VSA Browser

Glossary of VSA attributes

This Glossary alphabetically lists all attributes used in the VSAv20240809 database(s) held in the VSA. If you would like to have more information about the schema tables please use the VSAv20240809 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

J

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

J twomass SIXDF J magnitude (JEXT) used for J selection real 4 mag

j_1AperMag1 vvvSource VVVDR5 Point source J_1 aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

j_1AperMag1Err vvvSource VVVDR5 Error in point source J_1 mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

j_1AperMag3 vikingSource VIKINGv20151230 Default point source J_1 aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

j_1AperMag3 vikingSource VIKINGv20160406 Default point source J_1 aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

j_1AperMag3 vikingSource VIKINGv20161202 Default point source J_1 aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

j_1AperMag3 vikingSource VIKINGv20170715 Default point source J_1 aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

j_1AperMag3 vvvSource VVVDR5 Default point source J_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.J

j_1AperMag3Err vikingSource VIKINGv20151230 Error in default point/extended source J_1 mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag

j_1AperMag3Err vikingSource VIKINGv20160406 Error in default point/extended source J_1 mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag

j_1AperMag3Err vikingSource VIKINGv20161202 Error in default point/extended source J_1 mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag

j_1AperMag3Err vikingSource VIKINGv20170715 Error in default point/extended source J_1 mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag

j_1AperMag3Err vvvSource VVVDR5 Error in default point source J_1 mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

j_1AperMag4 vikingSource VIKINGv20151230 Point source J_1 aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

j_1AperMag4 vikingSource VIKINGv20160406 Point source J_1 aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

j_1AperMag4 vikingSource VIKINGv20161202 Point source J_1 aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

j_1AperMag4 vikingSource VIKINGv20170715 Point source J_1 aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

j_1AperMag4 vvvSource VVVDR5 Point source J_1 aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

j_1AperMag4Err vikingSource VIKINGv20151230 Error in point/extended source J_1 mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag

j_1AperMag4Err vikingSource VIKINGv20160406 Error in point/extended source J_1 mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag

j_1AperMag4Err vikingSource VIKINGv20161202 Error in point/extended source J_1 mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag

j_1AperMag4Err vikingSource VIKINGv20170715 Error in point/extended source J_1 mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag

j_1AperMag4Err vvvSource VVVDR5 Error in point source J_1 mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

j_1AperMag6 vikingSource VIKINGv20151230 Point source J_1 aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

j_1AperMag6 vikingSource VIKINGv20160406 Point source J_1 aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

j_1AperMag6 vikingSource VIKINGv20161202 Point source J_1 aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

j_1AperMag6 vikingSource VIKINGv20170715 Point source J_1 aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

j_1AperMag6Err vikingSource VIKINGv20151230 Error in point/extended source J_1 mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag

j_1AperMag6Err vikingSource VIKINGv20160406 Error in point/extended source J_1 mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag

j_1AperMag6Err vikingSource VIKINGv20161202 Error in point/extended source J_1 mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag

j_1AperMag6Err vikingSource VIKINGv20170715 Error in point/extended source J_1 mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag

j_1AperMagNoAperCorr3 vikingSource VIKINGv20151230 Default extended source J_1 aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

j_1AperMagNoAperCorr3 vikingSource VIKINGv20160406 Default extended source J_1 aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

j_1AperMagNoAperCorr3 vikingSource VIKINGv20161202 Default extended source J_1 aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

j_1AperMagNoAperCorr3 vikingSource VIKINGv20170715 Default extended source J_1 aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

j_1AperMagNoAperCorr4 vikingSource VIKINGv20151230 Extended source J_1 aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

j_1AperMagNoAperCorr4 vikingSource VIKINGv20160406 Extended source J_1 aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

j_1AperMagNoAperCorr4 vikingSource VIKINGv20161202 Extended source J_1 aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

j_1AperMagNoAperCorr4 vikingSource VIKINGv20170715 Extended source J_1 aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

j_1AperMagNoAperCorr6 vikingSource VIKINGv20151230 Extended source J_1 aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

j_1AperMagNoAperCorr6 vikingSource VIKINGv20160406 Extended source J_1 aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

j_1AperMagNoAperCorr6 vikingSource VIKINGv20161202 Extended source J_1 aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

j_1AperMagNoAperCorr6 vikingSource VIKINGv20170715 Extended source J_1 aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

j_1AverageConf vikingSource VIKINGv20151230 average confidence in 2 arcsec diameter default aperture (aper3) J_1 real 4 -0.9999995e9 stat.likelihood

j_1AverageConf vikingSource VIKINGv20160406 average confidence in 2 arcsec diameter default aperture (aper3) J_1 real 4 -0.9999995e9 stat.likelihood

j_1AverageConf vikingSource VIKINGv20161202 average confidence in 2 arcsec diameter default aperture (aper3) J_1 real 4 -0.9999995e9 stat.likelihood

j_1AverageConf vikingSource VIKINGv20170715 average confidence in 2 arcsec diameter default aperture (aper3) J_1 real 4 -0.9999995e9 stat.likelihood

j_1AverageConf vvvSource VVVDR5 average confidence in 2 arcsec diameter default aperture (aper3) J_1 real 4 -0.9999995e9 stat.likelihood;em.IR.J

j_1Class vikingSource VIKINGv20151230 discrete image classification flag in J_1 smallint 2 -9999 src.class

j_1Class vikingSource VIKINGv20160406 discrete image classification flag in J_1 smallint 2 -9999 src.class

j_1Class vikingSource VIKINGv20161202 discrete image classification flag in J_1 smallint 2 -9999 src.class

j_1Class vikingSource VIKINGv20170715 discrete image classification flag in J_1 smallint 2 -9999 src.class

j_1Class vvvSource VVVDR5 discrete image classification flag in J_1 smallint 2 -9999 src.class;em.IR.J

j_1ClassStat vikingSource VIKINGv20151230 N(0,1) stellarness-of-profile statistic in J_1 real 4 -0.9999995e9 stat

j_1ClassStat vikingSource VIKINGv20160406 N(0,1) stellarness-of-profile statistic in J_1 real 4 -0.9999995e9 stat

j_1ClassStat vikingSource VIKINGv20161202 N(0,1) stellarness-of-profile statistic in J_1 real 4 -0.9999995e9 stat

j_1ClassStat vikingSource VIKINGv20170715 N(0,1) stellarness-of-profile statistic in J_1 real 4 -0.9999995e9 stat

j_1ClassStat vvvSource VVVDR5 S-Extractor classification statistic in J_1 real 4 -0.9999995e9 stat;em.IR.J

j_1Ell vikingSource VIKINGv20151230 1-b/a, where a/b=semi-major/minor axes in J_1 real 4 -0.9999995e9 src.ellipticity

j_1Ell vikingSource VIKINGv20160406 1-b/a, where a/b=semi-major/minor axes in J_1 real 4 -0.9999995e9 src.ellipticity

j_1Ell vikingSource VIKINGv20161202 1-b/a, where a/b=semi-major/minor axes in J_1 real 4 -0.9999995e9 src.ellipticity

j_1Ell vikingSource VIKINGv20170715 1-b/a, where a/b=semi-major/minor axes in J_1 real 4 -0.9999995e9 src.ellipticity

j_1Ell vvvSource VVVDR5 1-b/a, where a/b=semi-major/minor axes in J_1 real 4 -0.9999995e9 src.ellipticity;em.IR.J

j_1eNum vikingMergeLog VIKINGv20151230 the extension number of this J_1 frame tinyint 1 meta.number

j_1eNum vikingMergeLog VIKINGv20160406 the extension number of this J_1 frame tinyint 1 meta.number

j_1eNum vikingMergeLog VIKINGv20161202 the extension number of this J_1 frame tinyint 1 meta.number

j_1eNum vikingMergeLog VIKINGv20170715 the extension number of this J_1 frame tinyint 1 meta.number

j_1eNum vvvMergeLog VVVDR5 the extension number of this J_1 frame tinyint 1 meta.number;em.IR.J

j_1eNum vvvPsfDophotZYJHKsMergeLog VVVDR5 the extension number of this 1st epoch J frame tinyint 1 meta.number;em.IR.J

j_1ErrBits vikingSource VIKINGv20151230 processing warning/error bitwise flags in J_1 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.

j_1ErrBits vikingSource VIKINGv20160406 processing warning/error bitwise flags in J_1 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.

j_1ErrBits vikingSource VIKINGv20161202 processing warning/error bitwise flags in J_1 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.

j_1ErrBits vikingSource VIKINGv20170715 processing warning/error bitwise flags in J_1 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.

j_1ErrBits vvvSource VVVDR5 processing warning/error bitwise flags in J_1 int 4 -99999999 meta.code;em.IR.J

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

j_1Eta vikingSource VIKINGv20151230 Offset of J_1 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.

j_1Eta vikingSource VIKINGv20160406 Offset of J_1 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.

j_1Eta vikingSource VIKINGv20161202 Offset of J_1 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.

j_1Eta vikingSource VIKINGv20170715 Offset of J_1 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.

j_1Eta vvvSource VVVDR5 Offset of J_1 detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.J

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.

j_1Gausig vikingSource VIKINGv20151230 RMS of axes of ellipse fit in J_1 real 4 pixels -0.9999995e9 src.morph.param

j_1Gausig vikingSource VIKINGv20160406 RMS of axes of ellipse fit in J_1 real 4 pixels -0.9999995e9 src.morph.param

j_1Gausig vikingSource VIKINGv20161202 RMS of axes of ellipse fit in J_1 real 4 pixels -0.9999995e9 src.morph.param

j_1Gausig vikingSource VIKINGv20170715 RMS of axes of ellipse fit in J_1 real 4 pixels -0.9999995e9 src.morph.param

j_1Gausig vvvSource VVVDR5 RMS of axes of ellipse fit in J_1 real 4 pixels -0.9999995e9 src.morph.param;em.IR.J

j_1HlCorSMjRadAs vikingSource VIKINGv20151230 Seeing corrected half-light, semi-major axis in J_1 band real 4 arcsec -0.9999995e9 phys.angSize

j_1HlCorSMjRadAs vikingSource VIKINGv20160406 Seeing corrected half-light, semi-major axis in J_1 band real 4 arcsec -0.9999995e9 phys.angSize

j_1HlCorSMjRadAs vikingSource VIKINGv20161202 Seeing corrected half-light, semi-major axis in J_1 band real 4 arcsec -0.9999995e9 phys.angSize

j_1HlCorSMjRadAs vikingSource VIKINGv20170715 Seeing corrected half-light, semi-major axis in J_1 band real 4 arcsec -0.9999995e9 phys.angSize

j_1mfID vikingMergeLog VIKINGv20151230 the UID of the relevant J_1 multiframe bigint 8 meta.id;obs.field

j_1mfID vikingMergeLog VIKINGv20160406 the UID of the relevant J_1 multiframe bigint 8 meta.id;obs.field

j_1mfID vikingMergeLog VIKINGv20161202 the UID of the relevant J_1 multiframe bigint 8 meta.id;obs.field

j_1mfID vikingMergeLog VIKINGv20170715 the UID of the relevant J_1 multiframe bigint 8 meta.id;obs.field

j_1mfID vvvMergeLog VVVDR5 the UID of the relevant J_1 multiframe bigint 8 meta.id;obs.field;em.IR.J

j_1mfID vvvPsfDophotZYJHKsMergeLog VVVDR5 the UID of the relevant 1st epoch J tile multiframe bigint 8 meta.id;obs.field;em.IR.J

j_1mh_1Pnt vvvSource VVVDR5 Point source colour J_1-H_1 (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.J;em.IR.H

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.

j_1mh_1PntErr vvvSource VVVDR5 Error on point source colour J_1-H_1 real 4 mag -0.9999995e9 stat.error;em.IR.J;em.IR.H

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.

j_1mhExt vikingSource VIKINGv20151230 Extended source colour J_1-H (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color;em.IR.H

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.

j_1mhExt vikingSource VIKINGv20160406 Extended source colour J_1-H (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color;em.IR.H

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.

j_1mhExt vikingSource VIKINGv20161202 Extended source colour J_1-H (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color;em.IR.H

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.

j_1mhExt vikingSource VIKINGv20170715 Extended source colour J_1-H (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color;em.IR.H

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.

j_1mhExtErr vikingSource VIKINGv20151230 Error on extended source colour J_1-H real 4 mag -0.9999995e9 stat.error;em.IR.H

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.

j_1mhExtErr vikingSource VIKINGv20160406 Error on extended source colour J_1-H real 4 mag -0.9999995e9 stat.error;em.IR.H

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.

j_1mhExtErr vikingSource VIKINGv20161202 Error on extended source colour J_1-H real 4 mag -0.9999995e9 stat.error;em.IR.H

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.

j_1mhExtErr vikingSource VIKINGv20170715 Error on extended source colour J_1-H real 4 mag -0.9999995e9 stat.error;em.IR.H

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.

j_1mhPnt vikingSource VIKINGv20151230 Point source colour J_1-H (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H

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.

j_1mhPnt vikingSource VIKINGv20160406 Point source colour J_1-H (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H

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.

j_1mhPnt vikingSource VIKINGv20161202 Point source colour J_1-H (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H

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.

j_1mhPnt vikingSource VIKINGv20170715 Point source colour J_1-H (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H

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.

j_1mhPntErr vikingSource VIKINGv20151230 Error on point source colour J_1-H real 4 mag -0.9999995e9 stat.error;em.IR.H

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.

j_1mhPntErr vikingSource VIKINGv20160406 Error on point source colour J_1-H real 4 mag -0.9999995e9 stat.error;em.IR.H

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.

j_1mhPntErr vikingSource VIKINGv20161202 Error on point source colour J_1-H real 4 mag -0.9999995e9 stat.error;em.IR.H

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.

j_1mhPntErr vikingSource VIKINGv20170715 Error on point source colour J_1-H real 4 mag -0.9999995e9 stat.error;em.IR.H

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.

j_1Mjd vikingSource VIKINGv20151230 Modified Julian Day in J_1 band float 8 days -0.9999995e9 time.epoch

j_1Mjd vikingSource VIKINGv20160406 Modified Julian Day in J_1 band float 8 days -0.9999995e9 time.epoch

j_1Mjd vikingSource VIKINGv20161202 Modified Julian Day in J_1 band float 8 days -0.9999995e9 time.epoch

j_1Mjd vikingSource VIKINGv20170715 Modified Julian Day in J_1 band float 8 days -0.9999995e9 time.epoch

j_1Mjd vvvPsfDophotZYJHKsMergeLog VVVDR5 the MJD of the 1st epoch J tile multiframe float 8 time;em.IR.J

j_1Mjd vvvSource VVVDR5 Modified Julian Day in J_1 band float 8 days -0.9999995e9 time.epoch;em.IR.J

j_1PA vikingSource VIKINGv20151230 ellipse fit celestial orientation in J_1 real 4 Degrees -0.9999995e9 pos.posAng

j_1PA vikingSource VIKINGv20160406 ellipse fit celestial orientation in J_1 real 4 Degrees -0.9999995e9 pos.posAng

j_1PA vikingSource VIKINGv20161202 ellipse fit celestial orientation in J_1 real 4 Degrees -0.9999995e9 pos.posAng

j_1PA vikingSource VIKINGv20170715 ellipse fit celestial orientation in J_1 real 4 Degrees -0.9999995e9 pos.posAng

j_1PA vvvSource VVVDR5 ellipse fit celestial orientation in J_1 real 4 Degrees -0.9999995e9 pos.posAng;em.IR.J

j_1PetroMag vikingSource VIKINGv20151230 Extended source J_1 mag (Petrosian) real 4 mag -0.9999995e9 phot.mag

j_1PetroMag vikingSource VIKINGv20160406 Extended source J_1 mag (Petrosian) real 4 mag -0.9999995e9 phot.mag

j_1PetroMag vikingSource VIKINGv20161202 Extended source J_1 mag (Petrosian) real 4 mag -0.9999995e9 phot.mag

j_1PetroMag vikingSource VIKINGv20170715 Extended source J_1 mag (Petrosian) real 4 mag -0.9999995e9 phot.mag

j_1PetroMagErr vikingSource VIKINGv20151230 Error in extended source J_1 mag (Petrosian) real 4 mag -0.9999995e9 stat.error;phot.mag

j_1PetroMagErr vikingSource VIKINGv20160406 Error in extended source J_1 mag (Petrosian) real 4 mag -0.9999995e9 stat.error;phot.mag

j_1PetroMagErr vikingSource VIKINGv20161202 Error in extended source J_1 mag (Petrosian) real 4 mag -0.9999995e9 stat.error;phot.mag

j_1PetroMagErr vikingSource VIKINGv20170715 Error in extended source J_1 mag (Petrosian) real 4 mag -0.9999995e9 stat.error;phot.mag

j_1ppErrBits vikingSource VIKINGv20151230 additional WFAU post-processing error bits in J_1 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.

j_1ppErrBits vikingSource VIKINGv20160406 additional WFAU post-processing error bits in J_1 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.

j_1ppErrBits vikingSource VIKINGv20161202 additional WFAU post-processing error bits in J_1 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.

j_1ppErrBits vikingSource VIKINGv20170715 additional WFAU post-processing error bits in J_1 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.

j_1ppErrBits vvvSource VVVDR5 additional WFAU post-processing error bits in J_1 int 4 0 meta.code;em.IR.J

j_1PsfMag vikingSource VIKINGv20151230 Point source profile-fitted J_1 mag real 4 mag -0.9999995e9 phot.mag

j_1PsfMag vikingSource VIKINGv20160406 Point source profile-fitted J_1 mag real 4 mag -0.9999995e9 phot.mag

j_1PsfMag vikingSource VIKINGv20161202 Point source profile-fitted J_1 mag real 4 mag -0.9999995e9 phot.mag

j_1PsfMag vikingSource VIKINGv20170715 Point source profile-fitted J_1 mag real 4 mag -0.9999995e9 phot.mag

j_1PsfMagErr vikingSource VIKINGv20151230 Error in point source profile-fitted J_1 mag real 4 mag -0.9999995e9 stat.error;phot.mag

j_1PsfMagErr vikingSource VIKINGv20160406 Error in point source profile-fitted J_1 mag real 4 mag -0.9999995e9 stat.error;phot.mag

j_1PsfMagErr vikingSource VIKINGv20161202 Error in point source profile-fitted J_1 mag real 4 mag -0.9999995e9 stat.error;phot.mag

j_1PsfMagErr vikingSource VIKINGv20170715 Error in point source profile-fitted J_1 mag real 4 mag -0.9999995e9 stat.error;phot.mag

j_1SeqNum vikingSource VIKINGv20151230 the running number of the J_1 detection int 4 -99999999 meta.number

j_1SeqNum vikingSource VIKINGv20160406 the running number of the J_1 detection int 4 -99999999 meta.number

j_1SeqNum vikingSource VIKINGv20161202 the running number of the J_1 detection int 4 -99999999 meta.number

j_1SeqNum vikingSource VIKINGv20170715 the running number of the J_1 detection int 4 -99999999 meta.number

j_1SeqNum vvvSource VVVDR5 the running number of the J_1 detection int 4 -99999999 meta.number;em.IR.J

j_1SerMag2D vikingSource VIKINGv20151230 Extended source J_1 mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag

j_1SerMag2D vikingSource VIKINGv20160406 Extended source J_1 mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag

j_1SerMag2D vikingSource VIKINGv20161202 Extended source J_1 mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag

j_1SerMag2D vikingSource VIKINGv20170715 Extended source J_1 mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag

j_1SerMag2DErr vikingSource VIKINGv20151230 Error in extended source J_1 mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;phot.mag

j_1SerMag2DErr vikingSource VIKINGv20160406 Error in extended source J_1 mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;phot.mag

j_1SerMag2DErr vikingSource VIKINGv20161202 Error in extended source J_1 mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;phot.mag

j_1SerMag2DErr vikingSource VIKINGv20170715 Error in extended source J_1 mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;phot.mag

j_1Xi vikingSource VIKINGv20151230 Offset of J_1 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.

j_1Xi vikingSource VIKINGv20160406 Offset of J_1 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.

j_1Xi vikingSource VIKINGv20161202 Offset of J_1 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.

j_1Xi vikingSource VIKINGv20170715 Offset of J_1 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.

j_1Xi vvvSource VVVDR5 Offset of J_1 detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff;em.IR.J

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.

j_2AperMag1 vvvSource VVVDR5 Point source J_2 aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

j_2AperMag1Err vvvSource VVVDR5 Error in point source J_2 mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

j_2AperMag3 vikingSource VIKINGv20151230 Default point source J_2 aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

j_2AperMag3 vikingSource VIKINGv20160406 Default point source J_2 aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

j_2AperMag3 vikingSource VIKINGv20161202 Default point source J_2 aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

j_2AperMag3 vikingSource VIKINGv20170715 Default point source J_2 aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

j_2AperMag3 vvvSource VVVDR5 Default point source J_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.J

j_2AperMag3Err vikingSource VIKINGv20151230 Error in default point/extended source J_2 mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag

j_2AperMag3Err vikingSource VIKINGv20160406 Error in default point/extended source J_2 mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag

j_2AperMag3Err vikingSource VIKINGv20161202 Error in default point/extended source J_2 mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag

j_2AperMag3Err vikingSource VIKINGv20170715 Error in default point/extended source J_2 mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag

j_2AperMag3Err vvvSource VVVDR5 Error in default point source J_2 mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

j_2AperMag4 vikingSource VIKINGv20151230 Point source J_2 aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

j_2AperMag4 vikingSource VIKINGv20160406 Point source J_2 aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

j_2AperMag4 vikingSource VIKINGv20161202 Point source J_2 aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

j_2AperMag4 vikingSource VIKINGv20170715 Point source J_2 aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

j_2AperMag4 vvvSource VVVDR5 Point source J_2 aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

j_2AperMag4Err vikingSource VIKINGv20151230 Error in point/extended source J_2 mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag

j_2AperMag4Err vikingSource VIKINGv20160406 Error in point/extended source J_2 mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag

j_2AperMag4Err vikingSource VIKINGv20161202 Error in point/extended source J_2 mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag

j_2AperMag4Err vikingSource VIKINGv20170715 Error in point/extended source J_2 mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag

j_2AperMag4Err vvvSource VVVDR5 Error in point source J_2 mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

j_2AperMag6 vikingSource VIKINGv20151230 Point source J_2 aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

j_2AperMag6 vikingSource VIKINGv20160406 Point source J_2 aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

j_2AperMag6 vikingSource VIKINGv20161202 Point source J_2 aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

j_2AperMag6 vikingSource VIKINGv20170715 Point source J_2 aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

j_2AperMag6Err vikingSource VIKINGv20151230 Error in point/extended source J_2 mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag

j_2AperMag6Err vikingSource VIKINGv20160406 Error in point/extended source J_2 mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag

j_2AperMag6Err vikingSource VIKINGv20161202 Error in point/extended source J_2 mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag

j_2AperMag6Err vikingSource VIKINGv20170715 Error in point/extended source J_2 mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag

j_2AperMagNoAperCorr3 vikingSource VIKINGv20151230 Default extended source J_2 aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

j_2AperMagNoAperCorr3 vikingSource VIKINGv20160406 Default extended source J_2 aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

j_2AperMagNoAperCorr3 vikingSource VIKINGv20161202 Default extended source J_2 aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

j_2AperMagNoAperCorr3 vikingSource VIKINGv20170715 Default extended source J_2 aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

j_2AperMagNoAperCorr4 vikingSource VIKINGv20151230 Extended source J_2 aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

j_2AperMagNoAperCorr4 vikingSource VIKINGv20160406 Extended source J_2 aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

j_2AperMagNoAperCorr4 vikingSource VIKINGv20161202 Extended source J_2 aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

j_2AperMagNoAperCorr4 vikingSource VIKINGv20170715 Extended source J_2 aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

j_2AperMagNoAperCorr6 vikingSource VIKINGv20151230 Extended source J_2 aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

j_2AperMagNoAperCorr6 vikingSource VIKINGv20160406 Extended source J_2 aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

j_2AperMagNoAperCorr6 vikingSource VIKINGv20161202 Extended source J_2 aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

j_2AperMagNoAperCorr6 vikingSource VIKINGv20170715 Extended source J_2 aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

j_2AverageConf vikingSource VIKINGv20151230 average confidence in 2 arcsec diameter default aperture (aper3) J_2 real 4 -0.9999995e9 stat.likelihood

j_2AverageConf vikingSource VIKINGv20160406 average confidence in 2 arcsec diameter default aperture (aper3) J_2 real 4 -0.9999995e9 stat.likelihood

j_2AverageConf vikingSource VIKINGv20161202 average confidence in 2 arcsec diameter default aperture (aper3) J_2 real 4 -0.9999995e9 stat.likelihood

j_2AverageConf vikingSource VIKINGv20170715 average confidence in 2 arcsec diameter default aperture (aper3) J_2 real 4 -0.9999995e9 stat.likelihood

j_2AverageConf vvvSource VVVDR5 average confidence in 2 arcsec diameter default aperture (aper3) J_2 real 4 -0.9999995e9 stat.likelihood;em.IR.J

j_2Class vikingSource VIKINGv20151230 discrete image classification flag in J_2 smallint 2 -9999 src.class

j_2Class vikingSource VIKINGv20160406 discrete image classification flag in J_2 smallint 2 -9999 src.class

j_2Class vikingSource VIKINGv20161202 discrete image classification flag in J_2 smallint 2 -9999 src.class

j_2Class vikingSource VIKINGv20170715 discrete image classification flag in J_2 smallint 2 -9999 src.class

j_2Class vvvSource VVVDR5 discrete image classification flag in J_2 smallint 2 -9999 src.class;em.IR.J

j_2ClassStat vikingSource VIKINGv20151230 N(0,1) stellarness-of-profile statistic in J_2 real 4 -0.9999995e9 stat

j_2ClassStat vikingSource VIKINGv20160406 N(0,1) stellarness-of-profile statistic in J_2 real 4 -0.9999995e9 stat

j_2ClassStat vikingSource VIKINGv20161202 N(0,1) stellarness-of-profile statistic in J_2 real 4 -0.9999995e9 stat

j_2ClassStat vikingSource VIKINGv20170715 N(0,1) stellarness-of-profile statistic in J_2 real 4 -0.9999995e9 stat

j_2ClassStat vvvSource VVVDR5 S-Extractor classification statistic in J_2 real 4 -0.9999995e9 stat;em.IR.J

j_2Ell vikingSource VIKINGv20151230 1-b/a, where a/b=semi-major/minor axes in J_2 real 4 -0.9999995e9 src.ellipticity

j_2Ell vikingSource VIKINGv20160406 1-b/a, where a/b=semi-major/minor axes in J_2 real 4 -0.9999995e9 src.ellipticity

j_2Ell vikingSource VIKINGv20161202 1-b/a, where a/b=semi-major/minor axes in J_2 real 4 -0.9999995e9 src.ellipticity

j_2Ell vikingSource VIKINGv20170715 1-b/a, where a/b=semi-major/minor axes in J_2 real 4 -0.9999995e9 src.ellipticity

j_2Ell vvvSource VVVDR5 1-b/a, where a/b=semi-major/minor axes in J_2 real 4 -0.9999995e9 src.ellipticity;em.IR.J

j_2eNum vikingMergeLog VIKINGv20151230 the extension number of this J_2 frame tinyint 1 meta.number

j_2eNum vikingMergeLog VIKINGv20160406 the extension number of this J_2 frame tinyint 1 meta.number

j_2eNum vikingMergeLog VIKINGv20161202 the extension number of this J_2 frame tinyint 1 meta.number

j_2eNum vikingMergeLog VIKINGv20170715 the extension number of this J_2 frame tinyint 1 meta.number

j_2eNum vvvMergeLog VVVDR5 the extension number of this J_2 frame tinyint 1 meta.number;em.IR.J

j_2eNum vvvPsfDophotZYJHKsMergeLog VVVDR5 the extension number of this 2nd epoch J frame tinyint 1 meta.number;em.IR.J

j_2ErrBits vikingSource VIKINGv20151230 processing warning/error bitwise flags in J_2 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.

j_2ErrBits vikingSource VIKINGv20160406 processing warning/error bitwise flags in J_2 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.

j_2ErrBits vikingSource VIKINGv20161202 processing warning/error bitwise flags in J_2 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.

j_2ErrBits vikingSource VIKINGv20170715 processing warning/error bitwise flags in J_2 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.

j_2ErrBits vvvSource VVVDR5 processing warning/error bitwise flags in J_2 int 4 -99999999 meta.code;em.IR.J

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

j_2Eta vikingSource VIKINGv20151230 Offset of J_2 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.

j_2Eta vikingSource VIKINGv20160406 Offset of J_2 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.

j_2Eta vikingSource VIKINGv20161202 Offset of J_2 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.

j_2Eta vikingSource VIKINGv20170715 Offset of J_2 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.

j_2Eta vvvSource VVVDR5 Offset of J_2 detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.J

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.

j_2Gausig vikingSource VIKINGv20151230 RMS of axes of ellipse fit in J_2 real 4 pixels -0.9999995e9 src.morph.param

j_2Gausig vikingSource VIKINGv20160406 RMS of axes of ellipse fit in J_2 real 4 pixels -0.9999995e9 src.morph.param

j_2Gausig vikingSource VIKINGv20161202 RMS of axes of ellipse fit in J_2 real 4 pixels -0.9999995e9 src.morph.param

j_2Gausig vikingSource VIKINGv20170715 RMS of axes of ellipse fit in J_2 real 4 pixels -0.9999995e9 src.morph.param

j_2Gausig vvvSource VVVDR5 RMS of axes of ellipse fit in J_2 real 4 pixels -0.9999995e9 src.morph.param;em.IR.J

j_2HlCorSMjRadAs vikingSource VIKINGv20151230 Seeing corrected half-light, semi-major axis in J_2 band real 4 arcsec -0.9999995e9 phys.angSize

j_2HlCorSMjRadAs vikingSource VIKINGv20160406 Seeing corrected half-light, semi-major axis in J_2 band real 4 arcsec -0.9999995e9 phys.angSize

j_2HlCorSMjRadAs vikingSource VIKINGv20161202 Seeing corrected half-light, semi-major axis in J_2 band real 4 arcsec -0.9999995e9 phys.angSize

j_2HlCorSMjRadAs vikingSource VIKINGv20170715 Seeing corrected half-light, semi-major axis in J_2 band real 4 arcsec -0.9999995e9 phys.angSize

j_2mfID vikingMergeLog VIKINGv20151230 the UID of the relevant J_2 multiframe bigint 8 meta.id;obs.field

j_2mfID vikingMergeLog VIKINGv20160406 the UID of the relevant J_2 multiframe bigint 8 meta.id;obs.field

j_2mfID vikingMergeLog VIKINGv20161202 the UID of the relevant J_2 multiframe bigint 8 meta.id;obs.field

j_2mfID vikingMergeLog VIKINGv20170715 the UID of the relevant J_2 multiframe bigint 8 meta.id;obs.field

j_2mfID vvvMergeLog VVVDR5 the UID of the relevant J_2 multiframe bigint 8 meta.id;obs.field;em.IR.J

j_2mfID vvvPsfDophotZYJHKsMergeLog VVVDR5 the UID of the relevant 2nd epoch J tile multiframe bigint 8 meta.id;obs.field;em.IR.J

j_2mh_2Pnt vvvSource VVVDR5 Point source colour J_2-H_2 (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.J;em.IR.H

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.

j_2mh_2PntErr vvvSource VVVDR5 Error on point source colour J_2-H_2 real 4 mag -0.9999995e9 stat.error;em.IR.J;em.IR.H

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.

j_2Mjd vikingSource VIKINGv20151230 Modified Julian Day in J_2 band float 8 days -0.9999995e9 time.epoch

j_2Mjd vikingSource VIKINGv20160406 Modified Julian Day in J_2 band float 8 days -0.9999995e9 time.epoch

j_2Mjd vikingSource VIKINGv20161202 Modified Julian Day in J_2 band float 8 days -0.9999995e9 time.epoch

j_2Mjd vikingSource VIKINGv20170715 Modified Julian Day in J_2 band float 8 days -0.9999995e9 time.epoch

j_2Mjd vvvPsfDophotZYJHKsMergeLog VVVDR5 the MJD of the 2nd epoch J tile multiframe float 8 time;em.IR.J

j_2Mjd vvvSource VVVDR5 Modified Julian Day in J_2 band float 8 days -0.9999995e9 time.epoch;em.IR.J

j_2mrat twomass_scn TWOMASS J-band average 2nd image moment ratio. real 4 stat.fit.param

j_2mrat twomass_sixx2_scn TWOMASS J band average 2nd image moment ratio for scan real 4

j_2PA vikingSource VIKINGv20151230 ellipse fit celestial orientation in J_2 real 4 Degrees -0.9999995e9 pos.posAng

j_2PA vikingSource VIKINGv20160406 ellipse fit celestial orientation in J_2 real 4 Degrees -0.9999995e9 pos.posAng

j_2PA vikingSource VIKINGv20161202 ellipse fit celestial orientation in J_2 real 4 Degrees -0.9999995e9 pos.posAng

j_2PA vikingSource VIKINGv20170715 ellipse fit celestial orientation in J_2 real 4 Degrees -0.9999995e9 pos.posAng

j_2PA vvvSource VVVDR5 ellipse fit celestial orientation in J_2 real 4 Degrees -0.9999995e9 pos.posAng;em.IR.J

j_2PetroMag vikingSource VIKINGv20151230 Extended source J_2 mag (Petrosian) real 4 mag -0.9999995e9 phot.mag

j_2PetroMag vikingSource VIKINGv20160406 Extended source J_2 mag (Petrosian) real 4 mag -0.9999995e9 phot.mag

j_2PetroMag vikingSource VIKINGv20161202 Extended source J_2 mag (Petrosian) real 4 mag -0.9999995e9 phot.mag

j_2PetroMag vikingSource VIKINGv20170715 Extended source J_2 mag (Petrosian) real 4 mag -0.9999995e9 phot.mag

j_2PetroMagErr vikingSource VIKINGv20151230 Error in extended source J_2 mag (Petrosian) real 4 mag -0.9999995e9 stat.error;phot.mag

j_2PetroMagErr vikingSource VIKINGv20160406 Error in extended source J_2 mag (Petrosian) real 4 mag -0.9999995e9 stat.error;phot.mag

j_2PetroMagErr vikingSource VIKINGv20161202 Error in extended source J_2 mag (Petrosian) real 4 mag -0.9999995e9 stat.error;phot.mag

j_2PetroMagErr vikingSource VIKINGv20170715 Error in extended source J_2 mag (Petrosian) real 4 mag -0.9999995e9 stat.error;phot.mag

j_2ppErrBits vikingSource VIKINGv20151230 additional WFAU post-processing error bits in J_2 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.

j_2ppErrBits vikingSource VIKINGv20160406 additional WFAU post-processing error bits in J_2 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.

j_2ppErrBits vikingSource VIKINGv20161202 additional WFAU post-processing error bits in J_2 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.

j_2ppErrBits vikingSource VIKINGv20170715 additional WFAU post-processing error bits in J_2 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.

j_2ppErrBits vvvSource VVVDR5 additional WFAU post-processing error bits in J_2 int 4 0 meta.code;em.IR.J

j_2PsfMag vikingSource VIKINGv20151230 Point source profile-fitted J_2 mag real 4 mag -0.9999995e9 phot.mag

j_2PsfMag vikingSource VIKINGv20160406 Point source profile-fitted J_2 mag real 4 mag -0.9999995e9 phot.mag

j_2PsfMag vikingSource VIKINGv20161202 Point source profile-fitted J_2 mag real 4 mag -0.9999995e9 phot.mag

j_2PsfMag vikingSource VIKINGv20170715 Point source profile-fitted J_2 mag real 4 mag -0.9999995e9 phot.mag

j_2PsfMagErr vikingSource VIKINGv20151230 Error in point source profile-fitted J_2 mag real 4 mag -0.9999995e9 stat.error;phot.mag

j_2PsfMagErr vikingSource VIKINGv20160406 Error in point source profile-fitted J_2 mag real 4 mag -0.9999995e9 stat.error;phot.mag

j_2PsfMagErr vikingSource VIKINGv20161202 Error in point source profile-fitted J_2 mag real 4 mag -0.9999995e9 stat.error;phot.mag

j_2PsfMagErr vikingSource VIKINGv20170715 Error in point source profile-fitted J_2 mag real 4 mag -0.9999995e9 stat.error;phot.mag

j_2SeqNum vikingSource VIKINGv20151230 the running number of the J_2 detection int 4 -99999999 meta.number

j_2SeqNum vikingSource VIKINGv20160406 the running number of the J_2 detection int 4 -99999999 meta.number

j_2SeqNum vikingSource VIKINGv20161202 the running number of the J_2 detection int 4 -99999999 meta.number

j_2SeqNum vikingSource VIKINGv20170715 the running number of the J_2 detection int 4 -99999999 meta.number

j_2SeqNum vvvSource VVVDR5 the running number of the J_2 detection int 4 -99999999 meta.number;em.IR.J

j_2SerMag2D vikingSource VIKINGv20151230 Extended source J_2 mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag

j_2SerMag2D vikingSource VIKINGv20160406 Extended source J_2 mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag

j_2SerMag2D vikingSource VIKINGv20161202 Extended source J_2 mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag

j_2SerMag2D vikingSource VIKINGv20170715 Extended source J_2 mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag

j_2SerMag2DErr vikingSource VIKINGv20151230 Error in extended source J_2 mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;phot.mag

j_2SerMag2DErr vikingSource VIKINGv20160406 Error in extended source J_2 mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;phot.mag

j_2SerMag2DErr vikingSource VIKINGv20161202 Error in extended source J_2 mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;phot.mag

j_2SerMag2DErr vikingSource VIKINGv20170715 Error in extended source J_2 mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;phot.mag

j_2Xi vikingSource VIKINGv20151230 Offset of J_2 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.

j_2Xi vikingSource VIKINGv20160406 Offset of J_2 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.

j_2Xi vikingSource VIKINGv20161202 Offset of J_2 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.

j_2Xi vikingSource VIKINGv20170715 Offset of J_2 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.

j_2Xi vvvSource VVVDR5 Offset of J_2 detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff;em.IR.J

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.

j_5sig_ba twomass_xsc TWOMASS J minor/major axis ratio fit to the 5-sigma isophote. real 4 phys.size.axisRatio

j_5sig_phi twomass_xsc TWOMASS J angle to 5-sigma major axis (E of N). smallint 2 degrees stat.error

j_5surf twomass_xsc TWOMASS J central surface brightness (r<=5). real 4 mag phot.mag.sb

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

j_back twomass_xsc TWOMASS J coadd median background. real 4 meta.code

j_bisym_chi twomass_xsc TWOMASS J bi-symmetric cross-correlation chi. real 4 stat.fit.param

j_bisym_rat twomass_xsc TWOMASS J bi-symmetric flux ratio. real 4 phot.flux;arith.ratio

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

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

j_chif_ellf twomass_xsc TWOMASS J % chi-fraction for elliptical fit to 3-sig isophote. real 4 stat.fit.param

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

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

j_d_area twomass_xsc TWOMASS J 5-sigma to 3-sigma differential area. smallint 2 stat.fit.residual

j_flg_10 twomass_xsc TWOMASS J confusion flag for 10 arcsec circular ap. mag. smallint 2 meta.code

j_flg_15 twomass_xsc TWOMASS J confusion flag for 15 arcsec circular ap. mag. smallint 2 meta.code

j_flg_20 twomass_xsc TWOMASS J confusion flag for 20 arcsec circular ap. mag. smallint 2 meta.code

j_flg_25 twomass_xsc TWOMASS J confusion flag for 25 arcsec circular ap. mag. smallint 2 meta.code

j_flg_30 twomass_xsc TWOMASS J confusion flag for 30 arcsec circular ap. mag. smallint 2 meta.code

j_flg_40 twomass_xsc TWOMASS J confusion flag for 40 arcsec circular ap. mag. smallint 2 meta.code

j_flg_5 twomass_xsc TWOMASS J confusion flag for 5 arcsec circular ap. mag. smallint 2 meta.code

j_flg_50 twomass_xsc TWOMASS J confusion flag for 50 arcsec circular ap. mag. smallint 2 meta.code

j_flg_60 twomass_xsc TWOMASS J confusion flag for 60 arcsec circular ap. mag. smallint 2 meta.code

j_flg_7 twomass_sixx2_xsc TWOMASS J confusion flag for 7 arcsec circular ap. mag smallint 2

j_flg_7 twomass_xsc TWOMASS J confusion flag for 7 arcsec circular ap. mag. smallint 2 meta.code

j_flg_70 twomass_xsc TWOMASS J confusion flag for 70 arcsec circular ap. mag. smallint 2 meta.code

j_flg_c twomass_xsc TWOMASS J confusion flag for Kron circular mag. smallint 2 meta.code

j_flg_e twomass_xsc TWOMASS J confusion flag for Kron elliptical mag. smallint 2 meta.code

j_flg_fc twomass_xsc TWOMASS J confusion flag for fiducial Kron circ. mag. smallint 2 meta.code

j_flg_fe twomass_xsc TWOMASS J confusion flag for fiducial Kron ell. mag. smallint 2 meta.code

j_flg_i20c twomass_xsc TWOMASS J confusion flag for 20mag/sq." iso. circ. mag. smallint 2 meta.code

j_flg_i20e twomass_xsc TWOMASS J confusion flag for 20mag/sq." iso. ell. mag. smallint 2 meta.code

j_flg_i21c twomass_xsc TWOMASS J confusion flag for 21mag/sq." iso. circ. mag. smallint 2 meta.code

j_flg_i21e twomass_xsc TWOMASS J confusion flag for 21mag/sq." iso. ell. mag. smallint 2 meta.code

j_flg_j21fc twomass_xsc TWOMASS J confusion flag for 21mag/sq." iso. fid. circ. mag. smallint 2 meta.code

j_flg_j21fe twomass_xsc TWOMASS J confusion flag for 21mag/sq." iso. fid. ell. mag. smallint 2 meta.code

j_flg_k20fc twomass_xsc TWOMASS J confusion flag for 20mag/sq." iso. fid. circ. mag. smallint 2 meta.code

j_flg_k20fe twomass_sixx2_xsc TWOMASS J confusion flag for 20mag/sq.″ iso. fid. ell. mag smallint 2

j_flg_k20fe twomass_xsc TWOMASS J confusion flag for 20mag/sq." iso. fid. ell. mag. smallint 2 meta.code

j_h twomass_sixx2_psc TWOMASS The J-H color, computed from the J-band and H-band magnitudes (j_m and h_m, respectively) of the source. In cases where the first or second 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

j_k twomass_sixx2_psc TWOMASS The J-Ks color, computed from the J-band and Ks-band magnitudes (j_m and k_m, respectively) of the source. In cases where the first 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

j_m twomass_psc TWOMASS Default J-band magnitude real 4 mag phot.flux

j_m twomass_sixx2_psc TWOMASS J selected "default" magnitude real 4 mag

j_m_10 twomass_xsc TWOMASS J 10 arcsec radius circular aperture magnitude. real 4 mag phot.flux

j_m_15 twomass_xsc TWOMASS J 15 arcsec radius circular aperture magnitude. real 4 mag phot.flux

j_m_20 twomass_xsc TWOMASS J 20 arcsec radius circular aperture magnitude. real 4 mag phot.flux

j_m_25 twomass_xsc TWOMASS J 25 arcsec radius circular aperture magnitude. real 4 mag phot.flux

j_m_2mass allwise_sc WISE 2MASS J-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 J-band magnitude entry is "null". float 8 mag

j_m_2mass wise_allskysc WISE 2MASS J-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 J-band magnitude entry is default. real 4 mag -0.9999995e9

j_m_2mass wise_prelimsc WISE 2MASS J-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 J-band magnitude entry is default real 4 mag -0.9999995e9

j_m_30 twomass_xsc TWOMASS J 30 arcsec radius circular aperture magnitude. real 4 mag phot.flux

j_m_40 twomass_xsc TWOMASS J 40 arcsec radius circular aperture magnitude. real 4 mag phot.flux

j_m_5 twomass_xsc TWOMASS J 5 arcsec radius circular aperture magnitude. real 4 mag phot.flux

j_m_50 twomass_xsc TWOMASS J 50 arcsec radius circular aperture magnitude. real 4 mag phot.flux

j_m_60 twomass_xsc TWOMASS J 60 arcsec radius circular aperture magnitude. real 4 mag phot.flux

j_m_7 twomass_sixx2_xsc TWOMASS J 7 arcsec radius circular aperture magnitude real 4 mag

j_m_7 twomass_xsc TWOMASS J 7 arcsec radius circular aperture magnitude. real 4 mag phot.flux

j_m_70 twomass_xsc TWOMASS J 70 arcsec radius circular aperture magnitude. real 4 mag phot.flux

j_m_c twomass_xsc TWOMASS J Kron circular aperture magnitude. real 4 mag phot.flux

j_m_e twomass_xsc TWOMASS J Kron elliptical aperture magnitude. real 4 mag phot.flux

j_m_ext twomass_sixx2_xsc TWOMASS J mag from fit extrapolation real 4 mag

j_m_ext twomass_xsc TWOMASS J mag from fit extrapolation. real 4 mag phot.flux

j_m_fc twomass_xsc TWOMASS J fiducial Kron circular magnitude. real 4 mag phot.flux

j_m_fe twomass_xsc TWOMASS J fiducial Kron ell. mag aperture magnitude. real 4 mag phot.flux

j_m_i20c twomass_xsc TWOMASS J 20mag/sq." isophotal circular ap. magnitude. real 4 mag phot.flux

j_m_i20e twomass_xsc TWOMASS J 20mag/sq." isophotal elliptical ap. magnitude. real 4 mag phot.flux

j_m_i21c twomass_xsc TWOMASS J 21mag/sq." isophotal circular ap. magnitude. real 4 mag phot.flux

j_m_i21e twomass_xsc TWOMASS J 21mag/sq." isophotal elliptical ap. magnitude. real 4 mag phot.flux

j_m_j21fc twomass_xsc TWOMASS J 21mag/sq." isophotal fiducial circ. ap. mag. real 4 mag phot.flux

j_m_j21fe twomass_xsc TWOMASS J 21mag/sq." isophotal fiducial ell. ap. magnitude. real 4 mag phot.flux

j_m_k20fc twomass_xsc TWOMASS J 20mag/sq." isophotal fiducial circ. ap. mag. real 4 mag phot.flux

J_M_K20FE twomass SIXDF J 20mag/sq." isophotal fiducial ell. ap. magnitude real 4 mag

j_m_k20fe twomass_sixx2_xsc TWOMASS J 20mag/sq.″ isophotal fiducial ell. ap. magnitude real 4 mag

j_m_k20fe twomass_xsc TWOMASS J 20mag/sq." isophotal fiducial ell. ap. magnitude. real 4 mag phot.flux

j_m_stdap twomass_psc TWOMASS J-band "standard" aperture magnitude. real 4 mag phot.flux

j_m_sys twomass_xsc TWOMASS J system photometry magnitude. real 4 mag phot.flux

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

j_msig twomass_sixx2_psc TWOMASS J "default" mag uncertainty real 4 mag

j_msig_10 twomass_xsc TWOMASS J 1-sigma uncertainty in 10 arcsec circular ap. mag. real 4 mag stat.error

j_msig_15 twomass_xsc TWOMASS J 1-sigma uncertainty in 15 arcsec circular ap. mag. real 4 mag stat.error

j_msig_20 twomass_xsc TWOMASS J 1-sigma uncertainty in 20 arcsec circular ap. mag. real 4 mag stat.error

j_msig_25 twomass_xsc TWOMASS J 1-sigma uncertainty in 25 arcsec circular ap. mag. real 4 mag stat.error

j_msig_2mass allwise_sc WISE 2MASS J-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 J-band uncertainty entry is "null". float 8 mag

j_msig_2mass wise_allskysc WISE 2MASS J-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 J-band uncertainty entry is default. real 4 mag -0.9999995e9

j_msig_2mass wise_prelimsc WISE 2MASS J-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 J-band uncertainty entry is default real 4 mag -0.9999995e9

j_msig_30 twomass_xsc TWOMASS J 1-sigma uncertainty in 30 arcsec circular ap. mag. real 4 mag stat.error

j_msig_40 twomass_xsc TWOMASS J 1-sigma uncertainty in 40 arcsec circular ap. mag. real 4 mag stat.error

j_msig_5 twomass_xsc TWOMASS J 1-sigma uncertainty in 5 arcsec circular ap. mag. real 4 mag stat.error

j_msig_50 twomass_xsc TWOMASS J 1-sigma uncertainty in 50 arcsec circular ap. mag. real 4 mag stat.error

j_msig_60 twomass_xsc TWOMASS J 1-sigma uncertainty in 60 arcsec circular ap. mag. real 4 mag stat.error

j_msig_7 twomass_sixx2_xsc TWOMASS J 1-sigma uncertainty in 7 arcsec circular ap. mag real 4 mag

j_msig_7 twomass_xsc TWOMASS J 1-sigma uncertainty in 7 arcsec circular ap. mag. real 4 mag stat.error

j_msig_70 twomass_xsc TWOMASS J 1-sigma uncertainty in 70 arcsec circular ap. mag. real 4 mag stat.error

j_msig_c twomass_xsc TWOMASS J 1-sigma uncertainty in Kron circular mag. real 4 mag stat.error

j_msig_e twomass_xsc TWOMASS J 1-sigma uncertainty in Kron elliptical mag. real 4 mag stat.error

j_msig_ext twomass_sixx2_xsc TWOMASS J 1-sigma uncertainty in mag from fit extrapolation real 4 mag

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

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

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

j_msig_i20c twomass_xsc TWOMASS J 1-sigma uncertainty in 20mag/sq." iso. circ. mag. real 4 mag stat.error

j_msig_i20e twomass_xsc TWOMASS J 1-sigma uncertainty in 20mag/sq." iso. ell. mag. real 4 mag stat.error

j_msig_i21c twomass_xsc TWOMASS J 1-sigma uncertainty in 21mag/sq." iso. circ. mag. real 4 mag stat.error

j_msig_i21e twomass_xsc TWOMASS J 1-sigma uncertainty in 21mag/sq." iso. ell. mag. real 4 mag stat.error

j_msig_j21fc twomass_xsc TWOMASS J 1-sigma uncertainty in 21mag/sq." iso.fid.circ.mag. real 4 mag stat.error

j_msig_j21fe twomass_xsc TWOMASS J 1-sigma uncertainty in 21mag/sq." iso.fid.ell.mag. real 4 mag stat.error

j_msig_k20fc twomass_xsc TWOMASS J 1-sigma uncertainty in 20mag/sq." iso.fid.circ. mag. real 4 mag stat.error

j_msig_k20fe twomass_xsc TWOMASS J 1-sigma uncertainty in 20mag/sq." iso.fid.ell.mag. real 4 mag stat.error

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

j_msig_sys twomass_xsc TWOMASS J 1-sigma uncertainty in system photometry mag. real 4 mag stat.error

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

j_msigcom twomass_sixx2_psc TWOMASS combined (total) J band photometric uncertainty real 4 mag

j_msnr10 twomass_scn TWOMASS The estimated J-band magnitude at which SNR=10 is achieved for this scan. real 4 mag phot.flux

j_msnr10 twomass_sixx2_scn TWOMASS J mag at which SNR=10 is achieved, from j_psp and j_zp_ap real 4 mag

j_n_snr10 twomass_scn TWOMASS Number of point sources at J-band with SNR>10 (instrumental mag <=15.8) int 4 meta.number

j_n_snr10 twomass_sixx2_scn TWOMASS number of J point sources with SNR>10 (instrumental m<=15.8) int 4

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

j_peak twomass_xsc TWOMASS J peak pixel brightness. real 4 mag phot.mag.sb

j_perc_darea twomass_xsc TWOMASS J 5-sigma to 3-sigma percent area change. smallint 2 FIT_PARAM

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

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

j_psp twomass_scn TWOMASS J-band photometric sensitivity paramater (PSP). real 4 instr.sensitivity

j_psp twomass_sixx2_scn TWOMASS J photometric sensitivity param: j_shape_avg*(j_fbg_avg^.29) real 4

j_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 J-band photometric errors and is expressed in units of mJy. real 4 instr.det.noise

j_pts_noise twomass_sixx2_scn TWOMASS log10 of J band modal point src noise estimate real 4 logmJy

j_r_c twomass_xsc TWOMASS J Kron circular aperture radius. real 4 arcsec phys.angSize;src

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

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

j_r_i20c twomass_xsc TWOMASS J 20mag/sq." isophotal circular aperture radius. real 4 arcsec phys.angSize;src

j_r_i20e twomass_xsc TWOMASS J 20mag/sq." isophotal elliptical ap. semi-major axis. real 4 arcsec phys.angSize;src

j_r_i21c twomass_xsc TWOMASS J 21mag/sq." isophotal circular aperture radius. real 4 arcsec phys.angSize;src

j_r_i21e twomass_xsc TWOMASS J 21mag/sq." isophotal elliptical ap. semi-major axis. real 4 arcsec phys.angSize;src

j_resid_ann twomass_xsc TWOMASS J residual annulus background median. real 4 DN meta.code

j_sc_1mm twomass_xsc TWOMASS J 1st moment (score) (LCSB: super blk 2,4,8 SNR). real 4 meta.code

j_sc_2mm twomass_xsc TWOMASS J 2nd moment (score) (LCSB: SNRMAX - super SNR max). real 4 meta.code

j_sc_msh twomass_xsc TWOMASS J median shape score. real 4 meta.code

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

j_sc_r1 twomass_xsc TWOMASS J r1 (score). real 4 meta.code

j_sc_r23 twomass_xsc TWOMASS J r23 (score) (LCSB: TSNR - integrated SNR for r=15). real 4 meta.code

j_sc_sh twomass_xsc TWOMASS J shape (score). real 4 meta.code

j_sc_vint twomass_xsc TWOMASS J vint (score). real 4 meta.code

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

j_seetrack twomass_xsc TWOMASS J band seetracking score. real 4 meta.code

j_sh0 twomass_xsc TWOMASS J ridge shape (LCSB: BSNR limit). real 4 FIT_PARAM

j_shape_avg twomass_scn TWOMASS J-band average seeing shape for scan. real 4 instr.obsty.seeing

j_shape_avg twomass_sixx2_scn TWOMASS J band average seeing shape for scan real 4

j_shape_rms twomass_scn TWOMASS RMS-error of J-band average seeing shape. real 4 instr.obsty.seeing

j_shape_rms twomass_sixx2_scn TWOMASS rms of J band avg seeing shape for scan real 4

j_sig_sh0 twomass_xsc TWOMASS J ridge shape sigma (LCSB: B2SNR limit). real 4 FIT_PARAM

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

j_snr twomass_sixx2_psc TWOMASS J band "scan" signal-to-noise ratio real 4

j_subst2 twomass_xsc TWOMASS J residual background #2 (score). real 4 meta.code

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

j_zp_ap twomass_sixx2_scn TWOMASS J band ap. calibration photometric zero-point for scan real 4 mag

jAmpl vmcCepheidVariables VMCDR4 Peak-to-Peak amplitude in J band {catalogue TType keyword: A(J)} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.J

jAmpl vmcCepheidVariables VMCv20160311 Peak-to-Peak amplitude in J band {catalogue TType keyword: A(J)} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.J

jAmpl vmcCepheidVariables VMCv20160822 Peak-to-Peak amplitude in J band {catalogue TType keyword: A(J)} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.J

jAmpl vmcCepheidVariables VMCv20170109 Peak-to-Peak amplitude in J band {catalogue TType keyword: A(J)} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.J

jAmpl vmcCepheidVariables VMCv20170411 Peak-to-Peak amplitude in J band {catalogue TType keyword: A(J)} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.J

jAmpl vmcCepheidVariables VMCv20171101 Peak-to-Peak amplitude in J band {catalogue TType keyword: A(J)} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.J

jAmpl vmcCepheidVariables VMCv20180702 Peak-to-Peak amplitude in J band {catalogue TType keyword: A(J)} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.J

jAmpl vmcCepheidVariables VMCv20181120 Peak-to-Peak amplitude in J band {catalogue TType keyword: A(J)} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.J

jAmpl vmcCepheidVariables VMCv20191212 Peak-to-Peak amplitude in J band {catalogue TType keyword: A(J)} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.J

jAmpl vmcCepheidVariables VMCv20210708 Peak-to-Peak amplitude in J band {catalogue TType keyword: A(J)} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.J

jAmpl vmcCepheidVariables VMCv20230816 Peak-to-Peak amplitude in J band {catalogue TType keyword: A(J)} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.J

jAmpl vmcCepheidVariables VMCv20240226 Peak-to-Peak amplitude in J band {catalogue TType keyword: A(J)} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.J

jAmplErr vmcCepheidVariables VMCDR4 Error in Peak-to-Peak amplitude in J band {catalogue TType keyword: e_A(J)} real 4 mag -0.9999995e9 stat.error;src.var.amplitude;em.IR.J

jAmplErr vmcCepheidVariables VMCv20160311 Error in Peak-to-Peak amplitude in J band {catalogue TType keyword: e_A(J)} real 4 mag -0.9999995e9 stat.error;src.var.amplitude;em.IR.J

jAmplErr vmcCepheidVariables VMCv20160822 Error in Peak-to-Peak amplitude in J band {catalogue TType keyword: e_A(J)} real 4 mag -0.9999995e9 stat.error;src.var.amplitude;em.IR.J

jAmplErr vmcCepheidVariables VMCv20170109 Error in Peak-to-Peak amplitude in J band {catalogue TType keyword: e_A(J)} real 4 mag -0.9999995e9 stat.error;src.var.amplitude;em.IR.J

jAmplErr vmcCepheidVariables VMCv20170411 Error in Peak-to-Peak amplitude in J band {catalogue TType keyword: e_A(J)} real 4 mag -0.9999995e9 stat.error;src.var.amplitude;em.IR.J

jAmplErr vmcCepheidVariables VMCv20171101 Error in Peak-to-Peak amplitude in J band {catalogue TType keyword: e_A(J)} real 4 mag -0.9999995e9 stat.error;src.var.amplitude;em.IR.J

jAmplErr vmcCepheidVariables VMCv20180702 Error in Peak-to-Peak amplitude in J band {catalogue TType keyword: e_A(J)} real 4 mag -0.9999995e9 stat.error;src.var.amplitude;em.IR.J

jAmplErr vmcCepheidVariables VMCv20181120 Error in Peak-to-Peak amplitude in J band {catalogue TType keyword: e_A(J)} real 4 mag -0.9999995e9 stat.error;src.var.amplitude;em.IR.J

jAmplErr vmcCepheidVariables VMCv20191212 Error in Peak-to-Peak amplitude in J band {catalogue TType keyword: e_A(J)} real 4 mag -0.9999995e9 stat.error;src.var.amplitude;em.IR.J

jAmplErr vmcCepheidVariables VMCv20210708 Error in Peak-to-Peak amplitude in J band {catalogue TType keyword: e_A(J)} real 4 mag -0.9999995e9 stat.error;src.var.amplitude;em.IR.J

jAmplErr vmcCepheidVariables VMCv20230816 Error in Peak-to-Peak amplitude in J band {catalogue TType keyword: e_A(J)} real 4 mag -0.9999995e9 stat.error;src.var.amplitude;em.IR.J

jAmplErr vmcCepheidVariables VMCv20240226 Error in Peak-to-Peak amplitude in J band {catalogue TType keyword: e_A(J)} real 4 mag -0.9999995e9 stat.error;src.var.amplitude;em.IR.J

jAperJky3 ultravistaSourceRemeasurement ULTRAVISTADR4 Default point source J aperture corrected (2.0 arcsec aperture diameter) calibrated flux
If in doubt use this flux estimator real 4 jansky -0.9999995e9 phot.flux

jAperJky3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Default point source J aperture corrected (2.0 arcsec aperture diameter) calibrated flux
If in doubt use this flux estimator real 4 jansky -0.9999995e9 phot.flux

jAperJky3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Default point source J aperture corrected (2.0 arcsec aperture diameter) calibrated flux
If in doubt use this flux estimator real 4 jansky -0.9999995e9 phot.flux

jAperJky3Err ultravistaSourceRemeasurement ULTRAVISTADR4 Error in default point/extended source J (2.0 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error

jAperJky3Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in default point/extended source J (2.0 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error

jAperJky3Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in default point/extended source J (2.0 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error

jAperJky4 ultravistaSourceRemeasurement ULTRAVISTADR4 Point source J aperture corrected (2.8 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 phot.flux

jAperJky4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Point source J aperture corrected (2.8 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 phot.flux

jAperJky4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Point source J aperture corrected (2.8 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 phot.flux

jAperJky4Err ultravistaSourceRemeasurement ULTRAVISTADR4 Error in point/extended source J (2.8 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error

jAperJky4Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in point/extended source J (2.8 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error

jAperJky4Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in point/extended source J (2.8 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error

jAperJky6 ultravistaSourceRemeasurement ULTRAVISTADR4 Point source J aperture corrected (5.7 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 phot.flux

jAperJky6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Point source J aperture corrected (5.7 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 phot.flux

jAperJky6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Point source J aperture corrected (5.7 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 phot.flux

jAperJky6Err ultravistaSourceRemeasurement ULTRAVISTADR4 Error in point/extended source J (5.7 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error

jAperJky6Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in point/extended source J (5.7 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error

jAperJky6Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in point/extended source J (5.7 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error

jAperJkyNoAperCorr3 ultravistaSourceRemeasurement ULTRAVISTADR4 Default extended source J (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

jAperJkyNoAperCorr3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Default extended source J (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

jAperJkyNoAperCorr3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Default extended source J (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

jAperJkyNoAperCorr4 ultravistaSourceRemeasurement ULTRAVISTADR4 Extended source J (2.8 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux real 4 jansky -0.9999995e9 phot.flux

jAperJkyNoAperCorr4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Extended source J (2.8 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux real 4 jansky -0.9999995e9 phot.flux

jAperJkyNoAperCorr4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Extended source J (2.8 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux real 4 jansky -0.9999995e9 phot.flux

jAperJkyNoAperCorr6 ultravistaSourceRemeasurement ULTRAVISTADR4 Extended source J (5.7 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux real 4 jansky -0.9999995e9 phot.flux

jAperJkyNoAperCorr6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Extended source J (5.7 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux real 4 jansky -0.9999995e9 phot.flux

jAperJkyNoAperCorr6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Extended source J (5.7 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux real 4 jansky -0.9999995e9 phot.flux

jAperLup3 ultravistaSourceRemeasurement ULTRAVISTADR4 Default point source J aperture corrected (2.0 arcsec aperture diameter) luptitude
If in doubt use this flux estimator real 4 lup -0.9999995e9 phot.lup

jAperLup3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Default point source J aperture corrected (2.0 arcsec aperture diameter) luptitude
If in doubt use this flux estimator real 4 lup -0.9999995e9 phot.lup

jAperLup3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Default point source J aperture corrected (2.0 arcsec aperture diameter) luptitude
If in doubt use this flux estimator real 4 lup -0.9999995e9 phot.lup

jAperLup3Err ultravistaSourceRemeasurement ULTRAVISTADR4 Error in default point/extended source J (2.0 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error

jAperLup3Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in default point/extended source J (2.0 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error

jAperLup3Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in default point/extended source J (2.0 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error

jAperLup4 ultravistaSourceRemeasurement ULTRAVISTADR4 Point source J aperture corrected (2.8 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 phot.lup

jAperLup4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Point source J aperture corrected (2.8 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 phot.lup

jAperLup4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Point source J aperture corrected (2.8 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 phot.lup

jAperLup4Err ultravistaSourceRemeasurement ULTRAVISTADR4 Error in point/extended source J (2.8 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error

jAperLup4Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in point/extended source J (2.8 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error

jAperLup4Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in point/extended source J (2.8 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error

jAperLup6 ultravistaSourceRemeasurement ULTRAVISTADR4 Point source J aperture corrected (5.7 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 phot.lup

jAperLup6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Point source J aperture corrected (5.7 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 phot.lup

jAperLup6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Point source J aperture corrected (5.7 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 phot.lup

jAperLup6Err ultravistaSourceRemeasurement ULTRAVISTADR4 Error in point/extended source J (5.7 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error

jAperLup6Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in point/extended source J (5.7 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error

jAperLup6Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in point/extended source J (5.7 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error

jAperLupNoAperCorr3 ultravistaSourceRemeasurement ULTRAVISTADR4 Default extended source J (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

jAperLupNoAperCorr3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Default extended source J (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

jAperLupNoAperCorr3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Default extended source J (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

jAperLupNoAperCorr4 ultravistaSourceRemeasurement ULTRAVISTADR4 Extended source J (2.8 arcsec aperture diameter, but no aperture correction applied) aperture luptitude real 4 lup -0.9999995e9 phot.lup

jAperLupNoAperCorr4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Extended source J (2.8 arcsec aperture diameter, but no aperture correction applied) aperture luptitude real 4 lup -0.9999995e9 phot.lup

jAperLupNoAperCorr4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Extended source J (2.8 arcsec aperture diameter, but no aperture correction applied) aperture luptitude real 4 lup -0.9999995e9 phot.lup

jAperLupNoAperCorr6 ultravistaSourceRemeasurement ULTRAVISTADR4 Extended source J (5.7 arcsec aperture diameter, but no aperture correction applied) aperture luptitude real 4 lup -0.9999995e9 phot.lup

jAperLupNoAperCorr6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Extended source J (5.7 arcsec aperture diameter, but no aperture correction applied) aperture luptitude real 4 lup -0.9999995e9 phot.lup

jAperLupNoAperCorr6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Extended source J (5.7 arcsec aperture diameter, but no aperture correction applied) aperture luptitude real 4 lup -0.9999995e9 phot.lup

jAperMag1 vmcSynopticSource VMCDR1 Extended source J aperture corrected mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag1 vmcSynopticSource VMCDR2 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag1 vmcSynopticSource VMCDR3 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag1 vmcSynopticSource VMCDR4 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag1 vmcSynopticSource VMCDR5 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag1 vmcSynopticSource VMCv20110816 Extended source J aperture corrected mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag1 vmcSynopticSource VMCv20110909 Extended source J aperture corrected mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag1 vmcSynopticSource VMCv20120126 Extended source J aperture corrected mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag1 vmcSynopticSource VMCv20121128 Extended source J aperture corrected mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag1 vmcSynopticSource VMCv20130304 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag1 vmcSynopticSource VMCv20130805 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag1 vmcSynopticSource VMCv20140428 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag1 vmcSynopticSource VMCv20140903 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag1 vmcSynopticSource VMCv20150309 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag1 vmcSynopticSource VMCv20151218 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag1 vmcSynopticSource VMCv20160311 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag1 vmcSynopticSource VMCv20160822 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag1 vmcSynopticSource VMCv20170109 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag1 vmcSynopticSource VMCv20170411 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag1 vmcSynopticSource VMCv20171101 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag1 vmcSynopticSource VMCv20180702 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag1 vmcSynopticSource VMCv20181120 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag1 vmcSynopticSource VMCv20191212 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag1 vmcSynopticSource VMCv20210708 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag1 vmcSynopticSource VMCv20230816 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag1 vmcSynopticSource VMCv20240226 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag1 vmcdeepSynopticSource VMCDEEPv20230713 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag1 vmcdeepSynopticSource VMCDEEPv20240506 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag1 vvvSource VVVDR1 Extended source J aperture corrected mag (0.7 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMag1 vvvSource VVVDR5 Point source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag1 vvvSource VVVv20100531 Extended source J aperture corrected mag (0.7 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMag1 vvvSource VVVv20110718 Extended source J aperture corrected mag (0.7 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMag1 vvvSource, vvvSynopticSource VVVDR2 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag1Err vmcSynopticSource VMCDR1 Error in extended source J mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag1Err vmcSynopticSource VMCDR2 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag1Err vmcSynopticSource VMCDR3 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag1Err vmcSynopticSource VMCDR4 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag1Err vmcSynopticSource VMCDR5 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag1Err vmcSynopticSource VMCv20110816 Error in extended source J mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag1Err vmcSynopticSource VMCv20110909 Error in extended source J mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag1Err vmcSynopticSource VMCv20120126 Error in extended source J mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag1Err vmcSynopticSource VMCv20121128 Error in extended source J mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag1Err vmcSynopticSource VMCv20130304 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag1Err vmcSynopticSource VMCv20130805 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag1Err vmcSynopticSource VMCv20140428 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J

jAperMag1Err vmcSynopticSource VMCv20140903 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag1Err vmcSynopticSource VMCv20150309 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag1Err vmcSynopticSource VMCv20151218 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag1Err vmcSynopticSource VMCv20160311 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag1Err vmcSynopticSource VMCv20160822 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag1Err vmcSynopticSource VMCv20170109 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag1Err vmcSynopticSource VMCv20170411 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag1Err vmcSynopticSource VMCv20171101 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag1Err vmcSynopticSource VMCv20180702 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag1Err vmcSynopticSource VMCv20181120 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag1Err vmcSynopticSource VMCv20191212 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag1Err vmcSynopticSource VMCv20210708 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag1Err vmcSynopticSource VMCv20230816 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag1Err vmcSynopticSource VMCv20240226 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag1Err vmcdeepSynopticSource VMCDEEPv20230713 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag1Err vmcdeepSynopticSource VMCDEEPv20240506 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag1Err vvvSource VVVDR1 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag1Err vvvSource VVVDR5 Error in point source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag1Err vvvSource VVVv20100531 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag1Err vvvSource VVVv20110718 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag1Err vvvSource, vvvSynopticSource VVVDR2 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag2 vmcSynopticSource VMCDR1 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag2 vmcSynopticSource VMCDR2 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag2 vmcSynopticSource VMCDR3 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag2 vmcSynopticSource VMCDR4 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag2 vmcSynopticSource VMCDR5 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag2 vmcSynopticSource VMCv20110816 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag2 vmcSynopticSource VMCv20110909 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag2 vmcSynopticSource VMCv20120126 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag2 vmcSynopticSource VMCv20121128 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag2 vmcSynopticSource VMCv20130304 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag2 vmcSynopticSource VMCv20130805 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag2 vmcSynopticSource VMCv20140428 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag2 vmcSynopticSource VMCv20140903 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag2 vmcSynopticSource VMCv20150309 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag2 vmcSynopticSource VMCv20151218 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag2 vmcSynopticSource VMCv20160311 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag2 vmcSynopticSource VMCv20160822 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag2 vmcSynopticSource VMCv20170109 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag2 vmcSynopticSource VMCv20170411 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag2 vmcSynopticSource VMCv20171101 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag2 vmcSynopticSource VMCv20180702 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag2 vmcSynopticSource VMCv20181120 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag2 vmcSynopticSource VMCv20191212 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag2 vmcSynopticSource VMCv20210708 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag2 vmcSynopticSource VMCv20230816 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag2 vmcSynopticSource VMCv20240226 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag2 vmcdeepSynopticSource VMCDEEPv20230713 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag2 vmcdeepSynopticSource VMCDEEPv20240506 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag2 vvvSynopticSource VVVDR1 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag2 vvvSynopticSource VVVDR2 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag2Err vmcSynopticSource VMCDR1 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag2Err vmcSynopticSource VMCDR2 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag2Err vmcSynopticSource VMCDR3 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag2Err vmcSynopticSource VMCDR4 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag2Err vmcSynopticSource VMCDR5 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag2Err vmcSynopticSource VMCv20110816 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag2Err vmcSynopticSource VMCv20110909 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag2Err vmcSynopticSource VMCv20120126 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag2Err vmcSynopticSource VMCv20121128 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag2Err vmcSynopticSource VMCv20130304 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag2Err vmcSynopticSource VMCv20130805 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag2Err vmcSynopticSource VMCv20140428 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J

jAperMag2Err vmcSynopticSource VMCv20140903 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag2Err vmcSynopticSource VMCv20150309 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag2Err vmcSynopticSource VMCv20151218 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag2Err vmcSynopticSource VMCv20160311 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag2Err vmcSynopticSource VMCv20160822 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag2Err vmcSynopticSource VMCv20170109 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag2Err vmcSynopticSource VMCv20170411 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag2Err vmcSynopticSource VMCv20171101 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag2Err vmcSynopticSource VMCv20180702 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag2Err vmcSynopticSource VMCv20181120 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag2Err vmcSynopticSource VMCv20191212 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag2Err vmcSynopticSource VMCv20210708 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag2Err vmcSynopticSource VMCv20230816 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag2Err vmcSynopticSource VMCv20240226 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag2Err vmcdeepSynopticSource VMCDEEPv20230713 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag2Err vmcdeepSynopticSource VMCDEEPv20240506 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag2Err vvvSynopticSource VVVDR1 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag2Err vvvSynopticSource VVVDR2 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag3 ultravistaSource ULTRAVISTADR4 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 ultravistaSourceRemeasurement ULTRAVISTADR4 Default point source J aperture corrected (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMag3 vhsSource VHSDR1 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMag3 vhsSource VHSDR2 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMag3 vhsSource VHSDR3 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vhsSource VHSDR4 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vhsSource VHSDR5 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vhsSource VHSDR6 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vhsSource VHSv20120926 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMag3 vhsSource VHSv20130417 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMag3 vhsSource VHSv20140409 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vhsSource VHSv20150108 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vhsSource VHSv20160114 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vhsSource VHSv20160507 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vhsSource VHSv20170630 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vhsSource VHSv20180419 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vhsSource VHSv20201209 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vhsSource VHSv20231101 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vhsSource VHSv20240731 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 videoSource VIDEODR2 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMag3 videoSource VIDEODR3 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMag3 videoSource VIDEODR4 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 videoSource VIDEODR5 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 videoSource VIDEOv20100513 Default point/extended source J mag, no aperture correction applied
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMag3 videoSource VIDEOv20111208 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMag3 vikingSource VIKINGDR2 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMag3 vikingSource VIKINGDR3 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMag3 vikingSource VIKINGDR4 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vikingSource VIKINGv20110714 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMag3 vikingSource VIKINGv20111019 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMag3 vikingSource VIKINGv20130417 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMag3 vikingSource VIKINGv20140402 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vikingSource VIKINGv20150421 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vikingSource VIKINGv20151230 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vikingSource VIKINGv20160406 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vikingSource VIKINGv20161202 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vikingSource VIKINGv20170715 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Default point source J aperture corrected (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMag3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Default point source J aperture corrected (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMag3 vmcSource VMCDR1 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMag3 vmcSource VMCDR2 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSource VMCDR3 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSource VMCDR4 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSource VMCDR5 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSource VMCv20110816 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMag3 vmcSource VMCv20110909 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMag3 vmcSource VMCv20120126 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMag3 vmcSource VMCv20121128 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMag3 vmcSource VMCv20130304 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMag3 vmcSource VMCv20130805 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSource VMCv20140428 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSource VMCv20140903 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSource VMCv20150309 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSource VMCv20151218 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSource VMCv20160311 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSource VMCv20160822 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSource VMCv20170109 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSource VMCv20170411 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSource VMCv20171101 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSource VMCv20180702 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSource VMCv20181120 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSource VMCv20191212 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSource VMCv20210708 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSource VMCv20230816 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSource VMCv20240226 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSynopticSource VMCDR1 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag3 vmcSynopticSource VMCDR2 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSynopticSource VMCDR3 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSynopticSource VMCDR4 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSynopticSource VMCDR5 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSynopticSource VMCv20110816 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag3 vmcSynopticSource VMCv20110909 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag3 vmcSynopticSource VMCv20120126 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag3 vmcSynopticSource VMCv20121128 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag3 vmcSynopticSource VMCv20130304 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag3 vmcSynopticSource VMCv20130805 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSynopticSource VMCv20140428 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSynopticSource VMCv20140903 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSynopticSource VMCv20150309 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSynopticSource VMCv20151218 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSynopticSource VMCv20160311 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSynopticSource VMCv20160822 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSynopticSource VMCv20170109 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSynopticSource VMCv20170411 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSynopticSource VMCv20171101 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSynopticSource VMCv20180702 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSynopticSource VMCv20181120 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSynopticSource VMCv20191212 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSynopticSource VMCv20210708 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSynopticSource VMCv20230816 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcSynopticSource VMCv20240226 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcdeepSource VMCDEEPv20230713 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcdeepSource VMCDEEPv20240506 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcdeepSynopticSource VMCDEEPv20230713 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vmcdeepSynopticSource VMCDEEPv20240506 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vvvSource VVVDR1 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMag3 vvvSource VVVDR2 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vvvSource VVVDR5 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vvvSource VVVv20100531 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMag3 vvvSource VVVv20110718 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMag3 vvvSynopticSource VVVDR1 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag3 vvvSynopticSource VVVDR2 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag3 vvvVivaCatalogue VVVDR5 J magnitude using aperture corrected mag (2.0 arcsec aperture diameter, from VVVDR4 1st epoch JHKs contemporaneous OB) {catalogue TType keyword: jAperMag3} real 4 mag -9.999995e8

jAperMag3Err ultravistaSource ULTRAVISTADR4 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag3Err ultravistaSourceRemeasurement ULTRAVISTADR4 Error in default point/extended source J (2.0 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error

jAperMag3Err vhsSource VHSDR1 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag3Err vhsSource VHSDR2 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag3Err vhsSource VHSDR3 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J

jAperMag3Err vhsSource VHSDR4 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag3Err vhsSource VHSDR5 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag3Err vhsSource VHSDR6 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag3Err vhsSource VHSv20120926 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag3Err vhsSource VHSv20130417 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag3Err vhsSource VHSv20140409 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J

jAperMag3Err vhsSource VHSv20150108 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag3Err vhsSource VHSv20160114 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag3Err vhsSource VHSv20160507 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag3Err vhsSource VHSv20170630 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag3Err vhsSource VHSv20180419 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag3Err vhsSource VHSv20201209 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag3Err vhsSource VHSv20231101 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag3Err vhsSource VHSv20240731 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag3Err videoSource VIDEODR2 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag3Err videoSource VIDEODR3 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag3Err videoSource VIDEODR4 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag3Err videoSource VIDEODR5 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag3Err videoSource VIDEOv20100513 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag3Err videoSource VIDEOv20111208 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag3Err vikingSource VIKINGDR2 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag3Err vikingSource VIKINGDR3 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag3Err vikingSource VIKINGDR4 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J

jAperMag3Err vikingSource VIKINGv20110714 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag3Err vikingSource VIKINGv20111019 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag3Err vikingSource VIKINGv20130417 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag3Err vikingSource VIKINGv20140402 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag3Err vikingSource VIKINGv20150421 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag3Err vikingSource VIKINGv20151230 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag3Err vikingSource VIKINGv20160406 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag3Err vikingSource VIKINGv20161202 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag3Err vikingSource VIKINGv20170715 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag3Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in default point/extended source J (2.0 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error

jAperMag3Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in default point/extended source J (2.0 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error

jAperMag3Err vmcSource VMCDR2 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag3Err vmcSource VMCDR3 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag3Err vmcSource VMCDR4 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag3Err vmcSource VMCDR5 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag3Err vmcSource VMCv20110816 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag3Err vmcSource VMCv20110909 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag3Err vmcSource VMCv20120126 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag3Err vmcSource VMCv20121128 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag3Err vmcSource VMCv20130304 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag3Err vmcSource VMCv20130805 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag3Err vmcSource VMCv20140428 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J

jAperMag3Err vmcSource VMCv20140903 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag3Err vmcSource VMCv20150309 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag3Err vmcSource VMCv20151218 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag3Err vmcSource VMCv20160311 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag3Err vmcSource VMCv20160822 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag3Err vmcSource VMCv20170109 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag3Err vmcSource VMCv20170411 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag3Err vmcSource VMCv20171101 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag3Err vmcSource VMCv20180702 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag3Err vmcSource VMCv20181120 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag3Err vmcSource VMCv20191212 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag3Err vmcSource VMCv20210708 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag3Err vmcSource VMCv20230816 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag3Err vmcSource VMCv20240226 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag3Err vmcSource, vmcSynopticSource VMCDR1 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag3Err vmcdeepSource VMCDEEPv20240506 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag3Err vmcdeepSource, vmcdeepSynopticSource VMCDEEPv20230713 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag3Err vvvSource VVVDR2 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag3Err vvvSource VVVDR5 Error in default point source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag3Err vvvSource VVVv20100531 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag3Err vvvSource VVVv20110718 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag3Err vvvSource, vvvSynopticSource VVVDR1 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag3Err vvvVivaCatalogue VVVDR5 Error in default point source J mag, from VVVDR4 {catalogue TType keyword: jAperMag3Err} real 4 mag -9.999995e8

jAperMag4 ultravistaSource ULTRAVISTADR4 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 ultravistaSourceRemeasurement ULTRAVISTADR4 Point source J aperture corrected (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag4 vhsSource VHSDR1 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag4 vhsSource VHSDR2 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag4 vhsSource VHSDR3 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vhsSource VHSDR4 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vhsSource VHSDR5 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vhsSource VHSDR6 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vhsSource VHSv20120926 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag4 vhsSource VHSv20130417 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag4 vhsSource VHSv20140409 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vhsSource VHSv20150108 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vhsSource VHSv20160114 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vhsSource VHSv20160507 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vhsSource VHSv20170630 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vhsSource VHSv20180419 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vhsSource VHSv20201209 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vhsSource VHSv20231101 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vhsSource VHSv20240731 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 videoSource VIDEODR2 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag4 videoSource VIDEODR3 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag4 videoSource VIDEODR4 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 videoSource VIDEODR5 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 videoSource VIDEOv20100513 Extended source J mag, no aperture correction applied real 4 mag -0.9999995e9 phot.mag

jAperMag4 videoSource VIDEOv20111208 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag4 vikingSource VIKINGDR2 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag4 vikingSource VIKINGDR3 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag4 vikingSource VIKINGDR4 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vikingSource VIKINGv20110714 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag4 vikingSource VIKINGv20111019 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag4 vikingSource VIKINGv20130417 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag4 vikingSource VIKINGv20140402 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vikingSource VIKINGv20150421 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vikingSource VIKINGv20151230 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vikingSource VIKINGv20160406 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vikingSource VIKINGv20161202 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vikingSource VIKINGv20170715 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Point source J aperture corrected (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Point source J aperture corrected (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag4 vmcSource VMCDR1 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag4 vmcSource VMCDR2 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSource VMCDR3 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSource VMCDR4 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSource VMCDR5 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSource VMCv20110816 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag4 vmcSource VMCv20110909 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag4 vmcSource VMCv20120126 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag4 vmcSource VMCv20121128 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag4 vmcSource VMCv20130304 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag4 vmcSource VMCv20130805 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSource VMCv20140428 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSource VMCv20140903 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSource VMCv20150309 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSource VMCv20151218 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSource VMCv20160311 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSource VMCv20160822 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSource VMCv20170109 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSource VMCv20170411 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSource VMCv20171101 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSource VMCv20180702 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSource VMCv20181120 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSource VMCv20191212 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSource VMCv20210708 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSource VMCv20230816 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSource VMCv20240226 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSynopticSource VMCDR1 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag4 vmcSynopticSource VMCDR2 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSynopticSource VMCDR3 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSynopticSource VMCDR4 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSynopticSource VMCDR5 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSynopticSource VMCv20110816 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag4 vmcSynopticSource VMCv20110909 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag4 vmcSynopticSource VMCv20120126 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag4 vmcSynopticSource VMCv20121128 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag4 vmcSynopticSource VMCv20130304 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag4 vmcSynopticSource VMCv20130805 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSynopticSource VMCv20140428 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSynopticSource VMCv20140903 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSynopticSource VMCv20150309 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSynopticSource VMCv20151218 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSynopticSource VMCv20160311 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSynopticSource VMCv20160822 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSynopticSource VMCv20170109 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSynopticSource VMCv20170411 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSynopticSource VMCv20171101 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSynopticSource VMCv20180702 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSynopticSource VMCv20181120 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSynopticSource VMCv20191212 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSynopticSource VMCv20210708 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSynopticSource VMCv20230816 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcSynopticSource VMCv20240226 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcdeepSource VMCDEEPv20230713 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcdeepSource VMCDEEPv20240506 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcdeepSynopticSource VMCDEEPv20230713 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vmcdeepSynopticSource VMCDEEPv20240506 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vvvSource VVVDR2 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vvvSource VVVDR5 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag4 vvvSource VVVv20100531 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag4 vvvSource VVVv20110718 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag4 vvvSource, vvvSynopticSource VVVDR1 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag4Err ultravistaSource ULTRAVISTADR4 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err ultravistaSourceRemeasurement ULTRAVISTADR4 Error in point/extended source J (2.8 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error

jAperMag4Err vhsSource VHSDR1 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag4Err vhsSource VHSDR2 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag4Err vhsSource VHSDR3 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J

jAperMag4Err vhsSource VHSDR4 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag4Err vhsSource VHSDR5 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vhsSource VHSDR6 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vhsSource VHSv20120926 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag4Err vhsSource VHSv20130417 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag4Err vhsSource VHSv20140409 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J

jAperMag4Err vhsSource VHSv20150108 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag4Err vhsSource VHSv20160114 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vhsSource VHSv20160507 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vhsSource VHSv20170630 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vhsSource VHSv20180419 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vhsSource VHSv20201209 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vhsSource VHSv20231101 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vhsSource VHSv20240731 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err videoSource VIDEODR2 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag4Err videoSource VIDEODR3 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag4Err videoSource VIDEODR4 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag4Err videoSource VIDEODR5 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag4Err videoSource VIDEOv20100513 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag4Err videoSource VIDEOv20111208 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag4Err vikingSource VIKINGDR2 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag4Err vikingSource VIKINGDR3 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag4Err vikingSource VIKINGDR4 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J

jAperMag4Err vikingSource VIKINGv20110714 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag4Err vikingSource VIKINGv20111019 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag4Err vikingSource VIKINGv20130417 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag4Err vikingSource VIKINGv20140402 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag4Err vikingSource VIKINGv20150421 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag4Err vikingSource VIKINGv20151230 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vikingSource VIKINGv20160406 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vikingSource VIKINGv20161202 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vikingSource VIKINGv20170715 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in point/extended source J (2.8 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error

jAperMag4Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in point/extended source J (2.8 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error

jAperMag4Err vmcSource VMCDR1 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag4Err vmcSource VMCDR2 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag4Err vmcSource VMCDR3 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag4Err vmcSource VMCDR4 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vmcSource VMCDR5 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vmcSource VMCv20110816 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag4Err vmcSource VMCv20110909 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag4Err vmcSource VMCv20120126 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag4Err vmcSource VMCv20121128 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag4Err vmcSource VMCv20130304 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag4Err vmcSource VMCv20130805 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag4Err vmcSource VMCv20140428 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J

jAperMag4Err vmcSource VMCv20140903 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag4Err vmcSource VMCv20150309 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag4Err vmcSource VMCv20151218 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vmcSource VMCv20160311 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vmcSource VMCv20160822 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vmcSource VMCv20170109 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vmcSource VMCv20170411 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vmcSource VMCv20171101 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vmcSource VMCv20180702 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vmcSource VMCv20181120 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vmcSource VMCv20191212 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vmcSource VMCv20210708 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vmcSource VMCv20230816 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vmcSource VMCv20240226 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vmcSynopticSource VMCDR1 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag4Err vmcSynopticSource VMCDR2 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag4Err vmcSynopticSource VMCDR3 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag4Err vmcSynopticSource VMCDR4 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vmcSynopticSource VMCDR5 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vmcSynopticSource VMCv20110816 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag4Err vmcSynopticSource VMCv20110909 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag4Err vmcSynopticSource VMCv20120126 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag4Err vmcSynopticSource VMCv20121128 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag4Err vmcSynopticSource VMCv20130304 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag4Err vmcSynopticSource VMCv20130805 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag4Err vmcSynopticSource VMCv20140428 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J

jAperMag4Err vmcSynopticSource VMCv20140903 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag4Err vmcSynopticSource VMCv20150309 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag4Err vmcSynopticSource VMCv20151218 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vmcSynopticSource VMCv20160311 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vmcSynopticSource VMCv20160822 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vmcSynopticSource VMCv20170109 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vmcSynopticSource VMCv20170411 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vmcSynopticSource VMCv20171101 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vmcSynopticSource VMCv20180702 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vmcSynopticSource VMCv20181120 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vmcSynopticSource VMCv20191212 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vmcSynopticSource VMCv20210708 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vmcSynopticSource VMCv20230816 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vmcSynopticSource VMCv20240226 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vmcdeepSource VMCDEEPv20230713 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vmcdeepSource VMCDEEPv20240506 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vmcdeepSynopticSource VMCDEEPv20230713 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vmcdeepSynopticSource VMCDEEPv20240506 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vvvSource VVVDR2 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag4Err vvvSource VVVDR5 Error in point source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag4Err vvvSource VVVv20100531 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag4Err vvvSource VVVv20110718 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag4Err vvvSource, vvvSynopticSource VVVDR1 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag5 vmcSynopticSource VMCDR1 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag5 vmcSynopticSource VMCDR2 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag5 vmcSynopticSource VMCDR3 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag5 vmcSynopticSource VMCDR4 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag5 vmcSynopticSource VMCDR5 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag5 vmcSynopticSource VMCv20110816 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag5 vmcSynopticSource VMCv20110909 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag5 vmcSynopticSource VMCv20120126 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag5 vmcSynopticSource VMCv20121128 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag5 vmcSynopticSource VMCv20130304 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag5 vmcSynopticSource VMCv20130805 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag5 vmcSynopticSource VMCv20140428 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag5 vmcSynopticSource VMCv20140903 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag5 vmcSynopticSource VMCv20150309 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag5 vmcSynopticSource VMCv20151218 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag5 vmcSynopticSource VMCv20160311 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag5 vmcSynopticSource VMCv20160822 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag5 vmcSynopticSource VMCv20170109 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag5 vmcSynopticSource VMCv20170411 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag5 vmcSynopticSource VMCv20171101 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag5 vmcSynopticSource VMCv20180702 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag5 vmcSynopticSource VMCv20181120 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag5 vmcSynopticSource VMCv20191212 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag5 vmcSynopticSource VMCv20210708 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag5 vmcSynopticSource VMCv20230816 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag5 vmcSynopticSource VMCv20240226 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag5 vmcdeepSynopticSource VMCDEEPv20230713 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag5 vmcdeepSynopticSource VMCDEEPv20240506 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag5 vvvSynopticSource VVVDR1 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag5 vvvSynopticSource VVVDR2 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag5Err vmcSynopticSource VMCDR1 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag5Err vmcSynopticSource VMCDR2 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag5Err vmcSynopticSource VMCDR3 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag5Err vmcSynopticSource VMCDR4 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag5Err vmcSynopticSource VMCDR5 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag5Err vmcSynopticSource VMCv20110816 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag5Err vmcSynopticSource VMCv20110909 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag5Err vmcSynopticSource VMCv20120126 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag5Err vmcSynopticSource VMCv20121128 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag5Err vmcSynopticSource VMCv20130304 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag5Err vmcSynopticSource VMCv20130805 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag5Err vmcSynopticSource VMCv20140428 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J

jAperMag5Err vmcSynopticSource VMCv20140903 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag5Err vmcSynopticSource VMCv20150309 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag5Err vmcSynopticSource VMCv20151218 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag5Err vmcSynopticSource VMCv20160311 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag5Err vmcSynopticSource VMCv20160822 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag5Err vmcSynopticSource VMCv20170109 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag5Err vmcSynopticSource VMCv20170411 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag5Err vmcSynopticSource VMCv20171101 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag5Err vmcSynopticSource VMCv20180702 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag5Err vmcSynopticSource VMCv20181120 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag5Err vmcSynopticSource VMCv20191212 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag5Err vmcSynopticSource VMCv20210708 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag5Err vmcSynopticSource VMCv20230816 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag5Err vmcSynopticSource VMCv20240226 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag5Err vmcdeepSynopticSource VMCDEEPv20230713 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag5Err vmcdeepSynopticSource VMCDEEPv20240506 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag5Err vvvSynopticSource VVVDR1 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag5Err vvvSynopticSource VVVDR2 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag6 ultravistaSource ULTRAVISTADR4 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 ultravistaSourceRemeasurement ULTRAVISTADR4 Point source J aperture corrected (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag6 vhsSource VHSDR1 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag6 vhsSource VHSDR2 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag6 vhsSource VHSDR3 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vhsSource VHSDR4 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vhsSource VHSDR5 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vhsSource VHSDR6 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vhsSource VHSv20120926 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag6 vhsSource VHSv20130417 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag6 vhsSource VHSv20140409 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vhsSource VHSv20150108 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vhsSource VHSv20160114 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vhsSource VHSv20160507 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vhsSource VHSv20170630 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vhsSource VHSv20180419 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vhsSource VHSv20201209 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vhsSource VHSv20231101 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vhsSource VHSv20240731 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 videoSource VIDEODR2 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag6 videoSource VIDEODR3 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag6 videoSource VIDEODR4 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 videoSource VIDEODR5 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 videoSource VIDEOv20100513 Extended source J mag, no aperture correction applied real 4 mag -0.9999995e9 phot.mag

jAperMag6 videoSource VIDEOv20111208 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag6 vikingSource VIKINGDR2 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag6 vikingSource VIKINGDR3 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag6 vikingSource VIKINGDR4 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vikingSource VIKINGv20110714 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag6 vikingSource VIKINGv20111019 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag6 vikingSource VIKINGv20130417 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag6 vikingSource VIKINGv20140402 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vikingSource VIKINGv20150421 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vikingSource VIKINGv20151230 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vikingSource VIKINGv20160406 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vikingSource VIKINGv20161202 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vikingSource VIKINGv20170715 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Point source J aperture corrected (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Point source J aperture corrected (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag6 vmcSource VMCDR1 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag6 vmcSource VMCDR2 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vmcSource VMCDR3 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vmcSource VMCDR4 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vmcSource VMCDR5 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vmcSource VMCv20110816 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag6 vmcSource VMCv20110909 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag6 vmcSource VMCv20120126 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag6 vmcSource VMCv20121128 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag6 vmcSource VMCv20130304 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag6 vmcSource VMCv20130805 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vmcSource VMCv20140428 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vmcSource VMCv20140903 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vmcSource VMCv20150309 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vmcSource VMCv20151218 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vmcSource VMCv20160311 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vmcSource VMCv20160822 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vmcSource VMCv20170109 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vmcSource VMCv20170411 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vmcSource VMCv20171101 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vmcSource VMCv20180702 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vmcSource VMCv20181120 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vmcSource VMCv20191212 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vmcSource VMCv20210708 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vmcSource VMCv20230816 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vmcSource VMCv20240226 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vmcdeepSource VMCDEEPv20230713 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6 vmcdeepSource VMCDEEPv20240506 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMag6Err ultravistaSource ULTRAVISTADR4 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag6Err ultravistaSourceRemeasurement ULTRAVISTADR4 Error in point/extended source J (5.7 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error

jAperMag6Err vhsSource VHSDR1 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag6Err vhsSource VHSDR2 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag6Err vhsSource VHSDR3 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J

jAperMag6Err vhsSource VHSDR4 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag6Err vhsSource VHSDR5 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag6Err vhsSource VHSDR6 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag6Err vhsSource VHSv20120926 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag6Err vhsSource VHSv20130417 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag6Err vhsSource VHSv20140409 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J

jAperMag6Err vhsSource VHSv20150108 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag6Err vhsSource VHSv20160114 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag6Err vhsSource VHSv20160507 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag6Err vhsSource VHSv20170630 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag6Err vhsSource VHSv20180419 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag6Err vhsSource VHSv20201209 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag6Err vhsSource VHSv20231101 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag6Err vhsSource VHSv20240731 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag6Err videoSource VIDEODR2 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag6Err videoSource VIDEODR3 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag6Err videoSource VIDEODR4 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag6Err videoSource VIDEODR5 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag6Err videoSource VIDEOv20100513 Error in extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag6Err videoSource VIDEOv20111208 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag6Err vikingSource VIKINGDR2 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag6Err vikingSource VIKINGDR3 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag6Err vikingSource VIKINGDR4 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J

jAperMag6Err vikingSource VIKINGv20110714 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag6Err vikingSource VIKINGv20111019 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag6Err vikingSource VIKINGv20130417 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag6Err vikingSource VIKINGv20140402 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag6Err vikingSource VIKINGv20150421 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag6Err vikingSource VIKINGv20151230 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag6Err vikingSource VIKINGv20160406 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag6Err vikingSource VIKINGv20161202 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag6Err vikingSource VIKINGv20170715 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag6Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in point/extended source J (5.7 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error

jAperMag6Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in point/extended source J (5.7 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error

jAperMag6Err vmcSource VMCDR1 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag6Err vmcSource VMCDR2 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag6Err vmcSource VMCDR3 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag6Err vmcSource VMCDR4 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag6Err vmcSource VMCDR5 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag6Err vmcSource VMCv20110816 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag6Err vmcSource VMCv20110909 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag6Err vmcSource VMCv20120126 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag6Err vmcSource VMCv20121128 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag6Err vmcSource VMCv20130304 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag6Err vmcSource VMCv20130805 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error

jAperMag6Err vmcSource VMCv20140428 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J

jAperMag6Err vmcSource VMCv20140903 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag6Err vmcSource VMCv20150309 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag

jAperMag6Err vmcSource VMCv20151218 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag6Err vmcSource VMCv20160311 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag6Err vmcSource VMCv20160822 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag6Err vmcSource VMCv20170109 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag6Err vmcSource VMCv20170411 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag6Err vmcSource VMCv20171101 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag6Err vmcSource VMCv20180702 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag6Err vmcSource VMCv20181120 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag6Err vmcSource VMCv20191212 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag6Err vmcSource VMCv20210708 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag6Err vmcSource VMCv20230816 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag6Err vmcSource VMCv20240226 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag6Err vmcdeepSource VMCDEEPv20230713 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMag6Err vmcdeepSource VMCDEEPv20240506 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J

jAperMagNoAperCorr3 ultravistaSource ULTRAVISTADR4 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 ultravistaSourceRemeasurement ULTRAVISTADR4 Default extended source J (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

jAperMagNoAperCorr3 vhsSource VHSDR1 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr3 vhsSource VHSDR2 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr3 vhsSource VHSDR3 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vhsSource VHSDR4 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vhsSource VHSDR5 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vhsSource VHSDR6 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vhsSource VHSv20120926 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr3 vhsSource VHSv20130417 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr3 vhsSource VHSv20140409 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vhsSource VHSv20150108 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vhsSource VHSv20160114 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vhsSource VHSv20160507 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vhsSource VHSv20170630 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vhsSource VHSv20180419 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vhsSource VHSv20201209 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vhsSource VHSv20231101 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vhsSource VHSv20240731 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 videoSource VIDEODR2 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr3 videoSource VIDEODR3 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr3 videoSource VIDEODR4 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 videoSource VIDEODR5 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 videoSource VIDEOv20111208 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr3 vikingSource VIKINGDR2 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr3 vikingSource VIKINGDR3 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr3 vikingSource VIKINGDR4 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vikingSource VIKINGv20110714 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr3 vikingSource VIKINGv20111019 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr3 vikingSource VIKINGv20130417 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr3 vikingSource VIKINGv20140402 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vikingSource VIKINGv20150421 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vikingSource VIKINGv20151230 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vikingSource VIKINGv20160406 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vikingSource VIKINGv20161202 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vikingSource VIKINGv20170715 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Default extended source J (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

jAperMagNoAperCorr3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Default extended source J (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

jAperMagNoAperCorr3 vmcSource VMCDR1 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr3 vmcSource VMCDR2 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vmcSource VMCDR3 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vmcSource VMCDR4 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vmcSource VMCDR5 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vmcSource VMCv20110816 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr3 vmcSource VMCv20110909 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr3 vmcSource VMCv20120126 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr3 vmcSource VMCv20121128 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr3 vmcSource VMCv20130304 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr3 vmcSource VMCv20130805 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vmcSource VMCv20140428 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vmcSource VMCv20140903 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vmcSource VMCv20150309 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vmcSource VMCv20151218 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vmcSource VMCv20160311 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vmcSource VMCv20160822 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vmcSource VMCv20170109 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vmcSource VMCv20170411 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vmcSource VMCv20171101 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vmcSource VMCv20180702 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vmcSource VMCv20181120 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vmcSource VMCv20191212 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vmcSource VMCv20210708 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vmcSource VMCv20230816 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vmcSource VMCv20240226 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vmcdeepSource VMCDEEPv20230713 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr3 vmcdeepSource VMCDEEPv20240506 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 ultravistaSource ULTRAVISTADR4 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 ultravistaSourceRemeasurement ULTRAVISTADR4 Extended source J (2.8 arcsec aperture diameter, but no aperture correction applied) aperture magnitude real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr4 vhsSource VHSDR1 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr4 vhsSource VHSDR2 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr4 vhsSource VHSDR3 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vhsSource VHSDR4 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vhsSource VHSDR5 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vhsSource VHSDR6 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vhsSource VHSv20120926 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr4 vhsSource VHSv20130417 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr4 vhsSource VHSv20140409 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vhsSource VHSv20150108 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vhsSource VHSv20160114 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vhsSource VHSv20160507 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vhsSource VHSv20170630 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vhsSource VHSv20180419 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vhsSource VHSv20201209 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vhsSource VHSv20231101 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vhsSource VHSv20240731 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 videoSource VIDEODR2 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr4 videoSource VIDEODR3 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr4 videoSource VIDEODR4 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 videoSource VIDEODR5 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 videoSource VIDEOv20111208 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr4 vikingSource VIKINGDR2 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr4 vikingSource VIKINGDR3 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr4 vikingSource VIKINGDR4 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vikingSource VIKINGv20110714 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr4 vikingSource VIKINGv20111019 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr4 vikingSource VIKINGv20130417 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr4 vikingSource VIKINGv20140402 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vikingSource VIKINGv20150421 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vikingSource VIKINGv20151230 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vikingSource VIKINGv20160406 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vikingSource VIKINGv20161202 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vikingSource VIKINGv20170715 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Extended source J (2.8 arcsec aperture diameter, but no aperture correction applied) aperture magnitude real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Extended source J (2.8 arcsec aperture diameter, but no aperture correction applied) aperture magnitude real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr4 vmcSource VMCDR1 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr4 vmcSource VMCDR2 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vmcSource VMCDR3 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vmcSource VMCDR4 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vmcSource VMCDR5 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vmcSource VMCv20110816 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr4 vmcSource VMCv20110909 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr4 vmcSource VMCv20120126 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr4 vmcSource VMCv20121128 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr4 vmcSource VMCv20130304 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr4 vmcSource VMCv20130805 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vmcSource VMCv20140428 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vmcSource VMCv20140903 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vmcSource VMCv20150309 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vmcSource VMCv20151218 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vmcSource VMCv20160311 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vmcSource VMCv20160822 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vmcSource VMCv20170109 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vmcSource VMCv20170411 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vmcSource VMCv20171101 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vmcSource VMCv20180702 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vmcSource VMCv20181120 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vmcSource VMCv20191212 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vmcSource VMCv20210708 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vmcSource VMCv20230816 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vmcSource VMCv20240226 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vmcdeepSource VMCDEEPv20230713 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr4 vmcdeepSource VMCDEEPv20240506 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 ultravistaSource ULTRAVISTADR4 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 ultravistaSourceRemeasurement ULTRAVISTADR4 Extended source J (5.7 arcsec aperture diameter, but no aperture correction applied) aperture magnitude real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr6 vhsSource VHSDR1 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr6 vhsSource VHSDR2 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr6 vhsSource VHSDR3 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vhsSource VHSDR4 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vhsSource VHSDR5 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vhsSource VHSDR6 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vhsSource VHSv20120926 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr6 vhsSource VHSv20130417 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr6 vhsSource VHSv20140409 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vhsSource VHSv20150108 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vhsSource VHSv20160114 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vhsSource VHSv20160507 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vhsSource VHSv20170630 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vhsSource VHSv20180419 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vhsSource VHSv20201209 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vhsSource VHSv20231101 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vhsSource VHSv20240731 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 videoSource VIDEODR2 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr6 videoSource VIDEODR3 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr6 videoSource VIDEODR4 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 videoSource VIDEODR5 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 videoSource VIDEOv20111208 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr6 vikingSource VIKINGDR2 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr6 vikingSource VIKINGDR3 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr6 vikingSource VIKINGDR4 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vikingSource VIKINGv20110714 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr6 vikingSource VIKINGv20111019 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr6 vikingSource VIKINGv20130417 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr6 vikingSource VIKINGv20140402 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vikingSource VIKINGv20150421 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vikingSource VIKINGv20151230 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vikingSource VIKINGv20160406 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vikingSource VIKINGv20161202 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vikingSource VIKINGv20170715 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Extended source J (5.7 arcsec aperture diameter, but no aperture correction applied) aperture magnitude real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Extended source J (5.7 arcsec aperture diameter, but no aperture correction applied) aperture magnitude real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr6 vmcSource VMCDR1 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr6 vmcSource VMCDR2 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vmcSource VMCDR3 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vmcSource VMCDR4 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vmcSource VMCDR5 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vmcSource VMCv20110816 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr6 vmcSource VMCv20110909 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr6 vmcSource VMCv20120126 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr6 vmcSource VMCv20121128 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr6 vmcSource VMCv20130304 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr6 vmcSource VMCv20130805 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vmcSource VMCv20140428 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vmcSource VMCv20140903 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vmcSource VMCv20150309 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vmcSource VMCv20151218 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vmcSource VMCv20160311 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vmcSource VMCv20160822 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vmcSource VMCv20170109 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vmcSource VMCv20170411 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vmcSource VMCv20171101 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vmcSource VMCv20180702 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vmcSource VMCv20181120 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vmcSource VMCv20191212 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vmcSource VMCv20210708 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vmcSource VMCv20230816 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vmcSource VMCv20240226 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vmcdeepSource VMCDEEPv20230713 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jAperMagNoAperCorr6 vmcdeepSource VMCDEEPv20240506 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J

jaStratAst ultravistaVarFrameSetInfo ULTRAVISTADR4 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratAst videoVarFrameSetInfo VIDEODR2 Strateva parameter, a, in fit to astrometric rms vs magnitude in J 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.

jaStratAst videoVarFrameSetInfo VIDEODR3 Strateva parameter, a, in fit to astrometric rms vs magnitude in J 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.

jaStratAst videoVarFrameSetInfo VIDEODR4 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratAst videoVarFrameSetInfo VIDEODR5 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratAst videoVarFrameSetInfo VIDEOv20100513 Strateva parameter, a, in fit to astrometric rms vs magnitude in J 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.

jaStratAst videoVarFrameSetInfo VIDEOv20111208 Strateva parameter, a, in fit to astrometric rms vs magnitude in J 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.

jaStratAst vikingVarFrameSetInfo VIKINGDR2 Strateva parameter, a, in fit to astrometric rms vs magnitude in J 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.

jaStratAst vikingVarFrameSetInfo VIKINGDR3 Strateva parameter, a, in fit to astrometric rms vs magnitude in J 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.

jaStratAst vikingVarFrameSetInfo VIKINGDR4 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratAst vikingVarFrameSetInfo VIKINGv20110714 Strateva parameter, a, in fit to astrometric rms vs magnitude in J 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.

jaStratAst vikingVarFrameSetInfo VIKINGv20111019 Strateva parameter, a, in fit to astrometric rms vs magnitude in J 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.

jaStratAst vikingVarFrameSetInfo VIKINGv20130417 Strateva parameter, a, in fit to astrometric rms vs magnitude in J 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.

jaStratAst vikingVarFrameSetInfo VIKINGv20140402 Strateva parameter, a, in fit to astrometric rms vs magnitude in J 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.

jaStratAst vikingVarFrameSetInfo VIKINGv20150421 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratAst vikingVarFrameSetInfo VIKINGv20151230 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratAst vikingVarFrameSetInfo VIKINGv20160406 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratAst vikingVarFrameSetInfo VIKINGv20161202 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratAst vikingVarFrameSetInfo VIKINGv20170715 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratAst vmcVarFrameSetInfo VMCDR1 Strateva parameter, a, in fit to astrometric rms vs magnitude in J 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.

jaStratAst vmcVarFrameSetInfo VMCDR2 Strateva parameter, a, in fit to astrometric rms vs magnitude in J 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.

jaStratAst vmcVarFrameSetInfo VMCDR3 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratAst vmcVarFrameSetInfo VMCDR4 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratAst vmcVarFrameSetInfo VMCDR5 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratAst vmcVarFrameSetInfo VMCv20110816 Strateva parameter, a, in fit to astrometric rms vs magnitude in J 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.

jaStratAst vmcVarFrameSetInfo VMCv20110909 Strateva parameter, a, in fit to astrometric rms vs magnitude in J 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.

jaStratAst vmcVarFrameSetInfo VMCv20120126 Strateva parameter, a, in fit to astrometric rms vs magnitude in J 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.

jaStratAst vmcVarFrameSetInfo VMCv20121128 Strateva parameter, a, in fit to astrometric rms vs magnitude in J 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.

jaStratAst vmcVarFrameSetInfo VMCv20130304 Strateva parameter, a, in fit to astrometric rms vs magnitude in J 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.

jaStratAst vmcVarFrameSetInfo VMCv20130805 Strateva parameter, a, in fit to astrometric rms vs magnitude in J 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.

jaStratAst vmcVarFrameSetInfo VMCv20140428 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratAst vmcVarFrameSetInfo VMCv20140903 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratAst vmcVarFrameSetInfo VMCv20150309 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratAst vmcVarFrameSetInfo VMCv20151218 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratAst vmcVarFrameSetInfo VMCv20160311 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratAst vmcVarFrameSetInfo VMCv20160822 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratAst vmcVarFrameSetInfo VMCv20170109 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratAst vmcVarFrameSetInfo VMCv20170411 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratAst vmcVarFrameSetInfo VMCv20171101 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratAst vmcVarFrameSetInfo VMCv20180702 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratAst vmcVarFrameSetInfo VMCv20181120 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratAst vmcVarFrameSetInfo VMCv20191212 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratAst vmcVarFrameSetInfo VMCv20210708 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratAst vmcVarFrameSetInfo VMCv20230816 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratAst vmcVarFrameSetInfo VMCv20240226 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratAst vmcdeepVarFrameSetInfo VMCDEEPv20230713 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratAst vmcdeepVarFrameSetInfo VMCDEEPv20240506 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratAst vvvVarFrameSetInfo VVVDR5 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratAst vvvVarFrameSetInfo VVVv20100531 Strateva parameter, a, in fit to astrometric rms vs magnitude in J 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.

jaStratPht ultravistaMapLcVarFrameSetInfo ULTRAVISTADR4 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratPht ultravistaVarFrameSetInfo ULTRAVISTADR4 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratPht videoVarFrameSetInfo VIDEODR2 Strateva parameter, a, in fit to photometric rms vs magnitude in J 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.

jaStratPht videoVarFrameSetInfo VIDEODR3 Strateva parameter, a, in fit to photometric rms vs magnitude in J 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.

jaStratPht videoVarFrameSetInfo VIDEODR4 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratPht videoVarFrameSetInfo VIDEODR5 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratPht videoVarFrameSetInfo VIDEOv20100513 Strateva parameter, a, in fit to photometric rms vs magnitude in J 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.

jaStratPht videoVarFrameSetInfo VIDEOv20111208 Strateva parameter, a, in fit to photometric rms vs magnitude in J 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.

jaStratPht vikingVarFrameSetInfo VIKINGDR2 Strateva parameter, a, in fit to photometric rms vs magnitude in J 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.

jaStratPht vikingVarFrameSetInfo VIKINGDR3 Strateva parameter, a, in fit to photometric rms vs magnitude in J 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.

jaStratPht vikingVarFrameSetInfo VIKINGDR4 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratPht vikingVarFrameSetInfo VIKINGv20110714 Strateva parameter, a, in fit to photometric rms vs magnitude in J 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.

jaStratPht vikingVarFrameSetInfo VIKINGv20111019 Strateva parameter, a, in fit to photometric rms vs magnitude in J 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.

jaStratPht vikingVarFrameSetInfo VIKINGv20130417 Strateva parameter, a, in fit to photometric rms vs magnitude in J 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.

jaStratPht vikingVarFrameSetInfo VIKINGv20140402 Strateva parameter, a, in fit to photometric rms vs magnitude in J 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.

jaStratPht vikingVarFrameSetInfo VIKINGv20150421 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratPht vikingVarFrameSetInfo VIKINGv20151230 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratPht vikingVarFrameSetInfo VIKINGv20160406 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratPht vikingVarFrameSetInfo VIKINGv20161202 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratPht vikingVarFrameSetInfo VIKINGv20170715 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratPht vmcVarFrameSetInfo VMCDR1 Strateva parameter, a, in fit to photometric rms vs magnitude in J 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.

jaStratPht vmcVarFrameSetInfo VMCDR2 Strateva parameter, a, in fit to photometric rms vs magnitude in J 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.

jaStratPht vmcVarFrameSetInfo VMCDR3 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratPht vmcVarFrameSetInfo VMCDR4 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratPht vmcVarFrameSetInfo VMCDR5 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratPht vmcVarFrameSetInfo VMCv20110816 Strateva parameter, a, in fit to photometric rms vs magnitude in J 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.

jaStratPht vmcVarFrameSetInfo VMCv20110909 Strateva parameter, a, in fit to photometric rms vs magnitude in J 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.

jaStratPht vmcVarFrameSetInfo VMCv20120126 Strateva parameter, a, in fit to photometric rms vs magnitude in J 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.

jaStratPht vmcVarFrameSetInfo VMCv20121128 Strateva parameter, a, in fit to photometric rms vs magnitude in J 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.

jaStratPht vmcVarFrameSetInfo VMCv20130304 Strateva parameter, a, in fit to photometric rms vs magnitude in J 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.

jaStratPht vmcVarFrameSetInfo VMCv20130805 Strateva parameter, a, in fit to photometric rms vs magnitude in J 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.

jaStratPht vmcVarFrameSetInfo VMCv20140428 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratPht vmcVarFrameSetInfo VMCv20140903 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratPht vmcVarFrameSetInfo VMCv20150309 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratPht vmcVarFrameSetInfo VMCv20151218 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratPht vmcVarFrameSetInfo VMCv20160311 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratPht vmcVarFrameSetInfo VMCv20160822 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratPht vmcVarFrameSetInfo VMCv20170109 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratPht vmcVarFrameSetInfo VMCv20170411 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratPht vmcVarFrameSetInfo VMCv20171101 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratPht vmcVarFrameSetInfo VMCv20180702 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratPht vmcVarFrameSetInfo VMCv20181120 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratPht vmcVarFrameSetInfo VMCv20191212 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratPht vmcVarFrameSetInfo VMCv20210708 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratPht vmcVarFrameSetInfo VMCv20230816 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratPht vmcVarFrameSetInfo VMCv20240226 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratPht vmcdeepVarFrameSetInfo VMCDEEPv20230713 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratPht vmcdeepVarFrameSetInfo VMCDEEPv20240506 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratPht vvvVarFrameSetInfo VVVDR5 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jaStratPht vvvVarFrameSetInfo VVVv20100531 Strateva parameter, a, in fit to photometric rms vs magnitude in J 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.

jAverageConf ultravistaSourceRemeasurement ULTRAVISTADR4 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.NIR

jAverageConf vhsSource VHSDR1 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -99999999 meta.code

jAverageConf vhsSource VHSDR2 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -99999999 meta.code

jAverageConf vhsSource VHSDR3 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vhsSource VHSDR4 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vhsSource VHSDR5 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vhsSource VHSDR6 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vhsSource VHSv20120926 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -99999999 stat.likelihood;em.IR.NIR

jAverageConf vhsSource VHSv20130417 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.NIR

jAverageConf vhsSource VHSv20140409 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vhsSource VHSv20150108 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vhsSource VHSv20160114 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vhsSource VHSv20160507 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vhsSource VHSv20170630 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vhsSource VHSv20180419 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vhsSource VHSv20201209 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vhsSource VHSv20231101 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vhsSource VHSv20240731 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vikingSource VIKINGDR2 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -99999999 meta.code

jAverageConf vikingSource VIKINGDR3 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -99999999 stat.likelihood;em.IR.NIR

jAverageConf vikingSource VIKINGDR4 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vikingSource VIKINGv20110714 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -99999999 meta.code

jAverageConf vikingSource VIKINGv20111019 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -99999999 meta.code

jAverageConf vikingSource VIKINGv20130417 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.NIR

jAverageConf vikingSource VIKINGv20140402 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.NIR

jAverageConf vikingSource VIKINGv20150421 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vikingSource VIKINGv20151230 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vikingSource VIKINGv20160406 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vikingSource VIKINGv20161202 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vikingSource VIKINGv20170715 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.NIR

jAverageConf vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.NIR

jAverageConf vmcSource VMCDR2 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.NIR

jAverageConf vmcSource VMCDR3 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vmcSource VMCDR4 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vmcSource VMCDR5 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vmcSource VMCv20110816 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -99999999 meta.code

jAverageConf vmcSource VMCv20110909 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -99999999 meta.code

jAverageConf vmcSource VMCv20120126 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -99999999 meta.code

jAverageConf vmcSource VMCv20121128 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -99999999 stat.likelihood;em.IR.NIR

jAverageConf vmcSource VMCv20130304 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.NIR

jAverageConf vmcSource VMCv20130805 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.NIR

jAverageConf vmcSource VMCv20140428 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vmcSource VMCv20140903 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vmcSource VMCv20150309 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vmcSource VMCv20151218 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vmcSource VMCv20160311 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vmcSource VMCv20160822 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vmcSource VMCv20170109 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vmcSource VMCv20170411 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vmcSource VMCv20171101 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vmcSource VMCv20180702 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vmcSource VMCv20181120 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vmcSource VMCv20191212 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vmcSource VMCv20210708 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vmcSource VMCv20230816 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vmcSource VMCv20240226 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vmcSource, vmcSynopticSource VMCDR1 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -99999999 meta.code

jAverageConf vmcdeepSource VMCDEEPv20240506 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vmcdeepSource, vmcdeepSynopticSource VMCDEEPv20230713 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.J

jAverageConf vvvSource VVVDR2 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.NIR

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

jAverageConf vvvSource, vvvSynopticSource VVVDR1 average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -99999999 stat.likelihood;em.IR.NIR

jbestAper ultravistaMapLcVariability ULTRAVISTADR4 Best aperture (1-3) for photometric statistics in the J 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)

jbestAper ultravistaVariability ULTRAVISTADR4 Best aperture (1-6) for photometric statistics in the J band int 4 -9999 meta.code.class;em.IR.J

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)

jbestAper videoVariability VIDEODR2 Best aperture (1-6) for photometric statistics in the J 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)

jbestAper videoVariability VIDEODR3 Best aperture (1-6) for photometric statistics in the J 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)

jbestAper videoVariability VIDEODR4 Best aperture (1-6) for photometric statistics in the J band int 4 -9999 meta.code.class;em.IR.J

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)

jbestAper videoVariability VIDEODR5 Best aperture (1-6) for photometric statistics in the J band int 4 -9999 meta.code.class;em.IR.J

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)

jbestAper videoVariability VIDEOv20100513 Best aperture (1-6) for photometric statistics in the J 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)

jbestAper videoVariability VIDEOv20111208 Best aperture (1-6) for photometric statistics in the J 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)

jbestAper vikingVariability VIKINGDR2 Best aperture (1-6) for photometric statistics in the J 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)

jbestAper vikingVariability VIKINGDR3 Best aperture (1-6) for photometric statistics in the J 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)

jbestAper vikingVariability VIKINGDR4 Best aperture (1-6) for photometric statistics in the J band int 4 -9999 meta.code.class;em.IR.J

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)

jbestAper vikingVariability VIKINGv20110714 Best aperture (1-6) for photometric statistics in the J 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)

jbestAper vikingVariability VIKINGv20111019 Best aperture (1-6) for photometric statistics in the J 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)

jbestAper vikingVariability VIKINGv20130417 Best aperture (1-6) for photometric statistics in the J 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)

jbestAper vikingVariability VIKINGv20140402 Best aperture (1-6) for photometric statistics in the J 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)

jbestAper vikingVariability VIKINGv20150421 Best aperture (1-6) for photometric statistics in the J band int 4 -9999 meta.code.class;em.IR.J

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)

jbestAper vikingVariability VIKINGv20151230 Best aperture (1-6) for photometric statistics in the J band int 4 -9999 meta.code.class;em.IR.J

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)

jbestAper vikingVariability VIKINGv20160406 Best aperture (1-6) for photometric statistics in the J band int 4 -9999 meta.code.class;em.IR.J

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)

jbestAper vikingVariability VIKINGv20161202 Best aperture (1-6) for photometric statistics in the J band int 4 -9999 meta.code.class;em.IR.J

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)

jbestAper vikingVariability VIKINGv20170715 Best aperture (1-6) for photometric statistics in the J band int 4 -9999 meta.code.class;em.IR.J

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)

jbestAper vmcVariability VMCDR1 Best aperture (1-6) for photometric statistics in the J 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)

jbestAper vmcVariability VMCDR2 Best aperture (1-6) for photometric statistics in the J 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)

jbestAper vmcVariability VMCDR3 Best aperture (1-6) for photometric statistics in the J band int 4 -9999 meta.code.class;em.IR.J

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)

jbestAper vmcVariability VMCDR4 Best aperture (1-6) for photometric statistics in the J band int 4 -9999 meta.code.class;em.IR.J

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)

jbestAper vmcVariability VMCDR5 Best aperture (1-6) for photometric statistics in the J band int 4 -9999 meta.code.class;em.IR.J

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)

jbestAper vmcVariability VMCv20110816 Best aperture (1-6) for photometric statistics in the J 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)

jbestAper vmcVariability VMCv20110909 Best aperture (1-6) for photometric statistics in the J 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)

jbestAper vmcVariability VMCv20120126 Best aperture (1-6) for photometric statistics in the J 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)

jbestAper vmcVariability VMCv20121128 Best aperture (1-6) for photometric statistics in the J 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)

jbestAper vmcVariability VMCv20130304 Best aperture (1-6) for photometric statistics in the J 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)

jbestAper vmcVariability VMCv20130805 Best aperture (1-6) for photometric statistics in the J 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)

jbestAper vmcVariability VMCv20140428 Best aperture (1-6) for photometric statistics in the J band int 4 -9999 meta.code.class;em.IR.J

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)

jbestAper vmcVariability VMCv20140903 Best aperture (1-6) for photometric statistics in the J band int 4 -9999 meta.code.class;em.IR.J

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)

jbestAper vmcVariability VMCv20150309 Best aperture (1-6) for photometric statistics in the J band int 4 -9999 meta.code.class;em.IR.J

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)

jbestAper vmcVariability VMCv20151218 Best aperture (1-6) for photometric statistics in the J band int 4 -9999 meta.code.class;em.IR.J

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)

jbestAper vmcVariability VMCv20160311 Best aperture (1-6) for photometric statistics in the J band int 4 -9999 meta.code.class;em.IR.J

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)

jbestAper vmcVariability VMCv20160822 Best aperture (1-6) for photometric statistics in the J band int 4 -9999 meta.code.class;em.IR.J

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)

jbestAper vmcVariability VMCv20170109 Best aperture (1-6) for photometric statistics in the J band int 4 -9999 meta.code.class;em.IR.J

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)

jbestAper vmcVariability VMCv20170411 Best aperture (1-6) for photometric statistics in the J band int 4 -9999 meta.code.class;em.IR.J

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)

jbestAper vmcVariability VMCv20171101 Best aperture (1-6) for photometric statistics in the J band int 4 -9999 meta.code.class;em.IR.J

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)

jbestAper vmcVariability VMCv20180702 Best aperture (1-6) for photometric statistics in the J band int 4 -9999 meta.code.class;em.IR.J

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)

jbestAper vmcVariability VMCv20181120 Best aperture (1-6) for photometric statistics in the J band int 4 -9999 meta.code.class;em.IR.J

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)

jbestAper vmcVariability VMCv20191212 Best aperture (1-6) for photometric statistics in the J band int 4 -9999 meta.code.class;em.IR.J

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)

jbestAper vmcVariability VMCv20210708 Best aperture (1-6) for photometric statistics in the J band int 4 -9999 meta.code.class;em.IR.J

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)

jbestAper vmcVariability VMCv20230816 Best aperture (1-6) for photometric statistics in the J band int 4 -9999 meta.code.class;em.IR.J

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)

jbestAper vmcVariability VMCv20240226 Best aperture (1-6) for photometric statistics in the J band int 4 -9999 meta.code.class;em.IR.J

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)

jbestAper vmcdeepVariability VMCDEEPv20230713 Best aperture (1-6) for photometric statistics in the J band int 4 -9999 meta.code.class;em.IR.J

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)

jbestAper vmcdeepVariability VMCDEEPv20240506 Best aperture (1-6) for photometric statistics in the J band int 4 -9999 meta.code.class;em.IR.J

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)

jbestAper vvvVariability VVVDR5 Best aperture (1-6) for photometric statistics in the J band int 4 -9999 meta.code.class;em.IR.J

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)

jbestAper vvvVariability VVVv20100531 Best aperture (1-6) for photometric statistics in the J 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)

jbStratAst ultravistaVarFrameSetInfo ULTRAVISTADR4 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratAst videoVarFrameSetInfo VIDEODR2 Strateva parameter, b, in fit to astrometric rms vs magnitude in J 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.

jbStratAst videoVarFrameSetInfo VIDEODR3 Strateva parameter, b, in fit to astrometric rms vs magnitude in J 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.

jbStratAst videoVarFrameSetInfo VIDEODR4 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratAst videoVarFrameSetInfo VIDEODR5 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratAst videoVarFrameSetInfo VIDEOv20100513 Strateva parameter, b, in fit to astrometric rms vs magnitude in J 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.

jbStratAst videoVarFrameSetInfo VIDEOv20111208 Strateva parameter, b, in fit to astrometric rms vs magnitude in J 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.

jbStratAst vikingVarFrameSetInfo VIKINGDR2 Strateva parameter, b, in fit to astrometric rms vs magnitude in J 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.

jbStratAst vikingVarFrameSetInfo VIKINGDR3 Strateva parameter, b, in fit to astrometric rms vs magnitude in J 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.

jbStratAst vikingVarFrameSetInfo VIKINGDR4 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratAst vikingVarFrameSetInfo VIKINGv20110714 Strateva parameter, b, in fit to astrometric rms vs magnitude in J 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.

jbStratAst vikingVarFrameSetInfo VIKINGv20111019 Strateva parameter, b, in fit to astrometric rms vs magnitude in J 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.

jbStratAst vikingVarFrameSetInfo VIKINGv20130417 Strateva parameter, b, in fit to astrometric rms vs magnitude in J 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.

jbStratAst vikingVarFrameSetInfo VIKINGv20140402 Strateva parameter, b, in fit to astrometric rms vs magnitude in J 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.

jbStratAst vikingVarFrameSetInfo VIKINGv20150421 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratAst vikingVarFrameSetInfo VIKINGv20151230 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratAst vikingVarFrameSetInfo VIKINGv20160406 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratAst vikingVarFrameSetInfo VIKINGv20161202 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratAst vikingVarFrameSetInfo VIKINGv20170715 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratAst vmcVarFrameSetInfo VMCDR1 Strateva parameter, b, in fit to astrometric rms vs magnitude in J 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.

jbStratAst vmcVarFrameSetInfo VMCDR2 Strateva parameter, b, in fit to astrometric rms vs magnitude in J 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.

jbStratAst vmcVarFrameSetInfo VMCDR3 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratAst vmcVarFrameSetInfo VMCDR4 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratAst vmcVarFrameSetInfo VMCDR5 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratAst vmcVarFrameSetInfo VMCv20110816 Strateva parameter, b, in fit to astrometric rms vs magnitude in J 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.

jbStratAst vmcVarFrameSetInfo VMCv20110909 Strateva parameter, b, in fit to astrometric rms vs magnitude in J 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.

jbStratAst vmcVarFrameSetInfo VMCv20120126 Strateva parameter, b, in fit to astrometric rms vs magnitude in J 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.

jbStratAst vmcVarFrameSetInfo VMCv20121128 Strateva parameter, b, in fit to astrometric rms vs magnitude in J 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.

jbStratAst vmcVarFrameSetInfo VMCv20130304 Strateva parameter, b, in fit to astrometric rms vs magnitude in J 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.

jbStratAst vmcVarFrameSetInfo VMCv20130805 Strateva parameter, b, in fit to astrometric rms vs magnitude in J 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.

jbStratAst vmcVarFrameSetInfo VMCv20140428 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratAst vmcVarFrameSetInfo VMCv20140903 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratAst vmcVarFrameSetInfo VMCv20150309 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratAst vmcVarFrameSetInfo VMCv20151218 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratAst vmcVarFrameSetInfo VMCv20160311 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratAst vmcVarFrameSetInfo VMCv20160822 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratAst vmcVarFrameSetInfo VMCv20170109 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratAst vmcVarFrameSetInfo VMCv20170411 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratAst vmcVarFrameSetInfo VMCv20171101 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratAst vmcVarFrameSetInfo VMCv20180702 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratAst vmcVarFrameSetInfo VMCv20181120 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratAst vmcVarFrameSetInfo VMCv20191212 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratAst vmcVarFrameSetInfo VMCv20210708 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratAst vmcVarFrameSetInfo VMCv20230816 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratAst vmcVarFrameSetInfo VMCv20240226 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratAst vmcdeepVarFrameSetInfo VMCDEEPv20230713 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratAst vmcdeepVarFrameSetInfo VMCDEEPv20240506 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratAst vvvVarFrameSetInfo VVVDR5 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratAst vvvVarFrameSetInfo VVVv20100531 Strateva parameter, b, in fit to astrometric rms vs magnitude in J 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.

jbStratPht ultravistaMapLcVarFrameSetInfo ULTRAVISTADR4 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratPht ultravistaVarFrameSetInfo ULTRAVISTADR4 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratPht videoVarFrameSetInfo VIDEODR2 Strateva parameter, b, in fit to photometric rms vs magnitude in J 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.

jbStratPht videoVarFrameSetInfo VIDEODR3 Strateva parameter, b, in fit to photometric rms vs magnitude in J 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.

jbStratPht videoVarFrameSetInfo VIDEODR4 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratPht videoVarFrameSetInfo VIDEODR5 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratPht videoVarFrameSetInfo VIDEOv20100513 Strateva parameter, b, in fit to photometric rms vs magnitude in J 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.

jbStratPht videoVarFrameSetInfo VIDEOv20111208 Strateva parameter, b, in fit to photometric rms vs magnitude in J 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.

jbStratPht vikingVarFrameSetInfo VIKINGDR2 Strateva parameter, b, in fit to photometric rms vs magnitude in J 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.

jbStratPht vikingVarFrameSetInfo VIKINGDR3 Strateva parameter, b, in fit to photometric rms vs magnitude in J 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.

jbStratPht vikingVarFrameSetInfo VIKINGDR4 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratPht vikingVarFrameSetInfo VIKINGv20110714 Strateva parameter, b, in fit to photometric rms vs magnitude in J 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.

jbStratPht vikingVarFrameSetInfo VIKINGv20111019 Strateva parameter, b, in fit to photometric rms vs magnitude in J 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.

jbStratPht vikingVarFrameSetInfo VIKINGv20130417 Strateva parameter, b, in fit to photometric rms vs magnitude in J 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.

jbStratPht vikingVarFrameSetInfo VIKINGv20140402 Strateva parameter, b, in fit to photometric rms vs magnitude in J 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.

jbStratPht vikingVarFrameSetInfo VIKINGv20150421 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratPht vikingVarFrameSetInfo VIKINGv20151230 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratPht vikingVarFrameSetInfo VIKINGv20160406 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratPht vikingVarFrameSetInfo VIKINGv20161202 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratPht vikingVarFrameSetInfo VIKINGv20170715 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratPht vmcVarFrameSetInfo VMCDR1 Strateva parameter, b, in fit to photometric rms vs magnitude in J 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.

jbStratPht vmcVarFrameSetInfo VMCDR2 Strateva parameter, b, in fit to photometric rms vs magnitude in J 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.

jbStratPht vmcVarFrameSetInfo VMCDR3 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratPht vmcVarFrameSetInfo VMCDR4 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratPht vmcVarFrameSetInfo VMCDR5 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratPht vmcVarFrameSetInfo VMCv20110816 Strateva parameter, b, in fit to photometric rms vs magnitude in J 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.

jbStratPht vmcVarFrameSetInfo VMCv20110909 Strateva parameter, b, in fit to photometric rms vs magnitude in J 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.

jbStratPht vmcVarFrameSetInfo VMCv20120126 Strateva parameter, b, in fit to photometric rms vs magnitude in J 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.

jbStratPht vmcVarFrameSetInfo VMCv20121128 Strateva parameter, b, in fit to photometric rms vs magnitude in J 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.

jbStratPht vmcVarFrameSetInfo VMCv20130304 Strateva parameter, b, in fit to photometric rms vs magnitude in J 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.

jbStratPht vmcVarFrameSetInfo VMCv20130805 Strateva parameter, b, in fit to photometric rms vs magnitude in J 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.

jbStratPht vmcVarFrameSetInfo VMCv20140428 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratPht vmcVarFrameSetInfo VMCv20140903 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratPht vmcVarFrameSetInfo VMCv20150309 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratPht vmcVarFrameSetInfo VMCv20151218 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratPht vmcVarFrameSetInfo VMCv20160311 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratPht vmcVarFrameSetInfo VMCv20160822 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratPht vmcVarFrameSetInfo VMCv20170109 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratPht vmcVarFrameSetInfo VMCv20170411 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratPht vmcVarFrameSetInfo VMCv20171101 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratPht vmcVarFrameSetInfo VMCv20180702 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratPht vmcVarFrameSetInfo VMCv20181120 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratPht vmcVarFrameSetInfo VMCv20191212 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratPht vmcVarFrameSetInfo VMCv20210708 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratPht vmcVarFrameSetInfo VMCv20230816 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratPht vmcVarFrameSetInfo VMCv20240226 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratPht vmcdeepVarFrameSetInfo VMCDEEPv20230713 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratPht vmcdeepVarFrameSetInfo VMCDEEPv20240506 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratPht vvvVarFrameSetInfo VVVDR5 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. real 4 -0.9999995e9 stat.fit.param;em.IR.J

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.

jbStratPht vvvVarFrameSetInfo VVVv20100531 Strateva parameter, b, in fit to photometric rms vs magnitude in J 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.

jchiSqAst ultravistaVarFrameSetInfo ULTRAVISTADR4 Goodness of fit of Strateva function to astrometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqAst videoVarFrameSetInfo VIDEODR2 Goodness of fit of Strateva function to astrometric data in J 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.

jchiSqAst videoVarFrameSetInfo VIDEODR3 Goodness of fit of Strateva function to astrometric data in J 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.

jchiSqAst videoVarFrameSetInfo VIDEODR4 Goodness of fit of Strateva function to astrometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqAst videoVarFrameSetInfo VIDEODR5 Goodness of fit of Strateva function to astrometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqAst videoVarFrameSetInfo VIDEOv20100513 Goodness of fit of Strateva function to astrometric data in J 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.

jchiSqAst videoVarFrameSetInfo VIDEOv20111208 Goodness of fit of Strateva function to astrometric data in J 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.

jchiSqAst vikingVarFrameSetInfo VIKINGDR2 Goodness of fit of Strateva function to astrometric data in J 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.

jchiSqAst vikingVarFrameSetInfo VIKINGDR3 Goodness of fit of Strateva function to astrometric data in J 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.

jchiSqAst vikingVarFrameSetInfo VIKINGDR4 Goodness of fit of Strateva function to astrometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqAst vikingVarFrameSetInfo VIKINGv20110714 Goodness of fit of Strateva function to astrometric data in J 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.

jchiSqAst vikingVarFrameSetInfo VIKINGv20111019 Goodness of fit of Strateva function to astrometric data in J 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.

jchiSqAst vikingVarFrameSetInfo VIKINGv20130417 Goodness of fit of Strateva function to astrometric data in J 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.

jchiSqAst vikingVarFrameSetInfo VIKINGv20140402 Goodness of fit of Strateva function to astrometric data in J 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.

jchiSqAst vikingVarFrameSetInfo VIKINGv20150421 Goodness of fit of Strateva function to astrometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqAst vikingVarFrameSetInfo VIKINGv20151230 Goodness of fit of Strateva function to astrometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqAst vikingVarFrameSetInfo VIKINGv20160406 Goodness of fit of Strateva function to astrometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqAst vikingVarFrameSetInfo VIKINGv20161202 Goodness of fit of Strateva function to astrometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqAst vikingVarFrameSetInfo VIKINGv20170715 Goodness of fit of Strateva function to astrometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqAst vmcVarFrameSetInfo VMCDR1 Goodness of fit of Strateva function to astrometric data in J 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.

jchiSqAst vmcVarFrameSetInfo VMCDR2 Goodness of fit of Strateva function to astrometric data in J 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.

jchiSqAst vmcVarFrameSetInfo VMCDR3 Goodness of fit of Strateva function to astrometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqAst vmcVarFrameSetInfo VMCDR4 Goodness of fit of Strateva function to astrometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqAst vmcVarFrameSetInfo VMCDR5 Goodness of fit of Strateva function to astrometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqAst vmcVarFrameSetInfo VMCv20110816 Goodness of fit of Strateva function to astrometric data in J 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.

jchiSqAst vmcVarFrameSetInfo VMCv20110909 Goodness of fit of Strateva function to astrometric data in J 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.

jchiSqAst vmcVarFrameSetInfo VMCv20120126 Goodness of fit of Strateva function to astrometric data in J 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.

jchiSqAst vmcVarFrameSetInfo VMCv20121128 Goodness of fit of Strateva function to astrometric data in J 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.

jchiSqAst vmcVarFrameSetInfo VMCv20130304 Goodness of fit of Strateva function to astrometric data in J 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.

jchiSqAst vmcVarFrameSetInfo VMCv20130805 Goodness of fit of Strateva function to astrometric data in J 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.

jchiSqAst vmcVarFrameSetInfo VMCv20140428 Goodness of fit of Strateva function to astrometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqAst vmcVarFrameSetInfo VMCv20140903 Goodness of fit of Strateva function to astrometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqAst vmcVarFrameSetInfo VMCv20150309 Goodness of fit of Strateva function to astrometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqAst vmcVarFrameSetInfo VMCv20151218 Goodness of fit of Strateva function to astrometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqAst vmcVarFrameSetInfo VMCv20160311 Goodness of fit of Strateva function to astrometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqAst vmcVarFrameSetInfo VMCv20160822 Goodness of fit of Strateva function to astrometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqAst vmcVarFrameSetInfo VMCv20170109 Goodness of fit of Strateva function to astrometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqAst vmcVarFrameSetInfo VMCv20170411 Goodness of fit of Strateva function to astrometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqAst vmcVarFrameSetInfo VMCv20171101 Goodness of fit of Strateva function to astrometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqAst vmcVarFrameSetInfo VMCv20180702 Goodness of fit of Strateva function to astrometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqAst vmcVarFrameSetInfo VMCv20181120 Goodness of fit of Strateva function to astrometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqAst vmcVarFrameSetInfo VMCv20191212 Goodness of fit of Strateva function to astrometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqAst vmcVarFrameSetInfo VMCv20210708 Goodness of fit of Strateva function to astrometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqAst vmcVarFrameSetInfo VMCv20230816 Goodness of fit of Strateva function to astrometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqAst vmcVarFrameSetInfo VMCv20240226 Goodness of fit of Strateva function to astrometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqAst vmcdeepVarFrameSetInfo VMCDEEPv20230713 Goodness of fit of Strateva function to astrometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqAst vmcdeepVarFrameSetInfo VMCDEEPv20240506 Goodness of fit of Strateva function to astrometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqAst vvvVarFrameSetInfo VVVDR5 Goodness of fit of Strateva function to astrometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqAst vvvVarFrameSetInfo VVVv20100531 Goodness of fit of Strateva function to astrometric data in J 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.

jchiSqpd 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.

jchiSqpd ultravistaVariability ULTRAVISTADR4 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2;em.IR.J

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.

jchiSqpd 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.

jchiSqpd 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.

jchiSqpd videoVariability VIDEODR4 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2;em.IR.J

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.

jchiSqpd videoVariability VIDEODR5 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2;em.IR.J

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.

jchiSqpd 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.

jchiSqpd 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.

jchiSqpd 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.

jchiSqpd vikingVariability VIKINGDR3 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.

jchiSqpd vikingVariability VIKINGDR4 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2;em.IR.J

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.

jchiSqpd 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.

jchiSqpd 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.

jchiSqpd vikingVariability VIKINGv20130417 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.

jchiSqpd vikingVariability VIKINGv20140402 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.

jchiSqpd vikingVariability VIKINGv20150421 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2;em.IR.J

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.

jchiSqpd vikingVariability VIKINGv20151230 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2;em.IR.J

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.

jchiSqpd vikingVariability VIKINGv20160406 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2;em.IR.J

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.

jchiSqpd vikingVariability VIKINGv20161202 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2;em.IR.J

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.

jchiSqpd vikingVariability VIKINGv20170715 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2;em.IR.J

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.

jchiSqpd vmcVariability VMCDR1 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.

jchiSqpd vmcVariability VMCDR2 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.

jchiSqpd vmcVariability VMCDR3 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2;em.IR.J

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.

jchiSqpd vmcVariability VMCDR4 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2;em.IR.J

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.

jchiSqpd vmcVariability VMCDR5 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2;em.IR.J

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.

jchiSqpd vmcVariability VMCv20110816 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.

jchiSqpd vmcVariability VMCv20110909 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.

jchiSqpd vmcVariability VMCv20120126 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.

jchiSqpd vmcVariability VMCv20121128 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.

jchiSqpd vmcVariability VMCv20130304 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.

jchiSqpd vmcVariability VMCv20130805 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.

jchiSqpd vmcVariability VMCv20140428 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2;em.IR.J

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.

jchiSqpd vmcVariability VMCv20140903 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2;em.IR.J

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.

jchiSqpd vmcVariability VMCv20150309 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2;em.IR.J

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.

jchiSqpd vmcVariability VMCv20151218 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2;em.IR.J

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.

jchiSqpd vmcVariability VMCv20160311 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2;em.IR.J

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.

jchiSqpd vmcVariability VMCv20160822 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2;em.IR.J

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.

jchiSqpd vmcVariability VMCv20170109 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2;em.IR.J

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.

jchiSqpd vmcVariability VMCv20170411 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2;em.IR.J

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.

jchiSqpd vmcVariability VMCv20171101 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2;em.IR.J

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.

jchiSqpd vmcVariability VMCv20180702 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2;em.IR.J

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.

jchiSqpd vmcVariability VMCv20181120 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2;em.IR.J

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.

jchiSqpd vmcVariability VMCv20191212 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2;em.IR.J

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.

jchiSqpd vmcVariability VMCv20210708 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2;em.IR.J

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.

jchiSqpd vmcVariability VMCv20230816 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2;em.IR.J

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.

jchiSqpd vmcVariability VMCv20240226 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2;em.IR.J

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.

jchiSqpd vmcdeepVariability VMCDEEPv20230713 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2;em.IR.J

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.

jchiSqpd vmcdeepVariability VMCDEEPv20240506 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2;em.IR.J

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.

jchiSqpd vvvVariability VVVDR5 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9 stat.fit.chi2;em.IR.J

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.

jchiSqpd 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.

jchiSqPht ultravistaMapLcVarFrameSetInfo, ultravistaVarFrameSetInfo ULTRAVISTADR4 Goodness of fit of Strateva function to photometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqPht videoVarFrameSetInfo VIDEODR2 Goodness of fit of Strateva function to photometric data in J 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.

jchiSqPht videoVarFrameSetInfo VIDEODR3 Goodness of fit of Strateva function to photometric data in J 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.

jchiSqPht videoVarFrameSetInfo VIDEODR4 Goodness of fit of Strateva function to photometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqPht videoVarFrameSetInfo VIDEODR5 Goodness of fit of Strateva function to photometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqPht videoVarFrameSetInfo VIDEOv20100513 Goodness of fit of Strateva function to photometric data in J 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.

jchiSqPht videoVarFrameSetInfo VIDEOv20111208 Goodness of fit of Strateva function to photometric data in J 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.

jchiSqPht vikingVarFrameSetInfo VIKINGDR2 Goodness of fit of Strateva function to photometric data in J 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.

jchiSqPht vikingVarFrameSetInfo VIKINGDR3 Goodness of fit of Strateva function to photometric data in J 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.

jchiSqPht vikingVarFrameSetInfo VIKINGDR4 Goodness of fit of Strateva function to photometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqPht vikingVarFrameSetInfo VIKINGv20110714 Goodness of fit of Strateva function to photometric data in J 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.

jchiSqPht vikingVarFrameSetInfo VIKINGv20111019 Goodness of fit of Strateva function to photometric data in J 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.

jchiSqPht vikingVarFrameSetInfo VIKINGv20130417 Goodness of fit of Strateva function to photometric data in J 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.

jchiSqPht vikingVarFrameSetInfo VIKINGv20140402 Goodness of fit of Strateva function to photometric data in J 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.

jchiSqPht vikingVarFrameSetInfo VIKINGv20150421 Goodness of fit of Strateva function to photometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqPht vikingVarFrameSetInfo VIKINGv20151230 Goodness of fit of Strateva function to photometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqPht vikingVarFrameSetInfo VIKINGv20160406 Goodness of fit of Strateva function to photometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqPht vikingVarFrameSetInfo VIKINGv20161202 Goodness of fit of Strateva function to photometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqPht vikingVarFrameSetInfo VIKINGv20170715 Goodness of fit of Strateva function to photometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqPht vmcVarFrameSetInfo VMCDR1 Goodness of fit of Strateva function to photometric data in J 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.

jchiSqPht vmcVarFrameSetInfo VMCDR2 Goodness of fit of Strateva function to photometric data in J 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.

jchiSqPht vmcVarFrameSetInfo VMCDR3 Goodness of fit of Strateva function to photometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqPht vmcVarFrameSetInfo VMCDR4 Goodness of fit of Strateva function to photometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqPht vmcVarFrameSetInfo VMCDR5 Goodness of fit of Strateva function to photometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqPht vmcVarFrameSetInfo VMCv20110816 Goodness of fit of Strateva function to photometric data in J 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.

jchiSqPht vmcVarFrameSetInfo VMCv20110909 Goodness of fit of Strateva function to photometric data in J 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.

jchiSqPht vmcVarFrameSetInfo VMCv20120126 Goodness of fit of Strateva function to photometric data in J 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.

jchiSqPht vmcVarFrameSetInfo VMCv20121128 Goodness of fit of Strateva function to photometric data in J 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.

jchiSqPht vmcVarFrameSetInfo VMCv20130304 Goodness of fit of Strateva function to photometric data in J 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.

jchiSqPht vmcVarFrameSetInfo VMCv20130805 Goodness of fit of Strateva function to photometric data in J 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.

jchiSqPht vmcVarFrameSetInfo VMCv20140428 Goodness of fit of Strateva function to photometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqPht vmcVarFrameSetInfo VMCv20140903 Goodness of fit of Strateva function to photometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqPht vmcVarFrameSetInfo VMCv20150309 Goodness of fit of Strateva function to photometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqPht vmcVarFrameSetInfo VMCv20151218 Goodness of fit of Strateva function to photometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqPht vmcVarFrameSetInfo VMCv20160311 Goodness of fit of Strateva function to photometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqPht vmcVarFrameSetInfo VMCv20160822 Goodness of fit of Strateva function to photometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqPht vmcVarFrameSetInfo VMCv20170109 Goodness of fit of Strateva function to photometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqPht vmcVarFrameSetInfo VMCv20170411 Goodness of fit of Strateva function to photometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqPht vmcVarFrameSetInfo VMCv20171101 Goodness of fit of Strateva function to photometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqPht vmcVarFrameSetInfo VMCv20180702 Goodness of fit of Strateva function to photometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqPht vmcVarFrameSetInfo VMCv20181120 Goodness of fit of Strateva function to photometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqPht vmcVarFrameSetInfo VMCv20191212 Goodness of fit of Strateva function to photometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqPht vmcVarFrameSetInfo VMCv20210708 Goodness of fit of Strateva function to photometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqPht vmcVarFrameSetInfo VMCv20230816 Goodness of fit of Strateva function to photometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqPht vmcVarFrameSetInfo VMCv20240226 Goodness of fit of Strateva function to photometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqPht vmcdeepVarFrameSetInfo VMCDEEPv20230713 Goodness of fit of Strateva function to photometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqPht vmcdeepVarFrameSetInfo VMCDEEPv20240506 Goodness of fit of Strateva function to photometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqPht vvvVarFrameSetInfo VVVDR5 Goodness of fit of Strateva function to photometric data in J band real 4 -0.9999995e9 stat.fit.goodness;em.IR.J

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.

jchiSqPht vvvVarFrameSetInfo VVVv20100531 Goodness of fit of Strateva function to photometric data in J 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.

Jclass vvvParallaxCatalogue, vvvProperMotionCatalogue VVVDR5 VVV DR4 J 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: Jclass} int 4 -99999999

jClass ultravistaSource ULTRAVISTADR4 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass ultravistaSourceRemeasurement ULTRAVISTADR4 discrete image classification flag in J smallint 2 -9999 src.class

jClass vhsSource VHSDR2 discrete image classification flag in J smallint 2 -9999 src.class

jClass vhsSource VHSDR3 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vhsSource VHSDR4 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vhsSource VHSDR5 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vhsSource VHSDR6 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vhsSource VHSv20120926 discrete image classification flag in J smallint 2 -9999 src.class

jClass vhsSource VHSv20130417 discrete image classification flag in J smallint 2 -9999 src.class

jClass vhsSource VHSv20140409 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vhsSource VHSv20150108 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vhsSource VHSv20160114 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vhsSource VHSv20160507 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vhsSource VHSv20170630 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vhsSource VHSv20180419 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vhsSource VHSv20201209 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vhsSource VHSv20231101 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vhsSource VHSv20240731 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vhsSource, vhsSourceRemeasurement VHSDR1 discrete image classification flag in J smallint 2 -9999 src.class

jClass videoSource VIDEODR2 discrete image classification flag in J smallint 2 -9999 src.class

jClass videoSource VIDEODR3 discrete image classification flag in J smallint 2 -9999 src.class

jClass videoSource VIDEODR4 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass videoSource VIDEODR5 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass videoSource VIDEOv20111208 discrete image classification flag in J smallint 2 -9999 src.class

jClass videoSource, videoSourceRemeasurement VIDEOv20100513 discrete image classification flag in J smallint 2 -9999 src.class

jClass vikingSource VIKINGDR2 discrete image classification flag in J smallint 2 -9999 src.class

jClass vikingSource VIKINGDR3 discrete image classification flag in J smallint 2 -9999 src.class

jClass vikingSource VIKINGDR4 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vikingSource VIKINGv20111019 discrete image classification flag in J smallint 2 -9999 src.class

jClass vikingSource VIKINGv20130417 discrete image classification flag in J smallint 2 -9999 src.class

jClass vikingSource VIKINGv20140402 discrete image classification flag in J smallint 2 -9999 src.class

jClass vikingSource VIKINGv20150421 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vikingSource VIKINGv20151230 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vikingSource VIKINGv20160406 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vikingSource VIKINGv20161202 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vikingSource VIKINGv20170715 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vikingSource, vikingSourceRemeasurement VIKINGv20110714 discrete image classification flag in J smallint 2 -9999 src.class

jClass vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 discrete image classification flag in J smallint 2 -9999 src.class

jClass vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 discrete image classification flag in J smallint 2 -9999 src.class

jClass vmcSource VMCDR2 discrete image classification flag in J smallint 2 -9999 src.class

jClass vmcSource VMCDR3 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vmcSource VMCDR4 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vmcSource VMCDR5 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vmcSource VMCv20110909 discrete image classification flag in J smallint 2 -9999 src.class

jClass vmcSource VMCv20120126 discrete image classification flag in J smallint 2 -9999 src.class

jClass vmcSource VMCv20121128 discrete image classification flag in J smallint 2 -9999 src.class

jClass vmcSource VMCv20130304 discrete image classification flag in J smallint 2 -9999 src.class

jClass vmcSource VMCv20130805 discrete image classification flag in J smallint 2 -9999 src.class

jClass vmcSource VMCv20140428 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vmcSource VMCv20140903 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vmcSource VMCv20150309 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vmcSource VMCv20151218 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vmcSource VMCv20160311 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vmcSource VMCv20160822 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vmcSource VMCv20170109 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vmcSource VMCv20170411 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vmcSource VMCv20171101 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vmcSource VMCv20180702 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vmcSource VMCv20181120 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vmcSource VMCv20191212 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vmcSource VMCv20210708 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vmcSource VMCv20230816 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vmcSource VMCv20240226 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vmcSource, vmcSourceRemeasurement VMCv20110816 discrete image classification flag in J smallint 2 -9999 src.class

jClass vmcSource, vmcSynopticSource VMCDR1 discrete image classification flag in J smallint 2 -9999 src.class

jClass vmcdeepSource VMCDEEPv20240506 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vmcdeepSource, vmcdeepSynopticSource VMCDEEPv20230713 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vvvSource VVVDR2 discrete image classification flag in J smallint 2 -9999 src.class

jClass vvvSource VVVDR5 discrete image classification flag in J smallint 2 -9999 src.class;em.IR.J

jClass vvvSource VVVv20110718 discrete image classification flag in J smallint 2 -9999 src.class

jClass vvvSource, vvvSourceRemeasurement VVVv20100531 discrete image classification flag in J smallint 2 -9999 src.class

jClass vvvSource, vvvSynopticSource VVVDR1 discrete image classification flag in J smallint 2 -9999 src.class

jClassStat ultravistaSource ULTRAVISTADR4 S-Extractor classification statistic in J real 4 -0.9999995e9 stat;em.IR.J

jClassStat ultravistaSourceRemeasurement ULTRAVISTADR4 N(0,1) stellarness-of-profile statistic in J real 4 -0.9999995e9 stat

jClassStat vhsSource VHSDR2 N(0,1) stellarness-of-profile statistic in J real 4 -0.9999995e9 stat

jClassStat vhsSource VHSDR3 N(0,1) stellarness-of-profile statistic in J real 4 -0.9999995e9 stat;em.IR.J

jClassStat vhsSource VHSDR4 N(0,1) stellarness-of-profile statistic in J real 4 -0.9999995e9 stat;em.IR.J

jClassStat vhsSource VHSDR5 N(0,1) stellarness-of-profile statistic in J real 4 -0.9999995e9 stat;em.IR.J

jClassStat vhsSource VHSDR6 N(0,1) stellarness-of-profile statistic in J real 4 -0.9999995e9 stat;em.IR.J

jClassStat vhsSource VHSv20120926 N(0,1) stellarness-of-profile statistic in J real 4 -0.9999995e9 stat

jClassStat vhsSource VHSv20130417 N(0,1) stellarness-of-profile statistic in J real 4 -0.9999995e9 stat

jClassStat vhsSource VHSv20140409 N(0,1) stellarness-of-profile statistic in J real 4 -0.9999995e9 stat;em.IR.J

jClassStat vhsSource VHSv20150108 N(0,1) stellarness-of-profile statistic in J real 4 -0.9999995e9 stat;em.IR.J

jClassStat vhsSource VHSv20160114 N(0,1) stellarness-of-profile statistic in J real 4 -0.9999995e9 stat;em.IR.J

jClassStat vhsSource VHSv20160507 N(0,1) stellarness-of-profile statistic in J real 4 -0.9999995e9 stat;em.IR.J

jClassStat vhsSource VHSv20170630 N(0,1) stellarness-of-profile statistic in J real 4 -0.9999995e9 stat;em.IR.J

jClassStat vhsSource VHSv20180419 N(0,1) stellarness-of-profile statistic in J real 4 -0.9999995e9 stat;em.IR.J

jClassStat vhsSource VHSv20201209 N(0,1) stellarness-of-profile statistic in J real 4 -0.9999995e9 stat;em.IR.J

jClassStat vhsSource VHSv20231101 N(0,1) stellarness-of-profile statistic in J real 4 -0.9999995e9 stat;em.IR.J

jClassStat vhsSource VHSv20240731 N(0,1) stellarness-of-profile statistic in J real 4 -0.9999995e9 stat;em.IR.J

jClassStat vhsSource, vhsSourceRemeasurement VHSDR1 N(0,1) stellarness-of-profile statistic in J real 4 -0.9999995e9 stat

jClassStat videoSource VIDEODR2 S-Extractor classification statistic in J real 4 -0.9999995e9 stat

jClassStat videoSource VIDEODR3 S-Extractor classification statistic in J real 4 -0.9999995e9 stat

jClassStat videoSource VIDEODR4 S-Extractor classification statistic in J real 4 -0.9999995e9 stat;em.IR.J

jClassStat videoSource VIDEODR5 S-Extractor classification statistic in J real 4 -0.9999995e9 stat;em.IR.J

jClassStat videoSource VIDEOv20100513 S-Extractor classification statistic in J real 4 -0.9999995e9 stat

jClassStat videoSource VIDEOv20111208 S-Extractor classification statistic in J real 4 -0.9999995e9 stat

jClassStat videoSourceRemeasurement VIDEOv20100513 N(0,1) stellarness-of-profile statistic in J real 4 -0.9999995e9 stat

jClassStat vikingSource VIKINGDR2 N(0,1) stellarness-of-profile statistic in J real 4 -0.9999995e9 stat

jClassStat vikingSource VIKINGDR3 N(0,1) stellarness-of-profile statistic in J real 4 -0.9999995e9 stat

jClassStat viking