VHSDR1 Point source profile-fitted H mag real 4 mag -0.9999995e9 phot.mag

hPsfMag vhsSource VHSDR2 Point source profile-fitted H mag real 4 mag -0.9999995e9 phot.mag

hPsfMag vhsSource VHSDR3 Point source profile-fitted H mag real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPsfMag vhsSource VHSDR4 Point source profile-fitted H mag real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPsfMag vhsSource VHSDR5 Point source profile-fitted H mag real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPsfMag vhsSource VHSDR6 Point source profile-fitted H mag real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPsfMag vhsSource VHSv20120926 Point source profile-fitted H mag real 4 mag -0.9999995e9 phot.mag

hPsfMag vhsSource VHSv20130417 Point source profile-fitted H mag real 4 mag -0.9999995e9 phot.mag

hPsfMag vhsSource VHSv20140409 Point source profile-fitted H mag real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPsfMag vhsSource VHSv20150108 Point source profile-fitted H mag real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPsfMag vhsSource VHSv20160114 Point source profile-fitted H mag real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPsfMag vhsSource VHSv20160507 Point source profile-fitted H mag real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPsfMag vhsSource VHSv20170630 Point source profile-fitted H mag real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPsfMag vhsSource VHSv20180419 Point source profile-fitted H mag real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPsfMag vhsSource VHSv20201209 Point source profile-fitted H mag real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPsfMag vhsSource VHSv20231101 Point source profile-fitted H mag real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPsfMag vhsSource VHSv20240731 Point source profile-fitted H mag real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPsfMag videoSource VIDEOv20100513 Not available in SE output real 4 mag -0.9999995e9 phot.mag

hPsfMag vikingSource VIKINGDR2 Point source profile-fitted H mag real 4 mag -0.9999995e9 phot.mag

hPsfMag vikingSource VIKINGDR3 Point source profile-fitted H mag real 4 mag -0.9999995e9 phot.mag

hPsfMag vikingSource VIKINGDR4 Point source profile-fitted H mag real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPsfMag vikingSource VIKINGv20110714 Point source profile-fitted H mag real 4 mag -0.9999995e9 phot.mag

hPsfMag vikingSource VIKINGv20111019 Point source profile-fitted H mag real 4 mag -0.9999995e9 phot.mag

hPsfMag vikingSource VIKINGv20130417 Point source profile-fitted H mag real 4 mag -0.9999995e9 phot.mag

hPsfMag vikingSource VIKINGv20140402 Point source profile-fitted H mag real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPsfMag vikingSource VIKINGv20150421 Point source profile-fitted H mag real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPsfMag vikingSource VIKINGv20151230 Point source profile-fitted H mag real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPsfMag vikingSource VIKINGv20160406 Point source profile-fitted H mag real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPsfMag vikingSource VIKINGv20161202 Point source profile-fitted H mag real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPsfMag vikingSource VIKINGv20170715 Point source profile-fitted H mag real 4 mag -0.9999995e9 phot.mag;em.IR.H

hPsfMag vvvPsfDophotZYJHKsSource VVVDR5 Mean PSF magnitude in H band {catalogue TType keyword: mag_H} real 4 mag -0.9999995e9 instr.det.psf;phot.mag;em.IR.H;meta.main

hPsfMagErr vhsSource VHSDR1 Error in point source profile-fitted H mag real 4 mag -0.9999995e9 stat.error

hPsfMagErr vhsSource VHSDR2 Error in point source profile-fitted H mag real 4 mag -0.9999995e9 stat.error

hPsfMagErr vhsSource VHSDR3 Error in point source profile-fitted H mag real 4 mag -0.9999995e9 stat.error;em.IR.H

hPsfMagErr vhsSource VHSDR4 Error in point source profile-fitted H mag real 4 mag -0.9999995e9 stat.error;em.IR.H;phot.mag

hPsfMagErr vhsSource VHSDR5 Error in point source profile-fitted H mag real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hPsfMagErr vhsSource VHSDR6 Error in point source profile-fitted H mag real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hPsfMagErr vhsSource VHSv20120926 Error in point source profile-fitted H mag real 4 mag -0.9999995e9 stat.error

hPsfMagErr vhsSource VHSv20130417 Error in point source profile-fitted H mag real 4 mag -0.9999995e9 stat.error

hPsfMagErr vhsSource VHSv20140409 Error in point source profile-fitted H mag real 4 mag -0.9999995e9 stat.error;em.IR.H

hPsfMagErr vhsSource VHSv20150108 Error in point source profile-fitted H mag real 4 mag -0.9999995e9 stat.error;em.IR.H;phot.mag

hPsfMagErr vhsSource VHSv20160114 Error in point source profile-fitted H mag real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hPsfMagErr vhsSource VHSv20160507 Error in point source profile-fitted H mag real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hPsfMagErr vhsSource VHSv20170630 Error in point source profile-fitted H mag real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hPsfMagErr vhsSource VHSv20180419 Error in point source profile-fitted H mag real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hPsfMagErr vhsSource VHSv20201209 Error in point source profile-fitted H mag real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hPsfMagErr vhsSource VHSv20231101 Error in point source profile-fitted H mag real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hPsfMagErr vhsSource VHSv20240731 Error in point source profile-fitted H mag real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hPsfMagErr videoSource VIDEOv20100513 Not available in SE output real 4 mag -0.9999995e9 stat.error

hPsfMagErr vikingSource VIKINGDR2 Error in point source profile-fitted H mag real 4 mag -0.9999995e9 stat.error

hPsfMagErr vikingSource VIKINGDR3 Error in point source profile-fitted H mag real 4 mag -0.9999995e9 stat.error

hPsfMagErr vikingSource VIKINGDR4 Error in point source profile-fitted H mag real 4 mag -0.9999995e9 stat.error;em.IR.H

hPsfMagErr vikingSource VIKINGv20110714 Error in point source profile-fitted H mag real 4 mag -0.9999995e9 stat.error

hPsfMagErr vikingSource VIKINGv20111019 Error in point source profile-fitted H mag real 4 mag -0.9999995e9 stat.error

hPsfMagErr vikingSource VIKINGv20130417 Error in point source profile-fitted H mag real 4 mag -0.9999995e9 stat.error

hPsfMagErr vikingSource VIKINGv20140402 Error in point source profile-fitted H mag real 4 mag -0.9999995e9 stat.error

hPsfMagErr vikingSource VIKINGv20150421 Error in point source profile-fitted H mag real 4 mag -0.9999995e9 stat.error;em.IR.H;phot.mag

hPsfMagErr vikingSource VIKINGv20151230 Error in point source profile-fitted H mag real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hPsfMagErr vikingSource VIKINGv20160406 Error in point source profile-fitted H mag real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hPsfMagErr vikingSource VIKINGv20161202 Error in point source profile-fitted H mag real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hPsfMagErr vikingSource VIKINGv20170715 Error in point source profile-fitted H mag real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hPsfMagErr vvvPsfDophotZYJHKsSource VVVDR5 Error on mean PSF magnitude in H band {catalogue TType keyword: er_H} real 4 mag -0.9999995e9 stat.error;instr.det.psf;em.IR.H

hr1 rosat_bsc, rosat_fsc ROSAT hardness ratio 1 float 8 phot.flux;arith.ratio

hr2 rosat_bsc, rosat_fsc ROSAT hardness ratio 2 float 8 phot.flux;arith.ratio

HRV ravedr5Source RAVE Heliocentric radial velocity real 4 km/s spect.dopplerVeloc;pos.heliocentric

hry twomass_scn TWOMASS Flag indicating the H-band array configuration for the camera. smallint 2 meta.code

hry twomass_sixx2_scn TWOMASS H-band detector array switched, north only (0=old, 1=new) smallint 2

hsdFlag_100 iras_psc IRAS Source is located in high source density bin (100 micron). tinyint 1 meta.note

hsdFlag_12 iras_psc IRAS Source is located in high source density bin (12 micron). tinyint 1 meta.note

hsdFlag_25 iras_psc IRAS Source is located in high source density bin (25 micron). tinyint 1 meta.note

hsdFlag_60 iras_psc IRAS Source is located in high source density bin (60 micron). tinyint 1 meta.note

Hsep vvvProperMotionCatalogue VVVDR5 Sky distance between VVV DR4 H detection and the projected source position at the H observation epoch taking the pipeline proper motion into account. {catalogue TType keyword: Hsep} real 4 arcsec -999999500.0

hSeqNum ultravistaSource ULTRAVISTADR4 the running number of the H detection int 4 -99999999 meta.number;em.IR.H

hSeqNum vhsSource VHSDR1 the running number of the H detection int 4 -99999999 meta.id

hSeqNum vhsSource VHSDR2 the running number of the H detection int 4 -99999999 meta.id

hSeqNum vhsSource VHSDR3 the running number of the H detection int 4 -99999999 meta.number;em.IR.H

hSeqNum vhsSource VHSDR4 the running number of the H detection int 4 -99999999 meta.number;em.IR.H

hSeqNum vhsSource VHSDR5 the running number of the H detection int 4 -99999999 meta.number;em.IR.H

hSeqNum vhsSource VHSDR6 the running number of the H detection int 4 -99999999 meta.number;em.IR.H

hSeqNum vhsSource VHSv20120926 the running number of the H detection int 4 -99999999 meta.number

hSeqNum vhsSource VHSv20130417 the running number of the H detection int 4 -99999999 meta.number

hSeqNum vhsSource VHSv20140409 the running number of the H detection int 4 -99999999 meta.number;em.IR.H

hSeqNum vhsSource VHSv20150108 the running number of the H detection int 4 -99999999 meta.number;em.IR.H

hSeqNum vhsSource VHSv20160114 the running number of the H detection int 4 -99999999 meta.number;em.IR.H

hSeqNum vhsSource VHSv20160507 the running number of the H detection int 4 -99999999 meta.number;em.IR.H

hSeqNum vhsSource VHSv20170630 the running number of the H detection int 4 -99999999 meta.number;em.IR.H

hSeqNum vhsSource VHSv20180419 the running number of the H detection int 4 -99999999 meta.number;em.IR.H

hSeqNum vhsSource VHSv20201209 the running number of the H detection int 4 -99999999 meta.id;em.IR.H

hSeqNum vhsSource VHSv20231101 the running number of the H detection int 4 -99999999 meta.id;em.IR.H

hSeqNum vhsSource VHSv20240731 the running number of the H detection int 4 -99999999 meta.id;em.IR.H

hSeqNum vhsSourceRemeasurement VHSDR1 the running number of the H remeasurement int 4 -99999999 meta.id

hSeqNum videoSource VIDEODR2 the running number of the H detection int 4 -99999999 meta.id

hSeqNum videoSource VIDEODR3 the running number of the H detection int 4 -99999999 meta.number

hSeqNum videoSource VIDEODR4 the running number of the H detection int 4 -99999999 meta.number;em.IR.H

hSeqNum videoSource VIDEODR5 the running number of the H detection int 4 -99999999 meta.number;em.IR.H

hSeqNum videoSource VIDEOv20100513 the running number of the H detection int 4 -99999999 meta.id

hSeqNum videoSource VIDEOv20111208 the running number of the H detection int 4 -99999999 meta.id

hSeqNum videoSourceRemeasurement VIDEOv20100513 the running number of the H remeasurement int 4 -99999999 meta.id

hSeqNum vikingSource VIKINGDR2 the running number of the H detection int 4 -99999999 meta.id

hSeqNum vikingSource VIKINGDR3 the running number of the H detection int 4 -99999999 meta.number

hSeqNum vikingSource VIKINGDR4 the running number of the H detection int 4 -99999999 meta.number;em.IR.H

hSeqNum vikingSource VIKINGv20110714 the running number of the H detection int 4 -99999999 meta.id

hSeqNum vikingSource VIKINGv20111019 the running number of the H detection int 4 -99999999 meta.id

hSeqNum vikingSource VIKINGv20130417 the running number of the H detection int 4 -99999999 meta.number

hSeqNum vikingSource VIKINGv20140402 the running number of the H detection int 4 -99999999 meta.number

hSeqNum vikingSource VIKINGv20150421 the running number of the H detection int 4 -99999999 meta.number;em.IR.H

hSeqNum vikingSource VIKINGv20151230 the running number of the H detection int 4 -99999999 meta.number;em.IR.H

hSeqNum vikingSource VIKINGv20160406 the running number of the H detection int 4 -99999999 meta.number;em.IR.H

hSeqNum vikingSource VIKINGv20161202 the running number of the H detection int 4 -99999999 meta.number;em.IR.H

hSeqNum vikingSource VIKINGv20170715 the running number of the H detection int 4 -99999999 meta.number;em.IR.H

hSeqNum vikingSourceRemeasurement VIKINGv20110714 the running number of the H remeasurement int 4 -99999999 meta.id

hSeqNum vikingSourceRemeasurement VIKINGv20111019 the running number of the H remeasurement int 4 -99999999 meta.id

hSeqNum vvvSource VVVDR2 the running number of the H detection int 4 -99999999 meta.number

hSeqNum vvvSource VVVDR5 the running number of the H detection int 4 -99999999 meta.number;em.IR.H

hSeqNum vvvSource VVVv20100531 the running number of the H detection int 4 -99999999 meta.id

hSeqNum vvvSource VVVv20110718 the running number of the H detection int 4 -99999999 meta.id

hSeqNum vvvSource, vvvSynopticSource VVVDR1 the running number of the H detection int 4 -99999999 meta.number

hSeqNum vvvSourceRemeasurement VVVv20100531 the running number of the H remeasurement int 4 -99999999 meta.id

hSeqNum vvvSourceRemeasurement VVVv20110718 the running number of the H remeasurement int 4 -99999999 meta.id

hSeqNum vvvxSource VVVXDR1 the running number of the H detection int 4 -99999999 meta.id;em.IR.H

hSerMag2D vhsSource VHSDR1 Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag

hSerMag2D vhsSource VHSDR2 Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag

hSerMag2D vhsSource VHSDR3 Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hSerMag2D vhsSource VHSDR4 Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hSerMag2D vhsSource VHSDR5 Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hSerMag2D vhsSource VHSDR6 Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hSerMag2D vhsSource VHSv20120926 Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag

hSerMag2D vhsSource VHSv20130417 Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag

hSerMag2D vhsSource VHSv20140409 Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hSerMag2D vhsSource VHSv20150108 Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hSerMag2D vhsSource VHSv20160114 Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hSerMag2D vhsSource VHSv20160507 Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hSerMag2D vhsSource VHSv20170630 Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hSerMag2D vhsSource VHSv20180419 Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hSerMag2D vhsSource VHSv20201209 Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hSerMag2D vhsSource VHSv20231101 Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hSerMag2D vhsSource VHSv20240731 Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hSerMag2D videoSource VIDEOv20100513 Not available in SE output real 4 mag -0.9999995e9 phot.mag

hSerMag2D vikingSource VIKINGDR2 Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag

hSerMag2D vikingSource VIKINGDR3 Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag

hSerMag2D vikingSource VIKINGDR4 Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hSerMag2D vikingSource VIKINGv20110714 Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag

hSerMag2D vikingSource VIKINGv20111019 Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag

hSerMag2D vikingSource VIKINGv20130417 Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag

hSerMag2D vikingSource VIKINGv20140402 Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hSerMag2D vikingSource VIKINGv20150421 Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hSerMag2D vikingSource VIKINGv20151230 Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hSerMag2D vikingSource VIKINGv20160406 Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hSerMag2D vikingSource VIKINGv20161202 Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hSerMag2D vikingSource VIKINGv20170715 Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag;em.IR.H

hSerMag2DErr vhsSource VHSDR1 Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 stat.error

hSerMag2DErr vhsSource VHSDR2 Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 stat.error

hSerMag2DErr vhsSource VHSDR3 Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;em.IR.H

hSerMag2DErr vhsSource VHSDR4 Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;em.IR.H;phot.mag

hSerMag2DErr vhsSource VHSDR5 Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hSerMag2DErr vhsSource VHSDR6 Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hSerMag2DErr vhsSource VHSv20120926 Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 stat.error

hSerMag2DErr vhsSource VHSv20130417 Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 stat.error

hSerMag2DErr vhsSource VHSv20140409 Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;em.IR.H

hSerMag2DErr vhsSource VHSv20150108 Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;em.IR.H;phot.mag

hSerMag2DErr vhsSource VHSv20160114 Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hSerMag2DErr vhsSource VHSv20160507 Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hSerMag2DErr vhsSource VHSv20170630 Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hSerMag2DErr vhsSource VHSv20180419 Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hSerMag2DErr vhsSource VHSv20201209 Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hSerMag2DErr vhsSource VHSv20231101 Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hSerMag2DErr vhsSource VHSv20240731 Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hSerMag2DErr videoSource VIDEOv20100513 Not available in SE output real 4 mag -0.9999995e9 stat.error

hSerMag2DErr vikingSource VIKINGDR2 Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 stat.error

hSerMag2DErr vikingSource VIKINGDR3 Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 stat.error

hSerMag2DErr vikingSource VIKINGDR4 Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;em.IR.H

hSerMag2DErr vikingSource VIKINGv20110714 Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 stat.error

hSerMag2DErr vikingSource VIKINGv20111019 Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 stat.error

hSerMag2DErr vikingSource VIKINGv20130417 Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 stat.error

hSerMag2DErr vikingSource VIKINGv20140402 Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 stat.error

hSerMag2DErr vikingSource VIKINGv20150421 Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;em.IR.H;phot.mag

hSerMag2DErr vikingSource VIKINGv20151230 Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hSerMag2DErr vikingSource VIKINGv20160406 Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hSerMag2DErr vikingSource VIKINGv20161202 Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hSerMag2DErr vikingSource VIKINGv20170715 Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.H

hskewness ultravistaMapLcVariability ULTRAVISTADR4 Skewness in H band (see Sesar et al. 2007) real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hskewness ultravistaVariability ULTRAVISTADR4 Skewness in H band (see Sesar et al. 2007) real 4 mag -0.9999995e9 stat.param;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hskewness videoVariability VIDEODR2 Skewness in H band (see Sesar et al. 2007) real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hskewness videoVariability VIDEODR3 Skewness in H band (see Sesar et al. 2007) real 4 -0.9999995e9 stat.param;em.IR.NIR

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hskewness videoVariability VIDEODR4 Skewness in H band (see Sesar et al. 2007) real 4 mag -0.9999995e9 stat.param;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hskewness videoVariability VIDEODR5 Skewness in H band (see Sesar et al. 2007) real 4 mag -0.9999995e9 stat.param;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hskewness videoVariability VIDEOv20100513 Skewness in H band (see Sesar et al. 2007) real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hskewness videoVariability VIDEOv20111208 Skewness in H band (see Sesar et al. 2007) real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hskewness vikingVariability VIKINGDR2 Skewness in H band (see Sesar et al. 2007) real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hskewness vikingVariability VIKINGv20110714 Skewness in H band (see Sesar et al. 2007) real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hskewness vikingVariability VIKINGv20111019 Skewness in H band (see Sesar et al. 2007) real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hskewness vvvVariability VVVDR5 Skewness in H band (see Sesar et al. 2007) real 4 mag -0.9999995e9 stat.param;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hskewness vvvVariability VVVv20100531 Skewness in H band (see Sesar et al. 2007) real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

htm20 allwise_sc WISE Level 20 HTM spatial index key bigint 8

htm9 smashdr2_deep, smashdr2_object SMASH HTM index (order 9 => ~10 arcmin size) int 4

htm9 smashdr2_source SMASH HTM index (order 9 => ∼10 arcmin size) int 4

HTMID spectra SIXDF Hierarchical Triangular Mesh (20-deep), mainly useful internally for indexing on position bigint 8

HTMID target SIXDF Hierarchical Triangular Mesh (20-deep) number, mainly useful internally for indexing on position bigint 8

HTMID twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0, xmm3dr4 XMM Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID CurrentAstrometry SHARKSv20210222 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry SHARKSv20210421 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry ULTRAVISTADR4 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VHSDR1 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VHSDR2 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VHSDR3 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VHSDR4 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VHSDR5 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VHSDR6 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VHSv20120926 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VHSv20130417 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VHSv20140409 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VHSv20150108 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VHSv20160114 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VHSv20160507 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VHSv20170630 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VHSv20180419 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VHSv20201209 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VHSv20231101 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VHSv20240731 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VIDEODR2 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VIDEODR3 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VIDEODR4 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VIDEODR5 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VIDEOv20100513 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VIDEOv20111208 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VIKINGDR2 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VIKINGDR3 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VIKINGDR4 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VIKINGv20110714 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VIKINGv20111019 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VIKINGv20130417 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VIKINGv20140402 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VIKINGv20150421 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VIKINGv20151230 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VIKINGv20160406 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VIKINGv20161202 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VIKINGv20170715 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VMCDEEPv20230713 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VMCDEEPv20240506 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VMCDR1 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VMCDR2 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VMCDR3 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VMCDR4 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VMCDR5 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VMCv20110816 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VMCv20110909 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VMCv20120126 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VMCv20121128 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VMCv20130304 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VMCv20130805 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VMCv20140428 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VMCv20140903 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VMCv20150309 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VMCv20151218 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VMCv20160311 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VMCv20160822 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VMCv20170109 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VMCv20170411 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VMCv20171101 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VMCv20180702 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VMCv20181120 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VMCv20191212 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VMCv20210708 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VMCv20230816 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VMCv20240226 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VVVDR1 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VVVDR2 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VVVDR5 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VVVXDR1 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VVVv20100531 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID CurrentAstrometry VVVv20110718 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID ObjectThin PS1DR2 Hierarchical triangular mesh (Szalay 2007) index. bigint 8 pos.HTM

htmID akari_lmc_psa_v1, akari_lmc_psc_v1 AKARI Hierarchical Triangular Mesh (HTM) index for equatorial co-ordinates (computed to level 20) bigint 8 pos.eq

htmID catwise_2020, catwise_prelim WISE Level 20 Hierarchical Triangular Mesh (HTM) index for equatorial co-ordinates bigint 8 pos.eq

htmID combo17CDFSSource COMBO17 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID decapsSource DECAPS Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID denisDR3Source DENIS Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID eros2LMCSource, eros2SMCSource, erosLMCSource, erosSMCSource EROS Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID first08Jul16Source, firstSource, firstSource12Feb16 FIRST Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID gaia_source GAIADR2 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID gaia_source GAIAEDR3 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID gaia_source, hipparcos_new_reduction, igsl_source, tgas_source, tycho2 GAIADR1 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID glimpse1_hrc, glimpse1_mca, glimpse2_hrc, glimpse2_mca, glimpse_hrc_inter, glimpse_mca_inter GLIMPSE Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID grs_ngpSource, grs_ranSource, grs_sgpSource TWODFGRS Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID iras_psc IRAS Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID machoLMCSource, machoSMCSource MACHO Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID masterDR2 SKYMAPPER Level 20 Hierarchical Triangular Mesh (HTM) index for equatorial co-ordinates bigint 8 pos.htm

htmID mcps_lmcSource, mcps_smcSource MCPS Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID mgcDetection MGC Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID nvssSource NVSS Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID ogle3LpvLmcSource, ogle3LpvSmcSource, ogle4CepLmcSource, ogle4CepSmcSource, ogle4RRLyrLmcSource, ogle4RRLyrSmcSource OGLE Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID ravedr5Source RAVE Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.general

htmID rosat_bsc, rosat_fsc ROSAT Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID sage_lmcIracSource, sage_lmcMips160Source, sage_lmcMips24Source, sage_lmcMips70Source SPITZER 20-deep hierachical triangular mesh ID of this source bigint 8

htmID sage_smcIRACv1_5Source SPITZER The Hierchical Triangular Mesh partition, computed at index level 20, in which this source lies. bigint 8

htmID sharksCurrentAstrometry, ultravistaCurrentAstrometry, vhsCurrentAstrometry, videoCurrentAstrometry, vikingCurrentAstrometry, vmcCurrentAstrometry, vvvCurrentAstrometry VSAQC Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 pos.eq

htmID sharksDetection SHARKSv20210421 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID sharksDetection, sharksMergeLog, sharksSource, sharksTilePawPrints, sharksTileSet SHARKSv20210222 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID sharksTilePawTDOnly SHARKSv20210222 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID sharksTilePawTDOnly SHARKSv20210421 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID spitzer_smcSource SPITZER Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID twomass_psc, twomass_scn, twomass_sixx2_psc, twomass_sixx2_scn, twomass_sixx2_xsc, twomass_xsc TWOMASS Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID twompzPhotoz TWOMPZ Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID ultravistaDetection, ultravistaMergeLog, ultravistaSource, ultravistaTilePawPrints, ultravistaTileSet ULTRAVISTADR4 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID ultravistaMapRemeasAver, ultravistaMapRemeasurement, ultravistaRemeasMergeLog ULTRAVISTADR4 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID ultravistaSourceRemeasurement ULTRAVISTADR4 Hierarchical Triangular Mesh (HTM) index of aperture, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID ultravistaTilePawTDOnly ULTRAVISTADR4 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vhsDetection VHSDR3 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vhsDetection VHSDR4 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vhsDetection VHSDR5 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vhsDetection VHSDR6 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vhsDetection VHSv20120926 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vhsDetection VHSv20130417 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vhsDetection VHSv20140409 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vhsDetection VHSv20150108 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vhsDetection VHSv20160114 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vhsDetection VHSv20160507 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vhsDetection VHSv20170630 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vhsDetection VHSv20180419 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vhsDetection VHSv20201209 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vhsDetection VHSv20231101 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vhsDetection VHSv20240731 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vhsDetection, vhsListRemeasurement, vhsMergeLog, vhsSource, vhsSourceRemeasurement, vhsTilePawPrints, vhsTileSet VHSDR1 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID vhsDetection, vhsMergeLog, vhsTilePawPrints VHSDR2 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID vhsTilePawTDOnly VHSDR1 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID vhsTilePawTDOnly VHSDR2 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID vhsTilePawTDOnly VHSDR3 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vhsTilePawTDOnly VHSDR4 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vhsTilePawTDOnly VHSDR5 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vhsTilePawTDOnly VHSDR6 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vhsTilePawTDOnly VHSv20120926 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vhsTilePawTDOnly VHSv20130417 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vhsTilePawTDOnly VHSv20140409 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vhsTilePawTDOnly VHSv20150108 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vhsTilePawTDOnly VHSv20160114 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vhsTilePawTDOnly VHSv20160507 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vhsTilePawTDOnly VHSv20170630 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vhsTilePawTDOnly VHSv20180419 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vhsTilePawTDOnly VHSv20201209 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vhsTilePawTDOnly VHSv20231101 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vhsTilePawTDOnly VHSv20240731 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID videoDetection VIDEODR3 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID videoDetection VIDEODR4 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID videoDetection VIDEODR5 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID videoDetection VIDEOv20111208 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID videoDetection, videoListRemeasurement, videoSourceRemeasurement VIDEOv20100513 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID videoDetection, videoMergeLog, videoSource, videoTilePawPrints, videoTileSet VIDEODR2 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID videoTilePawTDOnly VIDEODR2 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID videoTilePawTDOnly VIDEODR3 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID videoTilePawTDOnly VIDEODR4 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID videoTilePawTDOnly VIDEODR5 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID videoTilePawTDOnly VIDEOv20111208 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID vikingDetection VIKINGDR3 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vikingDetection VIKINGDR4 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vikingDetection VIKINGv20111019 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID vikingDetection VIKINGv20130417 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vikingDetection VIKINGv20140402 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vikingDetection VIKINGv20150421 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vikingDetection VIKINGv20151230 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vikingDetection VIKINGv20160406 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vikingDetection VIKINGv20161202 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vikingDetection VIKINGv20170715 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vikingDetection, vikingListRemeasurement, vikingSourceRemeasurement VIKINGv20110714 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID vikingDetection, vikingMergeLog, vikingSource, vikingTilePawPrints, vikingTileSet VIKINGDR2 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID vikingMapRemeasAver VIKINGZYSELJv20170124 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID vikingMapRemeasAver, vikingMapRemeasurement, vikingZY_selJ_RemeasMergeLog VIKINGZYSELJv20160909 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID vikingTilePawTDOnly VIKINGDR2 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID vikingTilePawTDOnly VIKINGDR3 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vikingTilePawTDOnly VIKINGDR4 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vikingTilePawTDOnly VIKINGv20111019 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID vikingTilePawTDOnly VIKINGv20130417 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vikingTilePawTDOnly VIKINGv20140402 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vikingTilePawTDOnly VIKINGv20150421 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vikingTilePawTDOnly VIKINGv20151230 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vikingTilePawTDOnly VIKINGv20160406 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vikingTilePawTDOnly VIKINGv20161202 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vikingTilePawTDOnly VIKINGv20170715 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Hierarchical Triangular Mesh (HTM) index of aperture, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Hierarchical Triangular Mesh (HTM) index of aperture, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vmcDetection VMCDR2 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vmcDetection VMCDR3 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vmcDetection VMCDR4 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vmcDetection VMCv20110909 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID vmcDetection VMCv20120126 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID vmcDetection VMCv20121128 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vmcDetection VMCv20130304 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vmcDetection VMCv20130805 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vmcDetection VMCv20140428 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vmcDetection VMCv20140903 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vmcDetection VMCv20150309 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vmcDetection VMCv20151218 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vmcDetection VMCv20160311 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vmcDetection VMCv20160822 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vmcDetection VMCv20170109 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vmcDetection VMCv20170411 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vmcDetection VMCv20171101 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vmcDetection VMCv20181120 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vmcDetection VMCv20191212 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vmcDetection VMCv20210708 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vmcDetection VMCv20230816 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vmcDetection VMCv20240226 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vmcDetection, vmcListRemeasurement, vmcSourceRemeasurement VMCv20110816 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID vmcDetection, vmcMergeLog, vmcSource, vmcSynopticMergeLog, vmcSynopticSource, vmcTilePawPrints, vmcTileSet VMCDR1 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID vmcDetection, vmcPsfDetections VMCv20180702 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vmcDetection, vmcPsfSource VMCDR5 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vmcTilePawTDOnly VMCDR1 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID vmcTilePawTDOnly VMCDR2 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vmcTilePawTDOnly VMCDR3 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vmcTilePawTDOnly VMCDR4 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vmcTilePawTDOnly VMCDR5 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vmcTilePawTDOnly VMCv20110816 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID vmcTilePawTDOnly VMCv20110909 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID vmcTilePawTDOnly VMCv20120126 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID vmcTilePawTDOnly VMCv20121128 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vmcTilePawTDOnly VMCv20130304 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vmcTilePawTDOnly VMCv20130805 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vmcTilePawTDOnly VMCv20140428 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vmcTilePawTDOnly VMCv20140903 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vmcTilePawTDOnly VMCv20150309 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vmcTilePawTDOnly VMCv20151218 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vmcTilePawTDOnly VMCv20160311 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vmcTilePawTDOnly VMCv20160822 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vmcTilePawTDOnly VMCv20170109 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vmcTilePawTDOnly VMCv20170411 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vmcTilePawTDOnly VMCv20171101 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vmcTilePawTDOnly VMCv20180702 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vmcTilePawTDOnly VMCv20181120 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vmcTilePawTDOnly VMCv20191212 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vmcTilePawTDOnly VMCv20210708 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vmcTilePawTDOnly VMCv20230816 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vmcTilePawTDOnly VMCv20240226 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vmcdeepDetection VMCDEEPv20240506 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vmcdeepDetection, vmcdeepMergeLog, vmcdeepSource, vmcdeepSynopticMergeLog, vmcdeepSynopticSource, vmcdeepTilePawPrints, vmcdeepTileSet VMCDEEPv20230713 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vmcdeepTilePawTDOnly VMCDEEPv20230713 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vmcdeepTilePawTDOnly VMCDEEPv20240506 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vvvBulgeExtMapCoords EXTINCT Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vvvDetection VVVDR2 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vvvDetection, vvvDetectionPawPrints, vvvDetectionTiles, vvvParallaxCatalogue, vvvProperMotionCatalogue, vvvPsfDaophotJKsMergeLog, vvvPsfDaophotJKsSource, vvvPsfDophotZYJHKsMergeLog, vvvVivaCatalogue VVVDR5 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vvvDetection, vvvListRemeasurement, vvvSourceRemeasurement VVVv20100531 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.eq

htmID vvvDetection, vvvMergeLog, vvvSource, vvvSynopticMergeLog, vvvSynopticSource, vvvTilePawPrints, vvvTileSet VVVDR1 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vvvPsfDophotZYJHKsSource VVVDR5 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates, epoch1 bigint 8 pos.HTM

htmID vvvTilePawTDOnly VVVDR1 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vvvTilePawTDOnly VVVDR2 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID vvvTilePawTDOnly VVVDR5 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID vvvxMergeLog, vvvxSource VVVXDR1 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos.HTM

htmID wiseScosPhotoz, wiseScosPhotozRejects, wiseScosSvm WISExSCOSPZ Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htmID wise_allskysc, wise_prelimsc WISE Hierarchical Triangular Mesh (HTM) index for equatorial co-ordinates (similar to spt_ind in IPAC IRSA schema, but recomputed to level 20) bigint 8 pos.eq

htotalPeriod ultravistaMapLcVariability ULTRAVISTADR4 total period of observations (last obs-first obs) real 4 days -0.9999995e9

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

htotalPeriod ultravistaVariability ULTRAVISTADR4 total period of observations (last obs-first obs) real 4 days -0.9999995e9 time.duration

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

htotalPeriod videoVariability VIDEODR2 total period of observations (last obs-first obs) real 4 days -0.9999995e9

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

htotalPeriod videoVariability VIDEODR3 total period of observations (last obs-first obs) real 4 days -0.9999995e9 time.duration

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

htotalPeriod videoVariability VIDEODR4 total period of observations (last obs-first obs) real 4 days -0.9999995e9 time.duration

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

htotalPeriod videoVariability VIDEODR5 total period of observations (last obs-first obs) real 4 days -0.9999995e9 time.duration

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

htotalPeriod videoVariability VIDEOv20100513 total period of observations (last obs-first obs) real 4 days -0.9999995e9

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

htotalPeriod videoVariability VIDEOv20111208 total period of observations (last obs-first obs) real 4 days -0.9999995e9

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

htotalPeriod vikingVariability VIKINGDR2 total period of observations (last obs-first obs) real 4 days -0.9999995e9

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

htotalPeriod vikingVariability VIKINGv20110714 total period of observations (last obs-first obs) real 4 days -0.9999995e9

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

htotalPeriod vikingVariability VIKINGv20111019 total period of observations (last obs-first obs) real 4 days -0.9999995e9

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

htotalPeriod vvvVariability VVVDR5 total period of observations (last obs-first obs) real 4 days -0.9999995e9 time.duration

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

htotalPeriod vvvVariability VVVv20100531 total period of observations (last obs-first obs) real 4 days -0.9999995e9

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.

hVarClass ultravistaMapLcVariability ULTRAVISTADR4 Classification of variability in this band smallint 2 -9999

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hVarClass ultravistaVariability ULTRAVISTADR4 Classification of variability in this band smallint 2 -9999 meta.code.class;src.var;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hVarClass videoVariability VIDEODR2 Classification of variability in this band smallint 2 -9999

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hVarClass videoVariability VIDEODR3 Classification of variability in this band smallint 2 -9999 meta.code.class;src.var

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hVarClass videoVariability VIDEODR4 Classification of variability in this band smallint 2 -9999 meta.code.class;src.var;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hVarClass videoVariability VIDEODR5 Classification of variability in this band smallint 2 -9999 meta.code.class;src.var;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hVarClass videoVariability VIDEOv20100513 Classification of variability in this band smallint 2 -9999

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hVarClass videoVariability VIDEOv20111208 Classification of variability in this band smallint 2 -9999

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hVarClass vikingVariability VIKINGDR2 Classification of variability in this band smallint 2 -9999

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hVarClass vikingVariability VIKINGv20110714 Classification of variability in this band smallint 2 -9999

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hVarClass vikingVariability VIKINGv20111019 Classification of variability in this band smallint 2 -9999

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hVarClass vvvVariability VVVDR5 Classification of variability in this band smallint 2 -9999 meta.code.class;src.var;em.IR.H

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hVarClass vvvVariability VVVv20100531 Classification of variability in this band smallint 2 -9999

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hXi ultravistaSource ULTRAVISTADR4 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vhsSource VHSDR1 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vhsSource VHSDR2 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vhsSource VHSDR3 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vhsSource VHSDR4 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vhsSource VHSDR5 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vhsSource VHSDR6 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vhsSource VHSv20120926 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vhsSource VHSv20130417 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vhsSource VHSv20140409 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vhsSource VHSv20150108 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vhsSource VHSv20160114 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vhsSource VHSv20160507 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vhsSource VHSv20170630 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vhsSource VHSv20180419 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vhsSource VHSv20201209 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vhsSource VHSv20231101 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vhsSource VHSv20240731 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi videoSource VIDEODR2 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi videoSource VIDEODR3 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi videoSource VIDEODR4 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi videoSource VIDEODR5 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi videoSource VIDEOv20100513 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi videoSource VIDEOv20111208 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vikingSource VIKINGDR2 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vikingSource VIKINGDR3 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vikingSource VIKINGDR4 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vikingSource VIKINGv20110714 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vikingSource VIKINGv20111019 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vikingSource VIKINGv20130417 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vikingSource VIKINGv20140402 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vikingSource VIKINGv20150421 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vikingSource VIKINGv20151230 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vikingSource VIKINGv20160406 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vikingSource VIKINGv20161202 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vikingSource VIKINGv20170715 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vvvSource VVVDR2 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vvvSource VVVDR5 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vvvSource VVVv20100531 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vvvSource VVVv20110718 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vvvSource, vvvSynopticSource VVVDR1 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hXi vvvxSource VVVXDR1 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff;em.IR.H

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

WFAU, Institute for Astronomy,
Royal Observatory, Blackford Hill
Edinburgh, EH9 3HJ, UK

vsa-support@roe.ac.uk
09/12/2024