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Glossary of VSA attributes
This Glossary alphabetically lists all attributes used in the VSAv20240329 database(s) held in the VSA. If you would like to have more information about the schema tables please use the VSAv20240329 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

Z
Name	Schema Table	Database	Description	Type	Length	Unit	Default Value	Unified Content Descriptor
Z	spectra	SIXDF	raw measured redshift	real	4
z	allwise_sc	WISE	Unit sphere position z value	float	8
z_1AperMag1	vvvSource	VVVDR5	Point source Z_1 aperture corrected mag (1.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
z_1AperMag1Err	vvvSource	VVVDR5	Error in point source Z_1 mag (1.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.I
z_1AperMag3	vvvSource	VVVDR5	Default point source Z_1 aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
z_1AperMag3Err	vvvSource	VVVDR5	Error in default point source Z_1 mag (2.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.I
z_1AperMag4	vvvSource	VVVDR5	Point source Z_1 aperture corrected mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
z_1AperMag4Err	vvvSource	VVVDR5	Error in point source Z_1 mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.I
z_1AverageConf	vvvSource	VVVDR5	average confidence in 2 arcsec diameter default aperture (aper3) Z_1	real	4		-0.9999995e9	stat.likelihood;em.opt.I
z_1Class	vvvSource	VVVDR5	discrete image classification flag in Z_1	smallint	2		-9999	src.class;em.opt.I
z_1ClassStat	vvvSource	VVVDR5	S-Extractor classification statistic in Z_1	real	4		-0.9999995e9	stat;em.opt.I
z_1Ell	vvvSource	VVVDR5	1-b/a, where a/b=semi-major/minor axes in Z_1	real	4		-0.9999995e9	src.ellipticity;em.opt.I
z_1eNum	vvvMergeLog	VVVDR5	the extension number of this Z_1 frame	tinyint	1			meta.number;em.opt.I
z_1eNum	vvvPsfDophotZYJHKsMergeLog	VVVDR5	the extension number of this 1st epoch Z frame	tinyint	1			meta.number;em.opt.I
z_1ErrBits	vvvSource	VVVDR5	processing warning/error bitwise flags in Z_1	int	4		-99999999	meta.code;em.opt.I
			Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
z_1Eta	vvvSource	VVVDR5	Offset of Z_1 detection from master position (+north/-south)	real	4	arcsec	-0.9999995e9	pos.eq.dec;arith.diff;em.opt.I
			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.
z_1Gausig	vvvSource	VVVDR5	RMS of axes of ellipse fit in Z_1	real	4	pixels	-0.9999995e9	src.morph.param;em.opt.I
z_1mfID	vvvMergeLog	VVVDR5	the UID of the relevant Z_1 multiframe	bigint	8			meta.id;obs.field;em.opt.I
z_1mfID	vvvPsfDophotZYJHKsMergeLog	VVVDR5	the UID of the relevant 1st epoch Z tile multiframe	bigint	8			meta.id;obs.field;em.opt.I
z_1Mjd	vvvPsfDophotZYJHKsMergeLog	VVVDR5	the MJD of the 1st epoch Z tile multiframe	float	8			time;em.opt.I
z_1Mjd	vvvSource	VVVDR5	Modified Julian Day in Z_1 band	float	8	days	-0.9999995e9	time.epoch;em.opt.I
z_1my_1Pnt	vvvSource	VVVDR5	Point source colour Z_1-Y_1 (using aperMag3)	real	4	mag	-0.9999995e9	phot.color;em.opt.I;em.IR.NIR
			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.
z_1my_1PntErr	vvvSource	VVVDR5	Error on point source colour Z_1-Y_1	real	4	mag	-0.9999995e9	stat.error;em.opt.I;em.IR.NIR
			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.
z_1PA	vvvSource	VVVDR5	ellipse fit celestial orientation in Z_1	real	4	Degrees	-0.9999995e9	pos.posAng;em.opt.I
z_1ppErrBits	vvvSource	VVVDR5	additional WFAU post-processing error bits in Z_1	int	4		0	meta.code;em.opt.I
z_1SeqNum	vvvSource	VVVDR5	the running number of the Z_1 detection	int	4		-99999999	meta.number;em.opt.I
z_1Xi	vvvSource	VVVDR5	Offset of Z_1 detection from master position (+east/-west)	real	4	arcsec	-0.9999995e9	pos.eq.ra;arith.diff;em.opt.I
			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.
z_2AperMag1	vvvSource	VVVDR5	Point source Z_2 aperture corrected mag (1.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
z_2AperMag1Err	vvvSource	VVVDR5	Error in point source Z_2 mag (1.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.I
z_2AperMag3	vvvSource	VVVDR5	Default point source Z_2 aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
z_2AperMag3Err	vvvSource	VVVDR5	Error in default point source Z_2 mag (2.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.I
z_2AperMag4	vvvSource	VVVDR5	Point source Z_2 aperture corrected mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
z_2AperMag4Err	vvvSource	VVVDR5	Error in point source Z_2 mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.I
z_2AverageConf	vvvSource	VVVDR5	average confidence in 2 arcsec diameter default aperture (aper3) Z_2	real	4		-0.9999995e9	stat.likelihood;em.opt.I
z_2Class	vvvSource	VVVDR5	discrete image classification flag in Z_2	smallint	2		-9999	src.class;em.opt.I
z_2ClassStat	vvvSource	VVVDR5	S-Extractor classification statistic in Z_2	real	4		-0.9999995e9	stat;em.opt.I
z_2Ell	vvvSource	VVVDR5	1-b/a, where a/b=semi-major/minor axes in Z_2	real	4		-0.9999995e9	src.ellipticity;em.opt.I
z_2eNum	vvvMergeLog	VVVDR5	the extension number of this Z_2 frame	tinyint	1			meta.number;em.opt.I
z_2eNum	vvvPsfDophotZYJHKsMergeLog	VVVDR5	the extension number of this 2nd epoch Z frame	tinyint	1			meta.number;em.opt.I
z_2ErrBits	vvvSource	VVVDR5	processing warning/error bitwise flags in Z_2	int	4		-99999999	meta.code;em.opt.I
			Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
z_2Eta	vvvSource	VVVDR5	Offset of Z_2 detection from master position (+north/-south)	real	4	arcsec	-0.9999995e9	pos.eq.dec;arith.diff;em.opt.I
			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.
z_2Gausig	vvvSource	VVVDR5	RMS of axes of ellipse fit in Z_2	real	4	pixels	-0.9999995e9	src.morph.param;em.opt.I
z_2mfID	vvvMergeLog	VVVDR5	the UID of the relevant Z_2 multiframe	bigint	8			meta.id;obs.field;em.opt.I
z_2mfID	vvvPsfDophotZYJHKsMergeLog	VVVDR5	the UID of the relevant 2nd epoch Z tile multiframe	bigint	8			meta.id;obs.field;em.opt.I
z_2Mjd	vvvPsfDophotZYJHKsMergeLog	VVVDR5	the MJD of the 2nd epoch Z tile multiframe	float	8			time;em.opt.I
z_2Mjd	vvvSource	VVVDR5	Modified Julian Day in Z_2 band	float	8	days	-0.9999995e9	time.epoch;em.opt.I
z_2my_2Pnt	vvvSource	VVVDR5	Point source colour Z_2-Y_2 (using aperMag3)	real	4	mag	-0.9999995e9	phot.color;em.opt.I;em.IR.NIR
			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.
z_2my_2PntErr	vvvSource	VVVDR5	Error on point source colour Z_2-Y_2	real	4	mag	-0.9999995e9	stat.error;em.opt.I;em.IR.NIR
			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.
z_2PA	vvvSource	VVVDR5	ellipse fit celestial orientation in Z_2	real	4	Degrees	-0.9999995e9	pos.posAng;em.opt.I
z_2ppErrBits	vvvSource	VVVDR5	additional WFAU post-processing error bits in Z_2	int	4		0	meta.code;em.opt.I
z_2SeqNum	vvvSource	VVVDR5	the running number of the Z_2 detection	int	4		-99999999	meta.number;em.opt.I
z_2Xi	vvvSource	VVVDR5	Offset of Z_2 detection from master position (+east/-west)	real	4	arcsec	-0.9999995e9	pos.eq.ra;arith.diff;em.opt.I
			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.
Z_ABS	spectra	SIXDF	cross-correlation redshift	real	4
Z_COMM	spectra	SIXDF	observer's comment	varchar	29
Z_EMI	spectra	SIXDF	emission redshift	real	4
z_flags	masterDR2	SKYMAPPER	Bitwise OR of Source Extractor flags from z-band measurements in photometry table	smallint	2			meta.code
Z_HELIO	spectra	SIXDF	heliocentric redshift	real	4
z_nch	masterDR2	SKYMAPPER	Number of z-band child sources combined into this object_id	smallint	2			meta.number
z_nclip	masterDR2	SKYMAPPER	Number of z-band observations with magnitudes clipped from the final PSF magnitude estimate	smallint	2			meta.number
z_ngood	masterDR2	SKYMAPPER	Number of z-band observations used	smallint	2			meta.number
z_nimaflags	masterDR2	SKYMAPPER	Number of flagged pixels from bad, saturated, and crosstalk pixel masks from z-band measurements in photometry table	int	4			meta.code
Z_ORIGIN	spectra	SIXDF	redshift from C=combined V or R frame	char	1
z_petro	masterDR2	SKYMAPPER	Mean z-band Petrosian magnitude	real	4	mag		phot.mag;stat.mean
z_psf	masterDR2	SKYMAPPER	Mean z-band PSF magnitude	real	4	mag		phot.mag;stat.mean
z_rchi2var	masterDR2	SKYMAPPER	Reduced chi-squared for a constant-magnitude model of the z-band PSF magnitude, including clipped sources	real	4			stat.fit.chi2
ZABSBESTERR	spectra	SIXDF	error on the selected absorption line redshift, 0.0 if not measured	real	4
zAperJky3	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Default point source Z aperture corrected (2.0 arcsec aperture diameter) calibrated flux If in doubt use this flux estimator	real	4	jansky	-0.9999995e9	phot.flux
zAperJky3	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Default point source Z aperture corrected (2.0 arcsec aperture diameter) calibrated flux If in doubt use this flux estimator	real	4	jansky	-0.9999995e9	phot.flux
zAperJky3Err	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Error in default point/extended source Z (2.0 arcsec aperture diameter) calibrated flux	real	4	jansky	-0.9999995e9	stat.error
zAperJky3Err	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Error in default point/extended source Z (2.0 arcsec aperture diameter) calibrated flux	real	4	jansky	-0.9999995e9	stat.error
zAperJky4	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Point source Z aperture corrected (2.8 arcsec aperture diameter) calibrated flux	real	4	jansky	-0.9999995e9	phot.flux
zAperJky4	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Point source Z aperture corrected (2.8 arcsec aperture diameter) calibrated flux	real	4	jansky	-0.9999995e9	phot.flux
zAperJky4Err	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Error in point/extended source Z (2.8 arcsec aperture diameter) calibrated flux	real	4	jansky	-0.9999995e9	stat.error
zAperJky4Err	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Error in point/extended source Z (2.8 arcsec aperture diameter) calibrated flux	real	4	jansky	-0.9999995e9	stat.error
zAperJky6	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Point source Z aperture corrected (5.7 arcsec aperture diameter) calibrated flux	real	4	jansky	-0.9999995e9	phot.flux
zAperJky6	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Point source Z aperture corrected (5.7 arcsec aperture diameter) calibrated flux	real	4	jansky	-0.9999995e9	phot.flux
zAperJky6Err	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Error in point/extended source Z (5.7 arcsec aperture diameter) calibrated flux	real	4	jansky	-0.9999995e9	stat.error
zAperJky6Err	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Error in point/extended source Z (5.7 arcsec aperture diameter) calibrated flux	real	4	jansky	-0.9999995e9	stat.error
zAperJkyNoAperCorr3	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Default extended source Z (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
zAperJkyNoAperCorr3	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Default extended source Z (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
zAperJkyNoAperCorr4	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Extended source Z (2.8 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux	real	4	jansky	-0.9999995e9	phot.flux
zAperJkyNoAperCorr4	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Extended source Z (2.8 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux	real	4	jansky	-0.9999995e9	phot.flux
zAperJkyNoAperCorr6	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Extended source Z (5.7 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux	real	4	jansky	-0.9999995e9	phot.flux
zAperJkyNoAperCorr6	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Extended source Z (5.7 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux	real	4	jansky	-0.9999995e9	phot.flux
zAperLup3	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Default point source Z aperture corrected (2.0 arcsec aperture diameter) luptitude If in doubt use this flux estimator	real	4	lup	-0.9999995e9	phot.lup
zAperLup3	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Default point source Z aperture corrected (2.0 arcsec aperture diameter) luptitude If in doubt use this flux estimator	real	4	lup	-0.9999995e9	phot.lup
zAperLup3Err	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Error in default point/extended source Z (2.0 arcsec aperture diameter) luptitude	real	4	lup	-0.9999995e9	stat.error
zAperLup3Err	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Error in default point/extended source Z (2.0 arcsec aperture diameter) luptitude	real	4	lup	-0.9999995e9	stat.error
zAperLup4	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Point source Z aperture corrected (2.8 arcsec aperture diameter) luptitude	real	4	lup	-0.9999995e9	phot.lup
zAperLup4	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Point source Z aperture corrected (2.8 arcsec aperture diameter) luptitude	real	4	lup	-0.9999995e9	phot.lup
zAperLup4Err	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Error in point/extended source Z (2.8 arcsec aperture diameter) luptitude	real	4	lup	-0.9999995e9	stat.error
zAperLup4Err	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Error in point/extended source Z (2.8 arcsec aperture diameter) luptitude	real	4	lup	-0.9999995e9	stat.error
zAperLup6	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Point source Z aperture corrected (5.7 arcsec aperture diameter) luptitude	real	4	lup	-0.9999995e9	phot.lup
zAperLup6	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Point source Z aperture corrected (5.7 arcsec aperture diameter) luptitude	real	4	lup	-0.9999995e9	phot.lup
zAperLup6Err	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Error in point/extended source Z (5.7 arcsec aperture diameter) luptitude	real	4	lup	-0.9999995e9	stat.error
zAperLup6Err	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Error in point/extended source Z (5.7 arcsec aperture diameter) luptitude	real	4	lup	-0.9999995e9	stat.error
zAperLupNoAperCorr3	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Default extended source Z (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
zAperLupNoAperCorr3	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Default extended source Z (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
zAperLupNoAperCorr4	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Extended source Z (2.8 arcsec aperture diameter, but no aperture correction applied) aperture luptitude	real	4	lup	-0.9999995e9	phot.lup
zAperLupNoAperCorr4	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Extended source Z (2.8 arcsec aperture diameter, but no aperture correction applied) aperture luptitude	real	4	lup	-0.9999995e9	phot.lup
zAperLupNoAperCorr6	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Extended source Z (5.7 arcsec aperture diameter, but no aperture correction applied) aperture luptitude	real	4	lup	-0.9999995e9	phot.lup
zAperLupNoAperCorr6	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Extended source Z (5.7 arcsec aperture diameter, but no aperture correction applied) aperture luptitude	real	4	lup	-0.9999995e9	phot.lup
zAperMag1	vvvSource	VVVDR1	Extended source Z aperture corrected mag (0.7 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag
zAperMag1	vvvSource	VVVDR5	Point source Z aperture corrected mag (1.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag1	vvvSource	VVVv20100531	Extended source Z aperture corrected mag (0.7 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag
zAperMag1	vvvSource	VVVv20110718	Extended source Z aperture corrected mag (0.7 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag
zAperMag1	vvvSource, vvvSynopticSource	VVVDR2	Extended source Z aperture corrected mag (1.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag1Err	vvvSource	VVVDR1	Error in extended source Z mag (1.4 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag1Err	vvvSource	VVVDR5	Error in point source Z mag (1.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.I
zAperMag1Err	vvvSource	VVVv20100531	Error in extended source Z mag (1.4 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag1Err	vvvSource	VVVv20110718	Error in extended source Z mag (1.4 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag1Err	vvvSource, vvvSynopticSource	VVVDR2	Error in extended source Z mag (1.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag2	vvvSynopticSource	VVVDR1	Extended source Z aperture corrected mag (1.4 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMag2	vvvSynopticSource	VVVDR2	Extended source Z aperture corrected mag (1.4 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag2Err	vvvSynopticSource	VVVDR1	Error in extended source Z mag (1.4 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag2Err	vvvSynopticSource	VVVDR2	Error in extended source Z mag (1.4 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag3	videoSource	VIDEODR2	Default point source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag
zAperMag3	videoSource	VIDEODR3	Default point source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag
zAperMag3	videoSource	VIDEODR4	Default point source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag3	videoSource	VIDEODR5	Default point source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag3	videoSource	VIDEOv20100513	Default point/extended source Z mag, no aperture correction applied If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag
zAperMag3	videoSource	VIDEOv20111208	Default point source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag
zAperMag3	vikingSource	VIKINGDR2	Default point source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag
zAperMag3	vikingSource	VIKINGDR3	Default point source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag
zAperMag3	vikingSource	VIKINGDR4	Default point source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag3	vikingSource	VIKINGv20110714	Default point source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag
zAperMag3	vikingSource	VIKINGv20111019	Default point source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag
zAperMag3	vikingSource	VIKINGv20130417	Default point source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag
zAperMag3	vikingSource	VIKINGv20140402	Default point source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag3	vikingSource	VIKINGv20150421	Default point source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag3	vikingSource	VIKINGv20151230	Default point source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag3	vikingSource	VIKINGv20160406	Default point source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag3	vikingSource	VIKINGv20161202	Default point source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag3	vikingSource	VIKINGv20170715	Default point source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag3	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Default point source Z aperture corrected (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag
zAperMag3	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Default point source Z aperture corrected (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag
zAperMag3	vvvSource	VVVDR1	Default point/extended source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag
zAperMag3	vvvSource	VVVDR2	Default point/extended source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag3	vvvSource	VVVDR5	Default point source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag3	vvvSource	VVVv20100531	Default point/extended source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag
zAperMag3	vvvSource	VVVv20110718	Default point/extended source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag
zAperMag3	vvvSynopticSource	VVVDR1	Default point/extended source Z aperture corrected mag (2.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMag3	vvvSynopticSource	VVVDR2	Default point/extended source Z aperture corrected mag (2.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag3	vvvVivaCatalogue	VVVDR5	Z magnitude using aperture corrected mag (2.0 arcsec aperture diameter, from VVVDR4 1st epoch ZY contemporaneous OB) {catalogue TType keyword: zAperMag3}	real	4	mag	-9.999995e8
zAperMag3Err	videoSource	VIDEODR2	Error in default point/extended source Z mag (2.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag3Err	videoSource	VIDEODR3	Error in default point/extended source Z mag (2.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag3Err	videoSource	VIDEODR4	Error in default point/extended source Z mag (2.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error;em.opt.I;phot.mag
zAperMag3Err	videoSource	VIDEODR5	Error in default point/extended source Z mag (2.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error;em.opt.I;phot.mag
zAperMag3Err	videoSource	VIDEOv20100513	Error in default point/extended source Z mag (2.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag3Err	videoSource	VIDEOv20111208	Error in default point/extended source Z mag (2.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag3Err	vikingSource	VIKINGDR2	Error in default point/extended source Z mag (2.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag3Err	vikingSource	VIKINGDR3	Error in default point/extended source Z mag (2.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag3Err	vikingSource	VIKINGDR4	Error in default point/extended source Z mag (2.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error;em.opt.I
zAperMag3Err	vikingSource	VIKINGv20110714	Error in default point/extended source Z mag (2.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag3Err	vikingSource	VIKINGv20111019	Error in default point/extended source Z mag (2.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag3Err	vikingSource	VIKINGv20130417	Error in default point/extended source Z mag (2.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag3Err	vikingSource	VIKINGv20140402	Error in default point/extended source Z mag (2.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag3Err	vikingSource	VIKINGv20150421	Error in default point/extended source Z mag (2.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error;em.opt.I;phot.mag
zAperMag3Err	vikingSource	VIKINGv20151230	Error in default point/extended source Z mag (2.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.I
zAperMag3Err	vikingSource	VIKINGv20160406	Error in default point/extended source Z mag (2.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.I
zAperMag3Err	vikingSource	VIKINGv20161202	Error in default point/extended source Z mag (2.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.I
zAperMag3Err	vikingSource	VIKINGv20170715	Error in default point/extended source Z mag (2.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.I
zAperMag3Err	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Error in default point/extended source Z (2.0 arcsec aperture diameter) magnitude	real	4	mag	-0.9999995e9	stat.error
zAperMag3Err	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Error in default point/extended source Z (2.0 arcsec aperture diameter) magnitude	real	4	mag	-0.9999995e9	stat.error
zAperMag3Err	vvvSource	VVVDR2	Error in default point/extended source Z mag (2.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag3Err	vvvSource	VVVDR5	Error in default point source Z mag (2.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.I
zAperMag3Err	vvvSource	VVVv20100531	Error in default point/extended source Z mag (2.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag3Err	vvvSource	VVVv20110718	Error in default point/extended source Z mag (2.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag3Err	vvvSource, vvvSynopticSource	VVVDR1	Error in default point/extended source Z mag (2.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag3Err	vvvVivaCatalogue	VVVDR5	Error in default point source Z mag, from VVVDR4 {catalogue TType keyword: zAperMag3Err}	real	4	mag	-9.999995e8
zAperMag4	videoSource	VIDEODR2	Point source Z aperture corrected mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMag4	videoSource	VIDEODR3	Point source Z aperture corrected mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMag4	videoSource	VIDEODR4	Point source Z aperture corrected mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag4	videoSource	VIDEODR5	Point source Z aperture corrected mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag4	videoSource	VIDEOv20100513	Extended source Z mag, no aperture correction applied	real	4	mag	-0.9999995e9	phot.mag
zAperMag4	videoSource	VIDEOv20111208	Point source Z aperture corrected mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMag4	vikingSource	VIKINGDR2	Point source Z aperture corrected mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMag4	vikingSource	VIKINGDR3	Point source Z aperture corrected mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMag4	vikingSource	VIKINGDR4	Point source Z aperture corrected mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag4	vikingSource	VIKINGv20110714	Point source Z aperture corrected mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMag4	vikingSource	VIKINGv20111019	Point source Z aperture corrected mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMag4	vikingSource	VIKINGv20130417	Point source Z aperture corrected mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMag4	vikingSource	VIKINGv20140402	Point source Z aperture corrected mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag4	vikingSource	VIKINGv20150421	Point source Z aperture corrected mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag4	vikingSource	VIKINGv20151230	Point source Z aperture corrected mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag4	vikingSource	VIKINGv20160406	Point source Z aperture corrected mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag4	vikingSource	VIKINGv20161202	Point source Z aperture corrected mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag4	vikingSource	VIKINGv20170715	Point source Z aperture corrected mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag4	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Point source Z aperture corrected (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMag4	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Point source Z aperture corrected (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMag4	vvvSource	VVVDR2	Extended source Z aperture corrected mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag4	vvvSource	VVVDR5	Point source Z aperture corrected mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag4	vvvSource	VVVv20100531	Extended source Z aperture corrected mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMag4	vvvSource	VVVv20110718	Extended source Z aperture corrected mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMag4	vvvSource, vvvSynopticSource	VVVDR1	Extended source Z aperture corrected mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMag4Err	videoSource	VIDEODR2	Error in point/extended source Z mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag4Err	videoSource	VIDEODR3	Error in point/extended source Z mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag4Err	videoSource	VIDEODR4	Error in point/extended source Z mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error;em.opt.I;phot.mag
zAperMag4Err	videoSource	VIDEODR5	Error in point/extended source Z mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error;em.opt.I;phot.mag
zAperMag4Err	videoSource	VIDEOv20100513	Error in extended source Z mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag4Err	videoSource	VIDEOv20111208	Error in point/extended source Z mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag4Err	vikingSource	VIKINGDR2	Error in point/extended source Z mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag4Err	vikingSource	VIKINGDR3	Error in point/extended source Z mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag4Err	vikingSource	VIKINGDR4	Error in point/extended source Z mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error;em.opt.I
zAperMag4Err	vikingSource	VIKINGv20110714	Error in point/extended source Z mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag4Err	vikingSource	VIKINGv20111019	Error in point/extended source Z mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag4Err	vikingSource	VIKINGv20130417	Error in point/extended source Z mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag4Err	vikingSource	VIKINGv20140402	Error in point/extended source Z mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag4Err	vikingSource	VIKINGv20150421	Error in point/extended source Z mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error;em.opt.I;phot.mag
zAperMag4Err	vikingSource	VIKINGv20151230	Error in point/extended source Z mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.I
zAperMag4Err	vikingSource	VIKINGv20160406	Error in point/extended source Z mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.I
zAperMag4Err	vikingSource	VIKINGv20161202	Error in point/extended source Z mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.I
zAperMag4Err	vikingSource	VIKINGv20170715	Error in point/extended source Z mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.I
zAperMag4Err	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Error in point/extended source Z (2.8 arcsec aperture diameter) magnitude	real	4	mag	-0.9999995e9	stat.error
zAperMag4Err	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Error in point/extended source Z (2.8 arcsec aperture diameter) magnitude	real	4	mag	-0.9999995e9	stat.error
zAperMag4Err	vvvSource	VVVDR2	Error in extended source Z mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag4Err	vvvSource	VVVDR5	Error in point source Z mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.I
zAperMag4Err	vvvSource	VVVv20100531	Error in extended source Z mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag4Err	vvvSource	VVVv20110718	Error in extended source Z mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag4Err	vvvSource, vvvSynopticSource	VVVDR1	Error in extended source Z mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag5	vvvSynopticSource	VVVDR1	Extended source Z aperture corrected mag (4.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMag5	vvvSynopticSource	VVVDR2	Extended source Z aperture corrected mag (4.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag5Err	vvvSynopticSource	VVVDR1	Error in extended source Z mag (4.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag5Err	vvvSynopticSource	VVVDR2	Error in extended source Z mag (4.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag6	videoSource	VIDEODR2	Point source Z aperture corrected mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMag6	videoSource	VIDEODR3	Point source Z aperture corrected mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMag6	videoSource	VIDEODR4	Point source Z aperture corrected mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag6	videoSource	VIDEODR5	Point source Z aperture corrected mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag6	videoSource	VIDEOv20100513	Extended source Z mag, no aperture correction applied	real	4	mag	-0.9999995e9	phot.mag
zAperMag6	videoSource	VIDEOv20111208	Point source Z aperture corrected mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMag6	vikingSource	VIKINGDR2	Point source Z aperture corrected mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMag6	vikingSource	VIKINGDR3	Point source Z aperture corrected mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMag6	vikingSource	VIKINGDR4	Point source Z aperture corrected mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag6	vikingSource	VIKINGv20110714	Point source Z aperture corrected mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMag6	vikingSource	VIKINGv20111019	Point source Z aperture corrected mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMag6	vikingSource	VIKINGv20130417	Point source Z aperture corrected mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMag6	vikingSource	VIKINGv20140402	Point source Z aperture corrected mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag6	vikingSource	VIKINGv20150421	Point source Z aperture corrected mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag6	vikingSource	VIKINGv20151230	Point source Z aperture corrected mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag6	vikingSource	VIKINGv20160406	Point source Z aperture corrected mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag6	vikingSource	VIKINGv20161202	Point source Z aperture corrected mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag6	vikingSource	VIKINGv20170715	Point source Z aperture corrected mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMag6	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Point source Z aperture corrected (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMag6	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Point source Z aperture corrected (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMag6Err	videoSource	VIDEODR2	Error in point/extended source Z mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag6Err	videoSource	VIDEODR3	Error in point/extended source Z mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag6Err	videoSource	VIDEODR4	Error in point/extended source Z mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error;em.opt.I;phot.mag
zAperMag6Err	videoSource	VIDEODR5	Error in point/extended source Z mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error;em.opt.I;phot.mag
zAperMag6Err	videoSource	VIDEOv20100513	Error in extended source Z mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag6Err	videoSource	VIDEOv20111208	Error in point/extended source Z mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag6Err	vikingSource	VIKINGDR2	Error in point/extended source Z mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag6Err	vikingSource	VIKINGDR3	Error in point/extended source Z mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag6Err	vikingSource	VIKINGDR4	Error in point/extended source Z mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error;em.opt.I
zAperMag6Err	vikingSource	VIKINGv20110714	Error in point/extended source Z mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag6Err	vikingSource	VIKINGv20111019	Error in point/extended source Z mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag6Err	vikingSource	VIKINGv20130417	Error in point/extended source Z mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag6Err	vikingSource	VIKINGv20140402	Error in point/extended source Z mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error
zAperMag6Err	vikingSource	VIKINGv20150421	Error in point/extended source Z mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error;em.opt.I;phot.mag
zAperMag6Err	vikingSource	VIKINGv20151230	Error in point/extended source Z mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.I
zAperMag6Err	vikingSource	VIKINGv20160406	Error in point/extended source Z mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.I
zAperMag6Err	vikingSource	VIKINGv20161202	Error in point/extended source Z mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.I
zAperMag6Err	vikingSource	VIKINGv20170715	Error in point/extended source Z mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.I
zAperMag6Err	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Error in point/extended source Z (5.7 arcsec aperture diameter) magnitude	real	4	mag	-0.9999995e9	stat.error
zAperMag6Err	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Error in point/extended source Z (5.7 arcsec aperture diameter) magnitude	real	4	mag	-0.9999995e9	stat.error
zAperMagNoAperCorr3	videoSource	VIDEODR2	Default extended source Z aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag
zAperMagNoAperCorr3	videoSource	VIDEODR3	Default extended source Z aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag
zAperMagNoAperCorr3	videoSource	VIDEODR4	Default extended source Z aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMagNoAperCorr3	videoSource	VIDEODR5	Default extended source Z aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMagNoAperCorr3	videoSource	VIDEOv20111208	Default extended source Z aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag
zAperMagNoAperCorr3	vikingSource	VIKINGDR2	Default extended source Z aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag
zAperMagNoAperCorr3	vikingSource	VIKINGDR3	Default extended source Z aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag
zAperMagNoAperCorr3	vikingSource	VIKINGDR4	Default extended source Z aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMagNoAperCorr3	vikingSource	VIKINGv20110714	Default extended source Z aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag
zAperMagNoAperCorr3	vikingSource	VIKINGv20111019	Default extended source Z aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag
zAperMagNoAperCorr3	vikingSource	VIKINGv20130417	Default extended source Z aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag
zAperMagNoAperCorr3	vikingSource	VIKINGv20140402	Default extended source Z aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMagNoAperCorr3	vikingSource	VIKINGv20150421	Default extended source Z aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMagNoAperCorr3	vikingSource	VIKINGv20151230	Default extended source Z aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMagNoAperCorr3	vikingSource	VIKINGv20160406	Default extended source Z aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMagNoAperCorr3	vikingSource	VIKINGv20161202	Default extended source Z aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMagNoAperCorr3	vikingSource	VIKINGv20170715	Default extended source Z aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMagNoAperCorr3	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Default extended source Z (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
zAperMagNoAperCorr3	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Default extended source Z (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
zAperMagNoAperCorr4	videoSource	VIDEODR2	Extended source Z aperture mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMagNoAperCorr4	videoSource	VIDEODR3	Extended source Z aperture mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMagNoAperCorr4	videoSource	VIDEODR4	Extended source Z aperture mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMagNoAperCorr4	videoSource	VIDEODR5	Extended source Z aperture mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMagNoAperCorr4	videoSource	VIDEOv20111208	Extended source Z aperture mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMagNoAperCorr4	vikingSource	VIKINGDR2	Extended source Z aperture mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMagNoAperCorr4	vikingSource	VIKINGDR3	Extended source Z aperture mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMagNoAperCorr4	vikingSource	VIKINGDR4	Extended source Z aperture mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMagNoAperCorr4	vikingSource	VIKINGv20110714	Extended source Z aperture mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMagNoAperCorr4	vikingSource	VIKINGv20111019	Extended source Z aperture mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMagNoAperCorr4	vikingSource	VIKINGv20130417	Extended source Z aperture mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMagNoAperCorr4	vikingSource	VIKINGv20140402	Extended source Z aperture mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMagNoAperCorr4	vikingSource	VIKINGv20150421	Extended source Z aperture mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMagNoAperCorr4	vikingSource	VIKINGv20151230	Extended source Z aperture mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMagNoAperCorr4	vikingSource	VIKINGv20160406	Extended source Z aperture mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMagNoAperCorr4	vikingSource	VIKINGv20161202	Extended source Z aperture mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMagNoAperCorr4	vikingSource	VIKINGv20170715	Extended source Z aperture mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMagNoAperCorr4	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Extended source Z (2.8 arcsec aperture diameter, but no aperture correction applied) aperture magnitude	real	4	mag	-0.9999995e9	phot.mag
zAperMagNoAperCorr4	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Extended source Z (2.8 arcsec aperture diameter, but no aperture correction applied) aperture magnitude	real	4	mag	-0.9999995e9	phot.mag
zAperMagNoAperCorr6	videoSource	VIDEODR2	Extended source Z aperture mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMagNoAperCorr6	videoSource	VIDEODR3	Extended source Z aperture mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMagNoAperCorr6	videoSource	VIDEODR4	Extended source Z aperture mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMagNoAperCorr6	videoSource	VIDEODR5	Extended source Z aperture mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMagNoAperCorr6	videoSource	VIDEOv20111208	Extended source Z aperture mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMagNoAperCorr6	vikingSource	VIKINGDR2	Extended source Z aperture mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMagNoAperCorr6	vikingSource	VIKINGDR3	Extended source Z aperture mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMagNoAperCorr6	vikingSource	VIKINGDR4	Extended source Z aperture mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMagNoAperCorr6	vikingSource	VIKINGv20110714	Extended source Z aperture mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMagNoAperCorr6	vikingSource	VIKINGv20111019	Extended source Z aperture mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMagNoAperCorr6	vikingSource	VIKINGv20130417	Extended source Z aperture mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag
zAperMagNoAperCorr6	vikingSource	VIKINGv20140402	Extended source Z aperture mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMagNoAperCorr6	vikingSource	VIKINGv20150421	Extended source Z aperture mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMagNoAperCorr6	vikingSource	VIKINGv20151230	Extended source Z aperture mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMagNoAperCorr6	vikingSource	VIKINGv20160406	Extended source Z aperture mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMagNoAperCorr6	vikingSource	VIKINGv20161202	Extended source Z aperture mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMagNoAperCorr6	vikingSource	VIKINGv20170715	Extended source Z aperture mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zAperMagNoAperCorr6	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Extended source Z (5.7 arcsec aperture diameter, but no aperture correction applied) aperture magnitude	real	4	mag	-0.9999995e9	phot.mag
zAperMagNoAperCorr6	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Extended source Z (5.7 arcsec aperture diameter, but no aperture correction applied) aperture magnitude	real	4	mag	-0.9999995e9	phot.mag
zApFillFac	StackObjectAttributes	PS1DR2	Aperture fill factor from z filter stack detection.	real	4		-999
zApFlux	StackObjectAttributes	PS1DR2	Aperture flux from z filter stack detection.	real	4	Janskys	-999
zApFluxErr	StackObjectAttributes	PS1DR2	Error in aperture flux from z filter stack detection.	real	4	Janskys	-999
zApMag	StackObjectThin	PS1DR2	Aperture magnitude from z filter stack detection.	real	4	AB magnitudes	-999
zApMagErr	StackObjectThin	PS1DR2	Error in aperture magnitude from z filter stack detection.	real	4	AB magnitudes	-999
zApRadius	StackObjectAttributes	PS1DR2	Aperture radius for z filter stack detection.	real	4	arcsec	-999
zaStratAst	videoVarFrameSetInfo	VIDEODR2	Strateva parameter, a, in fit to astrometric rms vs magnitude in Z 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.
zaStratAst	videoVarFrameSetInfo	VIDEODR3	Strateva parameter, a, in fit to astrometric rms vs magnitude in Z 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.
zaStratAst	videoVarFrameSetInfo	VIDEODR4	Strateva parameter, a, in fit to astrometric rms vs magnitude in Z band, see Sesar et al. 2007.	real	4		-0.9999995e9	stat.fit.param;em.opt.I
			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.
zaStratAst	videoVarFrameSetInfo	VIDEODR5	Strateva parameter, a, in fit to astrometric rms vs magnitude in Z band, see Sesar et al. 2007.	real	4		-0.9999995e9	stat.fit.param;em.opt.I
			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.
zaStratAst	videoVarFrameSetInfo	VIDEOv20111208	Strateva parameter, a, in fit to astrometric rms vs magnitude in Z 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.
zaStratAst	vikingVarFrameSetInfo	VIKINGv20110714	Strateva parameter, a, in fit to astrometric rms vs magnitude in Z 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.
zaStratAst	vvvVarFrameSetInfo	VVVDR5	Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Z band.	real	4		-0.9999995e9	stat.fit.param;em.opt.I
			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.
zaStratPht	videoVarFrameSetInfo	VIDEODR2	Strateva parameter, a, in fit to photometric rms vs magnitude in Z 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.
zaStratPht	videoVarFrameSetInfo	VIDEODR3	Strateva parameter, a, in fit to photometric rms vs magnitude in Z 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.
zaStratPht	videoVarFrameSetInfo	VIDEODR4	Strateva parameter, a, in fit to photometric rms vs magnitude in Z band, see Sesar et al. 2007.	real	4		-0.9999995e9	stat.fit.param;em.opt.I
			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.
zaStratPht	videoVarFrameSetInfo	VIDEODR5	Strateva parameter, a, in fit to photometric rms vs magnitude in Z band, see Sesar et al. 2007.	real	4		-0.9999995e9	stat.fit.param;em.opt.I
			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.
zaStratPht	videoVarFrameSetInfo	VIDEOv20111208	Strateva parameter, a, in fit to photometric rms vs magnitude in Z 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.
zaStratPht	vikingVarFrameSetInfo	VIKINGv20110714	Strateva parameter, a, in fit to photometric rms vs magnitude in Z 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.
zaStratPht	vvvVarFrameSetInfo	VVVDR5	Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Z band.	real	4		-0.9999995e9	stat.fit.param;em.opt.I
			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.
zAverageConf	vikingSource	VIKINGDR2	average confidence in 2 arcsec diameter default aperture (aper3) Z	real	4		-99999999	meta.code
zAverageConf	vikingSource	VIKINGDR3	average confidence in 2 arcsec diameter default aperture (aper3) Z	real	4		-99999999	stat.likelihood;em.IR.NIR
zAverageConf	vikingSource	VIKINGDR4	average confidence in 2 arcsec diameter default aperture (aper3) Z	real	4		-0.9999995e9	stat.likelihood;em.opt.I
zAverageConf	vikingSource	VIKINGv20110714	average confidence in 2 arcsec diameter default aperture (aper3) Z	real	4		-99999999	meta.code
zAverageConf	vikingSource	VIKINGv20111019	average confidence in 2 arcsec diameter default aperture (aper3) Z	real	4		-99999999	meta.code
zAverageConf	vikingSource	VIKINGv20130417	average confidence in 2 arcsec diameter default aperture (aper3) Z	real	4		-0.9999995e9	stat.likelihood;em.IR.NIR
zAverageConf	vikingSource	VIKINGv20140402	average confidence in 2 arcsec diameter default aperture (aper3) Z	real	4		-0.9999995e9	stat.likelihood;em.IR.NIR
zAverageConf	vikingSource	VIKINGv20150421	average confidence in 2 arcsec diameter default aperture (aper3) Z	real	4		-0.9999995e9	stat.likelihood;em.opt.I
zAverageConf	vikingSource	VIKINGv20151230	average confidence in 2 arcsec diameter default aperture (aper3) Z	real	4		-0.9999995e9	stat.likelihood;em.opt.I
zAverageConf	vikingSource	VIKINGv20160406	average confidence in 2 arcsec diameter default aperture (aper3) Z	real	4		-0.9999995e9	stat.likelihood;em.opt.I
zAverageConf	vikingSource	VIKINGv20161202	average confidence in 2 arcsec diameter default aperture (aper3) Z	real	4		-0.9999995e9	stat.likelihood;em.opt.I
zAverageConf	vikingSource	VIKINGv20170715	average confidence in 2 arcsec diameter default aperture (aper3) Z	real	4		-0.9999995e9	stat.likelihood;em.opt.I
zAverageConf	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	average confidence in 2 arcsec diameter default aperture (aper3) Z	real	4		-0.9999995e9	stat.likelihood;em.IR.NIR
zAverageConf	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	average confidence in 2 arcsec diameter default aperture (aper3) Z	real	4		-0.9999995e9	stat.likelihood;em.IR.NIR
zAverageConf	vvvSource	VVVDR2	average confidence in 2 arcsec diameter default aperture (aper3) Z	real	4		-0.9999995e9	stat.likelihood;em.IR.NIR
zAverageConf	vvvSource	VVVDR5	average confidence in 2 arcsec diameter default aperture (aper3) Z	real	4		-0.9999995e9	stat.likelihood;em.opt.I
zAverageConf	vvvSource, vvvSynopticSource	VVVDR1	average confidence in 2 arcsec diameter default aperture (aper3) Z	real	4		-99999999	stat.likelihood;em.IR.NIR
zbestAper	videoVariability	VIDEODR2	Best aperture (1-6) for photometric statistics in the Z 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)
zbestAper	videoVariability	VIDEODR3	Best aperture (1-6) for photometric statistics in the Z 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)
zbestAper	videoVariability	VIDEODR4	Best aperture (1-6) for photometric statistics in the Z band	int	4		-9999	meta.code.class;em.opt.I
			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)
zbestAper	videoVariability	VIDEODR5	Best aperture (1-6) for photometric statistics in the Z band	int	4		-9999	meta.code.class;em.opt.I
			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)
zbestAper	videoVariability	VIDEOv20111208	Best aperture (1-6) for photometric statistics in the Z 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)
zbestAper	vikingVariability	VIKINGv20110714	Best aperture (1-6) for photometric statistics in the Z 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)
zbestAper	vvvVariability	VVVDR5	Best aperture (1-6) for photometric statistics in the Z band	int	4		-9999	meta.code.class;em.opt.I
			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)
zbStratAst	videoVarFrameSetInfo	VIDEODR2	Strateva parameter, b, in fit to astrometric rms vs magnitude in Z 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.
zbStratAst	videoVarFrameSetInfo	VIDEODR3	Strateva parameter, b, in fit to astrometric rms vs magnitude in Z 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.
zbStratAst	videoVarFrameSetInfo	VIDEODR4	Strateva parameter, b, in fit to astrometric rms vs magnitude in Z band, see Sesar et al. 2007.	real	4		-0.9999995e9	stat.fit.param;em.opt.I
			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.
zbStratAst	videoVarFrameSetInfo	VIDEODR5	Strateva parameter, b, in fit to astrometric rms vs magnitude in Z band, see Sesar et al. 2007.	real	4		-0.9999995e9	stat.fit.param;em.opt.I
			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.
zbStratAst	videoVarFrameSetInfo	VIDEOv20111208	Strateva parameter, b, in fit to astrometric rms vs magnitude in Z 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.
zbStratAst	vikingVarFrameSetInfo	VIKINGv20110714	Strateva parameter, b, in fit to astrometric rms vs magnitude in Z 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.
zbStratAst	vvvVarFrameSetInfo	VVVDR5	Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Z band.	real	4		-0.9999995e9	stat.fit.param;em.opt.I
			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.
zbStratPht	videoVarFrameSetInfo	VIDEODR2	Strateva parameter, b, in fit to photometric rms vs magnitude in Z 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.
zbStratPht	videoVarFrameSetInfo	VIDEODR3	Strateva parameter, b, in fit to photometric rms vs magnitude in Z 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.
zbStratPht	videoVarFrameSetInfo	VIDEODR4	Strateva parameter, b, in fit to photometric rms vs magnitude in Z band, see Sesar et al. 2007.	real	4		-0.9999995e9	stat.fit.param;em.opt.I
			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.
zbStratPht	videoVarFrameSetInfo	VIDEODR5	Strateva parameter, b, in fit to photometric rms vs magnitude in Z band, see Sesar et al. 2007.	real	4		-0.9999995e9	stat.fit.param;em.opt.I
			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.
zbStratPht	videoVarFrameSetInfo	VIDEOv20111208	Strateva parameter, b, in fit to photometric rms vs magnitude in Z 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.
zbStratPht	vikingVarFrameSetInfo	VIKINGv20110714	Strateva parameter, b, in fit to photometric rms vs magnitude in Z 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.
zbStratPht	vvvVarFrameSetInfo	VVVDR5	Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Z band.	real	4		-0.9999995e9	stat.fit.param;em.opt.I
			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.
ZCATERR	target	SIXDF	error on velocity in ZCAT	int	4	km/s
ZCATREF	target	SIXDF	ZCAT reference	smallint	2
ZCATVEL	target	SIXDF	velocity in ZCAT	int	4	km/s
zchiSqAst	videoVarFrameSetInfo	VIDEODR2	Goodness of fit of Strateva function to astrometric data in Z 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.
zchiSqAst	videoVarFrameSetInfo	VIDEODR3	Goodness of fit of Strateva function to astrometric data in Z 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.
zchiSqAst	videoVarFrameSetInfo	VIDEODR4	Goodness of fit of Strateva function to astrometric data in Z band	real	4		-0.9999995e9	stat.fit.goodness;em.opt.I
			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.
zchiSqAst	videoVarFrameSetInfo	VIDEODR5	Goodness of fit of Strateva function to astrometric data in Z band	real	4		-0.9999995e9	stat.fit.goodness;em.opt.I
			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.
zchiSqAst	videoVarFrameSetInfo	VIDEOv20111208	Goodness of fit of Strateva function to astrometric data in Z 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.
zchiSqAst	vikingVarFrameSetInfo	VIKINGv20110714	Goodness of fit of Strateva function to astrometric data in Z 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.
zchiSqAst	vvvVarFrameSetInfo	VVVDR5	Goodness of fit of Strateva function to astrometric data in Z band	real	4		-0.9999995e9	stat.fit.goodness;em.opt.I
			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.
zchiSqpd	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.
zchiSqpd	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.
zchiSqpd	videoVariability	VIDEODR4	Chi square (per degree of freedom) fit to data (mean and expected rms)	real	4		-0.9999995e9	stat.fit.chi2;em.opt.I
			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.
zchiSqpd	videoVariability	VIDEODR5	Chi square (per degree of freedom) fit to data (mean and expected rms)	real	4		-0.9999995e9	stat.fit.chi2;em.opt.I
			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.
zchiSqpd	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.
zchiSqpd	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.
zchiSqpd	vvvVariability	VVVDR5	Chi square (per degree of freedom) fit to data (mean and expected rms)	real	4		-0.9999995e9	stat.fit.chi2;em.opt.I
			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.
zchiSqPht	videoVarFrameSetInfo	VIDEODR2	Goodness of fit of Strateva function to photometric data in Z 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.
zchiSqPht	videoVarFrameSetInfo	VIDEODR3	Goodness of fit of Strateva function to photometric data in Z 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.
zchiSqPht	videoVarFrameSetInfo	VIDEODR4	Goodness of fit of Strateva function to photometric data in Z band	real	4		-0.9999995e9	stat.fit.goodness;em.opt.I
			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.
zchiSqPht	videoVarFrameSetInfo	VIDEODR5	Goodness of fit of Strateva function to photometric data in Z band	real	4		-0.9999995e9	stat.fit.goodness;em.opt.I
			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.
zchiSqPht	videoVarFrameSetInfo	VIDEOv20111208	Goodness of fit of Strateva function to photometric data in Z 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.
zchiSqPht	vikingVarFrameSetInfo	VIKINGv20110714	Goodness of fit of Strateva function to photometric data in Z 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.
zchiSqPht	vvvVarFrameSetInfo	VVVDR5	Goodness of fit of Strateva function to photometric data in Z band	real	4		-0.9999995e9	stat.fit.goodness;em.opt.I
			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.
Zclass	vvvParallaxCatalogue, vvvProperMotionCatalogue	VVVDR5	VVV DR4 Z 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: Zclass}	int	4		-99999999
zClass	videoSource	VIDEODR2	discrete image classification flag in Z	smallint	2		-9999	src.class
zClass	videoSource	VIDEODR3	discrete image classification flag in Z	smallint	2		-9999	src.class
zClass	videoSource	VIDEODR4	discrete image classification flag in Z	smallint	2		-9999	src.class;em.opt.I
zClass	videoSource	VIDEODR5	discrete image classification flag in Z	smallint	2		-9999	src.class;em.opt.I
zClass	videoSource	VIDEOv20111208	discrete image classification flag in Z	smallint	2		-9999	src.class
zClass	videoSource, videoSourceRemeasurement	VIDEOv20100513	discrete image classification flag in Z	smallint	2		-9999	src.class
zClass	vikingSource	VIKINGDR2	discrete image classification flag in Z	smallint	2		-9999	src.class
zClass	vikingSource	VIKINGDR3	discrete image classification flag in Z	smallint	2		-9999	src.class
zClass	vikingSource	VIKINGDR4	discrete image classification flag in Z	smallint	2		-9999	src.class;em.opt.I
zClass	vikingSource	VIKINGv20111019	discrete image classification flag in Z	smallint	2		-9999	src.class
zClass	vikingSource	VIKINGv20130417	discrete image classification flag in Z	smallint	2		-9999	src.class
zClass	vikingSource	VIKINGv20140402	discrete image classification flag in Z	smallint	2		-9999	src.class
zClass	vikingSource	VIKINGv20150421	discrete image classification flag in Z	smallint	2		-9999	src.class;em.opt.I
zClass	vikingSource	VIKINGv20151230	discrete image classification flag in Z	smallint	2		-9999	src.class;em.opt.I
zClass	vikingSource	VIKINGv20160406	discrete image classification flag in Z	smallint	2		-9999	src.class;em.opt.I
zClass	vikingSource	VIKINGv20161202	discrete image classification flag in Z	smallint	2		-9999	src.class;em.opt.I
zClass	vikingSource	VIKINGv20170715	discrete image classification flag in Z	smallint	2		-9999	src.class;em.opt.I
zClass	vikingSource, vikingSourceRemeasurement	VIKINGv20110714	discrete image classification flag in Z	smallint	2		-9999	src.class
zClass	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	discrete image classification flag in Z	smallint	2		-9999	src.class
zClass	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	discrete image classification flag in Z	smallint	2		-9999	src.class
zClass	vvvSource	VVVDR2	discrete image classification flag in Z	smallint	2		-9999	src.class
zClass	vvvSource	VVVDR5	discrete image classification flag in Z	smallint	2		-9999	src.class;em.opt.I
zClass	vvvSource	VVVv20110718	discrete image classification flag in Z	smallint	2		-9999	src.class
zClass	vvvSource, vvvSourceRemeasurement	VVVv20100531	discrete image classification flag in Z	smallint	2		-9999	src.class
zClass	vvvSource, vvvSynopticSource	VVVDR1	discrete image classification flag in Z	smallint	2		-9999	src.class
zClassStat	videoSource	VIDEODR2	S-Extractor classification statistic in Z	real	4		-0.9999995e9	stat
zClassStat	videoSource	VIDEODR3	S-Extractor classification statistic in Z	real	4		-0.9999995e9	stat
zClassStat	videoSource	VIDEODR4	S-Extractor classification statistic in Z	real	4		-0.9999995e9	stat;em.opt.I
zClassStat	videoSource	VIDEODR5	S-Extractor classification statistic in Z	real	4		-0.9999995e9	stat;em.opt.I
zClassStat	videoSource	VIDEOv20100513	S-Extractor classification statistic in Z	real	4		-0.9999995e9	stat
zClassStat	videoSource	VIDEOv20111208	S-Extractor classification statistic in Z	real	4		-0.9999995e9	stat
zClassStat	videoSourceRemeasurement	VIDEOv20100513	N(0,1) stellarness-of-profile statistic in Z	real	4		-0.9999995e9	stat
zClassStat	vikingSource	VIKINGDR2	N(0,1) stellarness-of-profile statistic in Z	real	4		-0.9999995e9	stat
zClassStat	vikingSource	VIKINGDR3	N(0,1) stellarness-of-profile statistic in Z	real	4		-0.9999995e9	stat
zClassStat	vikingSource	VIKINGDR4	N(0,1) stellarness-of-profile statistic in Z	real	4		-0.9999995e9	stat;em.opt.I
zClassStat	vikingSource	VIKINGv20111019	N(0,1) stellarness-of-profile statistic in Z	real	4		-0.9999995e9	stat
zClassStat	vikingSource	VIKINGv20130417	N(0,1) stellarness-of-profile statistic in Z	real	4		-0.9999995e9	stat
zClassStat	vikingSource	VIKINGv20140402	N(0,1) stellarness-of-profile statistic in Z	real	4		-0.9999995e9	stat
zClassStat	vikingSource	VIKINGv20150421	N(0,1) stellarness-of-profile statistic in Z	real	4		-0.9999995e9	stat;em.opt.I
zClassStat	vikingSource	VIKINGv20151230	N(0,1) stellarness-of-profile statistic in Z	real	4		-0.9999995e9	stat;em.opt.I
zClassStat	vikingSource	VIKINGv20160406	N(0,1) stellarness-of-profile statistic in Z	real	4		-0.9999995e9	stat;em.opt.I
zClassStat	vikingSource	VIKINGv20161202	N(0,1) stellarness-of-profile statistic in Z	real	4		-0.9999995e9	stat;em.opt.I
zClassStat	vikingSource	VIKINGv20170715	N(0,1) stellarness-of-profile statistic in Z	real	4		-0.9999995e9	stat;em.opt.I
zClassStat	vikingSource, vikingSourceRemeasurement	VIKINGv20110714	N(0,1) stellarness-of-profile statistic in Z	real	4		-0.9999995e9	stat
zClassStat	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	N(0,1) stellarness-of-profile statistic in Z	real	4		-0.9999995e9	stat
zClassStat	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	N(0,1) stellarness-of-profile statistic in Z	real	4		-0.9999995e9	stat
zClassStat	vvvSource	VVVDR1	S-Extractor classification statistic in Z	real	4		-0.9999995e9	stat
zClassStat	vvvSource	VVVDR2	S-Extractor classification statistic in Z	real	4		-0.9999995e9	stat
zClassStat	vvvSource	VVVDR5	S-Extractor classification statistic in Z	real	4		-0.9999995e9	stat;em.opt.I
zClassStat	vvvSource	VVVv20100531	S-Extractor classification statistic in Z	real	4		-0.9999995e9	stat
zClassStat	vvvSource	VVVv20110718	S-Extractor classification statistic in Z	real	4		-0.9999995e9	stat
zClassStat	vvvSourceRemeasurement	VVVv20100531	N(0,1) stellarness-of-profile statistic in Z	real	4		-0.9999995e9	stat
zClassStat	vvvSourceRemeasurement	VVVv20110718	N(0,1) stellarness-of-profile statistic in Z	real	4		-0.9999995e9	stat
zClassStat	vvvSynopticSource	VVVDR1	N(0,1) stellarness-of-profile statistic in Z	real	4		-0.9999995e9	stat
zClassStat	vvvSynopticSource	VVVDR2	N(0,1) stellarness-of-profile statistic in Z	real	4		-0.9999995e9	stat
zcStratAst	videoVarFrameSetInfo	VIDEODR2	Strateva parameter, c, in fit to astrometric rms vs magnitude in Z 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.
zcStratAst	videoVarFrameSetInfo	VIDEODR3	Strateva parameter, c, in fit to astrometric rms vs magnitude in Z 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.
zcStratAst	videoVarFrameSetInfo	VIDEODR4	Strateva parameter, c, in fit to astrometric rms vs magnitude in Z band, see Sesar et al. 2007.	real	4		-0.9999995e9	stat.fit.param;em.opt.I
			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.
zcStratAst	videoVarFrameSetInfo	VIDEODR5	Strateva parameter, c, in fit to astrometric rms vs magnitude in Z band, see Sesar et al. 2007.	real	4		-0.9999995e9	stat.fit.param;em.opt.I
			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.
zcStratAst	videoVarFrameSetInfo	VIDEOv20111208	Strateva parameter, c, in fit to astrometric rms vs magnitude in Z 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.
zcStratAst	vikingVarFrameSetInfo	VIKINGv20110714	Strateva parameter, c, in fit to astrometric rms vs magnitude in Z 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.
zcStratAst	vvvVarFrameSetInfo	VVVDR5	Parameter, c2 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Z band.	real	4		-0.9999995e9	stat.fit.param;em.opt.I
			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.
zcStratPht	videoVarFrameSetInfo	VIDEODR2	Strateva parameter, c, in fit to photometric rms vs magnitude in Z 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.
zcStratPht	videoVarFrameSetInfo	VIDEODR3	Strateva parameter, c, in fit to photometric rms vs magnitude in Z 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.
zcStratPht	videoVarFrameSetInfo	VIDEODR4	Strateva parameter, c, in fit to photometric rms vs magnitude in Z band, see Sesar et al. 2007.	real	4		-0.9999995e9	stat.fit.param;em.opt.I
			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.
zcStratPht	videoVarFrameSetInfo	VIDEODR5	Strateva parameter, c, in fit to photometric rms vs magnitude in Z band, see Sesar et al. 2007.	real	4		-0.9999995e9	stat.fit.param;em.opt.I
			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.
zcStratPht	videoVarFrameSetInfo	VIDEOv20111208	Strateva parameter, c, in fit to photometric rms vs magnitude in Z 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.
zcStratPht	vikingVarFrameSetInfo	VIKINGv20110714	Strateva parameter, c, in fit to photometric rms vs magnitude in Z 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.
zcStratPht	vvvVarFrameSetInfo	VVVDR5	Parameter, c2 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Z band.	real	4		-0.9999995e9	stat.fit.param;em.opt.I
			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.
zd	twomass_scn	TWOMASS	Scan's distance from the zenith at beginning of scan.	real	4	degrees		stat.fit.residual;pos.az.zd
zd	twomass_sixx2_scn	TWOMASS	beginning zenith distance of scan data	real	4	deg
zDeblend	videoSource, videoSourceRemeasurement	VIDEOv20100513	placeholder flag indicating parent/child relation in Z	int	4		-99999999	meta.code
zDeblend	vikingSourceRemeasurement	VIKINGv20110714	placeholder flag indicating parent/child relation in Z	int	4		-99999999	meta.code
zDeblend	vikingSourceRemeasurement	VIKINGv20111019	placeholder flag indicating parent/child relation in Z	int	4		-99999999	meta.code
zDeblend	vvvSource	VVVv20110718	placeholder flag indicating parent/child relation in Z	int	4		-99999999	meta.code
zDeblend	vvvSource, vvvSourceRemeasurement	VVVv20100531	placeholder flag indicating parent/child relation in Z	int	4		-99999999	meta.code
zdec	StackObjectThin	PS1DR2	Declination from z filter stack detection.	float	8	degrees	-999
zdecErr	StackObjectThin	PS1DR2	Declination error from z filter stack detection.	real	4	arcsec	-999
Zell	vvvParallaxCatalogue, vvvProperMotionCatalogue	VVVDR5	Ellipticity of the DR4 Z detection. {catalogue TType keyword: Zell}	real	4		-999999500.0
zEll	videoSource	VIDEODR2	1-b/a, where a/b=semi-major/minor axes in Z	real	4		-0.9999995e9	src.ellipticity
zEll	videoSource	VIDEODR3	1-b/a, where a/b=semi-major/minor axes in Z	real	4		-0.9999995e9	src.ellipticity
zEll	videoSource	VIDEODR4	1-b/a, where a/b=semi-major/minor axes in Z	real	4		-0.9999995e9	src.ellipticity;em.opt.I
zEll	videoSource	VIDEODR5	1-b/a, where a/b=semi-major/minor axes in Z	real	4		-0.9999995e9	src.ellipticity;em.opt.I
zEll	videoSource	VIDEOv20111208	1-b/a, where a/b=semi-major/minor axes in Z	real	4		-0.9999995e9	src.ellipticity
zEll	videoSource, videoSourceRemeasurement	VIDEOv20100513	1-b/a, where a/b=semi-major/minor axes in Z	real	4		-0.9999995e9	src.ellipticity
zEll	vikingSource	VIKINGDR2	1-b/a, where a/b=semi-major/minor axes in Z	real	4		-0.9999995e9	src.ellipticity
zEll	vikingSource	VIKINGDR3	1-b/a, where a/b=semi-major/minor axes in Z	real	4		-0.9999995e9	src.ellipticity
zEll	vikingSource	VIKINGDR4	1-b/a, where a/b=semi-major/minor axes in Z	real	4		-0.9999995e9	src.ellipticity;em.opt.I
zEll	vikingSource	VIKINGv20111019	1-b/a, where a/b=semi-major/minor axes in Z	real	4		-0.9999995e9	src.ellipticity
zEll	vikingSource	VIKINGv20130417	1-b/a, where a/b=semi-major/minor axes in Z	real	4		-0.9999995e9	src.ellipticity
zEll	vikingSource	VIKINGv20140402	1-b/a, where a/b=semi-major/minor axes in Z	real	4		-0.9999995e9	src.ellipticity
zEll	vikingSource	VIKINGv20150421	1-b/a, where a/b=semi-major/minor axes in Z	real	4		-0.9999995e9	src.ellipticity;em.opt.I
zEll	vikingSource	VIKINGv20151230	1-b/a, where a/b=semi-major/minor axes in Z	real	4		-0.9999995e9	src.ellipticity;em.opt.I
zEll	vikingSource	VIKINGv20160406	1-b/a, where a/b=semi-major/minor axes in Z	real	4		-0.9999995e9	src.ellipticity;em.opt.I
zEll	vikingSource	VIKINGv20161202	1-b/a, where a/b=semi-major/minor axes in Z	real	4		-0.9999995e9	src.ellipticity;em.opt.I
zEll	vikingSource	VIKINGv20170715	1-b/a, where a/b=semi-major/minor axes in Z	real	4		-0.9999995e9	src.ellipticity;em.opt.I
zEll	vikingSource, vikingSourceRemeasurement	VIKINGv20110714	1-b/a, where a/b=semi-major/minor axes in Z	real	4		-0.9999995e9	src.ellipticity
zEll	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	1-b/a, where a/b=semi-major/minor axes in Z	real	4		-0.9999995e9	src.ellipticity
zEll	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	1-b/a, where a/b=semi-major/minor axes in Z	real	4		-0.9999995e9	src.ellipticity
zEll	vvvSource	VVVDR2	1-b/a, where a/b=semi-major/minor axes in Z	real	4		-0.9999995e9	src.ellipticity
zEll	vvvSource	VVVDR5	1-b/a, where a/b=semi-major/minor axes in Z	real	4		-0.9999995e9	src.ellipticity;em.opt.I
zEll	vvvSource	VVVv20110718	1-b/a, where a/b=semi-major/minor axes in Z	real	4		-0.9999995e9	src.ellipticity
zEll	vvvSource, vvvSourceRemeasurement	VVVv20100531	1-b/a, where a/b=semi-major/minor axes in Z	real	4		-0.9999995e9	src.ellipticity
zEll	vvvSource, vvvSynopticSource	VVVDR1	1-b/a, where a/b=semi-major/minor axes in Z	real	4		-0.9999995e9	src.ellipticity
ZEMIBESTERR	spectra	SIXDF	error on the selected emission line redshift, 0.0 if not measured	real	4
zeNum	videoMergeLog	VIDEODR2	the extension number of this Z frame	tinyint	1			meta.number
zeNum	videoMergeLog	VIDEODR3	the extension number of this Z frame	tinyint	1			meta.number
zeNum	videoMergeLog	VIDEODR4	the extension number of this Z frame	tinyint	1			meta.number;em.opt.I
zeNum	videoMergeLog	VIDEODR5	the extension number of this Z frame	tinyint	1			meta.number;em.opt.I
zeNum	videoMergeLog	VIDEOv20100513	the extension number of this Z frame	tinyint	1			meta.number
zeNum	videoMergeLog	VIDEOv20111208	the extension number of this Z frame	tinyint	1			meta.number
zeNum	vikingMergeLog	VIKINGDR2	the extension number of this Z frame	tinyint	1			meta.number
zeNum	vikingMergeLog	VIKINGDR3	the extension number of this Z frame	tinyint	1			meta.number
zeNum	vikingMergeLog	VIKINGDR4	the extension number of this Z frame	tinyint	1			meta.number;em.opt.I
zeNum	vikingMergeLog	VIKINGv20110714	the extension number of this Z frame	tinyint	1			meta.number
zeNum	vikingMergeLog	VIKINGv20111019	the extension number of this Z frame	tinyint	1			meta.number
zeNum	vikingMergeLog	VIKINGv20130417	the extension number of this Z frame	tinyint	1			meta.number
zeNum	vikingMergeLog	VIKINGv20140402	the extension number of this Z frame	tinyint	1			meta.number
zeNum	vikingMergeLog	VIKINGv20150421	the extension number of this Z frame	tinyint	1			meta.number;em.opt.I
zeNum	vikingMergeLog	VIKINGv20151230	the extension number of this Z frame	tinyint	1			meta.number;em.opt.I
zeNum	vikingMergeLog	VIKINGv20160406	the extension number of this Z frame	tinyint	1			meta.number;em.opt.I
zeNum	vikingMergeLog	VIKINGv20161202	the extension number of this Z frame	tinyint	1			meta.number;em.opt.I
zeNum	vikingMergeLog	VIKINGv20170715	the extension number of this Z frame	tinyint	1			meta.number;em.opt.I
zeNum	vikingZY_selJ_RemeasMergeLog	VIKINGZYSELJv20160909	the extension number of this Z frame	tinyint	1			meta.number
zeNum	vikingZY_selJ_RemeasMergeLog	VIKINGZYSELJv20170124	the extension number of this Z frame	tinyint	1			meta.number
zeNum	vvvMergeLog	VVVDR2	the extension number of this Z frame	tinyint	1			meta.number
zeNum	vvvMergeLog	VVVDR5	the extension number of this Z frame	tinyint	1			meta.number;em.opt.I
zeNum	vvvMergeLog	VVVv20100531	the extension number of this Z frame	tinyint	1			meta.number
zeNum	vvvMergeLog	VVVv20110718	the extension number of this Z frame	tinyint	1			meta.number
zeNum	vvvMergeLog, vvvSynopticMergeLog	VVVDR1	the extension number of this Z frame	tinyint	1			meta.number
zEpoch	StackObjectThin	PS1DR2	Modified Julian Date of the mean epoch of images contributing to the the z-band stack (equinox J2000).	float	8	days	-999
zeroPoint	ExternalProduct	SHARKSv20210222	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	SHARKSv20210421	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	ULTRAVISTADR4	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VHSDR3	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VHSDR4	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VHSDR5	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VHSDR6	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VHSv20150108	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VHSv20160114	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VHSv20160507	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VHSv20170630	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VHSv20180419	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VHSv20201209	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VHSv20231101	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VIDEODR4	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VIDEODR5	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VIDEOv20111208	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VIKINGDR4	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VIKINGv20150421	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VIKINGv20151230	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VIKINGv20160406	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VIKINGv20161202	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VIKINGv20170715	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VMCDEEPv20230713	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VMCDR3	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VMCDR4	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VMCDR5	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VMCv20140428	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VMCv20140903	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VMCv20150309	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VMCv20151218	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VMCv20160311	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VMCv20160822	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VMCv20170109	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VMCv20170411	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VMCv20171101	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VMCv20180702	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VMCv20181120	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VMCv20191212	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VMCv20210708	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VMCv20230816	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VMCv20240226	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VVVDR5	Zeropoint of each product	real	4		-0.9999995e9
zeroPoint	ExternalProduct	VVVXDR1	Zeropoint of each product	real	4		-0.9999995e9
zeropoint	RequiredMosaicTopLevel	SHARKSv20210222	Zeropoint of each product	real	4		-0.9999995e9
zeropoint	RequiredMosaicTopLevel	SHARKSv20210421	Zeropoint of each product	real	4		-0.9999995e9
zeropoint	RequiredMosaicTopLevel	ULTRAVISTADR4	Zeropoint of each product	real	4		-0.9999995e9
zeropoint	RequiredMosaicTopLevel	VHSv20201209	Zeropoint of each product	real	4		-0.9999995e9
zeropoint	RequiredMosaicTopLevel	VHSv20231101	Zeropoint of each product	real	4		-0.9999995e9
zeropoint	RequiredMosaicTopLevel	VMCDEEPv20230713	Zeropoint of each product	real	4		-0.9999995e9
zeropoint	RequiredMosaicTopLevel	VMCDR5	Zeropoint of each product	real	4		-0.9999995e9
zeropoint	RequiredMosaicTopLevel	VMCv20191212	Zeropoint of each product	real	4		-0.9999995e9
zeropoint	RequiredMosaicTopLevel	VMCv20210708	Zeropoint of each product	real	4		-0.9999995e9
zeropoint	RequiredMosaicTopLevel	VMCv20230816	Zeropoint of each product	real	4		-0.9999995e9
zeropoint	RequiredMosaicTopLevel	VMCv20240226	Zeropoint of each product	real	4		-0.9999995e9
zeropoint	RequiredMosaicTopLevel	VVVDR5	Zeropoint of each product	real	4		-0.9999995e9
zeropoint	RequiredMosaicTopLevel	VVVXDR1	Zeropoint of each product	real	4		-0.9999995e9
zerr	decapsSource	DECAPS	Uncertainty in mean z-band flux (statistical only) {catalogue TType keyword: err[4]}	real	4	3631Jy	-9.999995e8	stat.error;phot.flux;em.opt.I
zerr	smashdr2_deep, smashdr2_object	SMASH	Uncertainty in calibrated z-band magnitude	real	4
zerr_lbs	decapsSource	DECAPS	Uncertainty in mean local background subtracted z-band flux (statistical only) {catalogue TType keyword: err_lbs[4]}	real	4	3631Jy	-9.999995e8	stat.error;phot.flux;em.opt.I
zErrBits	videoSource	VIDEODR2	processing warning/error bitwise flags in Z	int	4		-99999999	meta.code
			This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows: Bit Flag Meaning 1 The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected). 2 The object was originally blended with another 4 At least one pixel is saturated (or very close to) 8 The object is truncated (too close to an image boundary) 16 Object's aperture data are incomplete or corrupted 32 Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters. 64 Memory overflow occurred during deblending 128 Memory overflow occurred during extraction
zErrBits	videoSource	VIDEODR3	processing warning/error bitwise flags in Z	int	4		-99999999	meta.code
			This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows: Bit Flag Meaning 1 The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected). 2 The object was originally blended with another 4 At least one pixel is saturated (or very close to) 8 The object is truncated (too close to an image boundary) 16 Object's aperture data are incomplete or corrupted 32 Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters. 64 Memory overflow occurred during deblending 128 Memory overflow occurred during extraction
zErrBits	videoSource	VIDEODR4	processing warning/error bitwise flags in Z	int	4		-99999999	meta.code;em.opt.I
			This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows: Bit Flag Meaning 1 The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected). 2 The object was originally blended with another 4 At least one pixel is saturated (or very close to) 8 The object is truncated (too close to an image boundary) 16 Object's aperture data are incomplete or corrupted 32 Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters. 64 Memory overflow occurred during deblending 128 Memory overflow occurred during extraction
zErrBits	videoSource	VIDEODR5	processing warning/error bitwise flags in Z	int	4		-99999999	meta.code;em.opt.I
			This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows: Bit Flag Meaning 1 The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected). 2 The object was originally blended with another 4 At least one pixel is saturated (or very close to) 8 The object is truncated (too close to an image boundary) 16 Object's aperture data are incomplete or corrupted 32 Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters. 64 Memory overflow occurred during deblending 128 Memory overflow occurred during extraction
zErrBits	videoSource	VIDEOv20100513	processing warning/error bitwise flags in Z	int	4		-99999999	meta.code
			This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows: Bit Flag Meaning 1 The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected). 2 The object was originally blended with another 4 At least one pixel is saturated (or very close to) 8 The object is truncated (too close to an image boundary) 16 Object's aperture data are incomplete or corrupted 32 Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters. 64 Memory overflow occurred during deblending 128 Memory overflow occurred during extraction
zErrBits	videoSource	VIDEOv20111208	processing warning/error bitwise flags in Z	int	4		-99999999	meta.code
			This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows: Bit Flag Meaning 1 The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected). 2 The object was originally blended with another 4 At least one pixel is saturated (or very close to) 8 The object is truncated (too close to an image boundary) 16 Object's aperture data are incomplete or corrupted 32 Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters. 64 Memory overflow occurred during deblending 128 Memory overflow occurred during extraction
zErrBits	videoSourceRemeasurement	VIDEOv20100513	processing warning/error bitwise flags in Z	int	4		-99999999	meta.code
zErrBits	vikingSource	VIKINGDR2	processing warning/error bitwise flags in Z	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.
zErrBits	vikingSource	VIKINGDR3	processing warning/error bitwise flags in Z	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.
zErrBits	vikingSource	VIKINGDR4	processing warning/error bitwise flags in Z	int	4		-99999999	meta.code;em.opt.I
			Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
zErrBits	vikingSource	VIKINGv20110714	processing warning/error bitwise flags in Z	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.
zErrBits	vikingSource	VIKINGv20111019	processing warning/error bitwise flags in Z	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.
zErrBits	vikingSource	VIKINGv20130417	processing warning/error bitwise flags in Z	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.
zErrBits	vikingSource	VIKINGv20140402	processing warning/error bitwise flags in Z	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.
zErrBits	vikingSource	VIKINGv20150421	processing warning/error bitwise flags in Z	int	4		-99999999	meta.code;em.opt.I
			Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
zErrBits	vikingSource	VIKINGv20151230	processing warning/error bitwise flags in Z	int	4		-99999999	meta.code;em.opt.I
			Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
zErrBits	vikingSource	VIKINGv20160406	processing warning/error bitwise flags in Z	int	4		-99999999	meta.code;em.opt.I
			Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
zErrBits	vikingSource	VIKINGv20161202	processing warning/error bitwise flags in Z	int	4		-99999999	meta.code;em.opt.I
			Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
zErrBits	vikingSource	VIKINGv20170715	processing warning/error bitwise flags in Z	int	4		-99999999	meta.code;em.opt.I
			Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
zErrBits	vikingSourceRemeasurement	VIKINGv20110714	processing warning/error bitwise flags in Z	int	4		-99999999	meta.code
zErrBits	vikingSourceRemeasurement	VIKINGv20111019	processing warning/error bitwise flags in Z	int	4		-99999999	meta.code
zErrBits	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	processing warning/error bitwise flags in Z	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.
zErrBits	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	processing warning/error bitwise flags in Z	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.
zErrBits	vvvSource	VVVDR2	processing warning/error bitwise flags in Z	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.
zErrBits	vvvSource	VVVDR5	processing warning/error bitwise flags in Z	int	4		-99999999	meta.code;em.opt.I
			Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
zErrBits	vvvSource	VVVv20100531	processing warning/error bitwise flags in Z	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.
zErrBits	vvvSource	VVVv20110718	processing warning/error bitwise flags in Z	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.
zErrBits	vvvSource, vvvSynopticSource	VVVDR1	processing warning/error bitwise flags in Z	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.
zErrBits	vvvSourceRemeasurement	VVVv20100531	processing warning/error bitwise flags in Z	int	4		-99999999	meta.code
zErrBits	vvvSourceRemeasurement	VVVv20110718	processing warning/error bitwise flags in Z	int	4		-99999999	meta.code
zEta	videoSource	VIDEODR2	Offset of Z 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.
zEta	videoSource	VIDEODR3	Offset of Z 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.
zEta	videoSource	VIDEODR4	Offset of Z detection from master position (+north/-south)	real	4	arcsec	-0.9999995e9	pos.eq.dec;arith.diff;em.opt.I
			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.
zEta	videoSource	VIDEODR5	Offset of Z detection from master position (+north/-south)	real	4	arcsec	-0.9999995e9	pos.eq.dec;arith.diff;em.opt.I
			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.
zEta	videoSource	VIDEOv20100513	Offset of Z 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.
zEta	videoSource	VIDEOv20111208	Offset of Z 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.
zEta	vikingSource	VIKINGDR2	Offset of Z 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.
zEta	vikingSource	VIKINGDR3	Offset of Z 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.
zEta	vikingSource	VIKINGDR4	Offset of Z detection from master position (+north/-south)	real	4	arcsec	-0.9999995e9	pos.eq.dec;arith.diff;em.opt.I
			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.
zEta	vikingSource	VIKINGv20110714	Offset of Z 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.
zEta	vikingSource	VIKINGv20111019	Offset of Z 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.
zEta	vikingSource	VIKINGv20130417	Offset of Z 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.
zEta	vikingSource	VIKINGv20140402	Offset of Z 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.
zEta	vikingSource	VIKINGv20150421	Offset of Z detection from master position (+north/-south)	real	4	arcsec	-0.9999995e9	pos.eq.dec;arith.diff;em.opt.I
			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.
zEta	vikingSource	VIKINGv20151230	Offset of Z detection from master position (+north/-south)	real	4	arcsec	-0.9999995e9	pos.eq.dec;arith.diff;em.opt.I
			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.
zEta	vikingSource	VIKINGv20160406	Offset of Z detection from master position (+north/-south)	real	4	arcsec	-0.9999995e9	pos.eq.dec;arith.diff;em.opt.I
			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.
zEta	vikingSource	VIKINGv20161202	Offset of Z detection from master position (+north/-south)	real	4	arcsec	-0.9999995e9	pos.eq.dec;arith.diff;em.opt.I
			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.
zEta	vikingSource	VIKINGv20170715	Offset of Z detection from master position (+north/-south)	real	4	arcsec	-0.9999995e9	pos.eq.dec;arith.diff;em.opt.I
			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.
zEta	vvvSource	VVVDR2	Offset of Z 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.
zEta	vvvSource	VVVDR5	Offset of Z detection from master position (+north/-south)	real	4	arcsec	-0.9999995e9	pos.eq.dec;arith.diff;em.opt.I
			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.
zEta	vvvSource	VVVv20100531	Offset of Z 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.
zEta	vvvSource	VVVv20110718	Offset of Z 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.
zEta	vvvSource, vvvSynopticSource	VVVDR1	Offset of Z 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.
zexpML	videoVarFrameSetInfo	VIDEODR2	Expected magnitude limit of frameSet in this in Z band.	real	4		-0.9999995e9
zexpML	videoVarFrameSetInfo	VIDEODR3	Expected magnitude limit of frameSet in this in Z band.	real	4		-0.9999995e9	phot.mag;stat.max;em.IR.NIR
zexpML	videoVarFrameSetInfo	VIDEODR4	Expected magnitude limit of frameSet in this in Z band.	real	4	mag	-0.9999995e9	phot.mag;em.opt.I;stat.max
zexpML	videoVarFrameSetInfo	VIDEODR5	Expected magnitude limit of frameSet in this in Z band.	real	4	mag	-0.9999995e9	phot.mag;em.opt.I;stat.max
zexpML	videoVarFrameSetInfo	VIDEOv20111208	Expected magnitude limit of frameSet in this in Z band.	real	4		-0.9999995e9
zexpML	vikingVarFrameSetInfo	VIKINGv20110714	Expected magnitude limit of frameSet in this in Z band.	real	4		-0.9999995e9
zexpML	vvvVarFrameSetInfo	VVVDR5	Expected magnitude limit of frameSet in this in Z band.	real	4	mag	-0.9999995e9	phot.mag;em.opt.I;stat.max
zExpRms	videoVariability	VIDEODR2	Rms calculated from polynomial fit to modal RMS as a function of magnitude in Z band	real	4	mag	-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zExpRms	videoVariability	VIDEODR3	Rms calculated from polynomial fit to modal RMS as a function of magnitude in Z band	real	4	mag	-0.9999995e9	stat.error;em.IR.NIR
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zExpRms	videoVariability	VIDEODR4	Rms calculated from polynomial fit to modal RMS as a function of magnitude in Z band	real	4	mag	-0.9999995e9	stat.error;em.opt.I
			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.
zExpRms	videoVariability	VIDEODR5	Rms calculated from polynomial fit to modal RMS as a function of magnitude in Z band	real	4	mag	-0.9999995e9	stat.error;em.opt.I
			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.
zExpRms	videoVariability	VIDEOv20111208	Rms calculated from polynomial fit to modal RMS as a function of magnitude in Z band	real	4	mag	-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zExpRms	vikingVariability	VIKINGv20110714	Rms calculated from polynomial fit to modal RMS as a function of magnitude in Z band	real	4	mag	-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zExpRms	vvvVariability	VVVDR5	Rms calculated from polynomial fit to modal RMS as a function of magnitude in Z band	real	4	mag	-0.9999995e9	stat.error;em.opt.I
			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.
zexpTime	StackObjectAttributes	PS1DR2	Exposure time of the z filter stack. Necessary for converting listed fluxes and magnitudes back to measured ADU counts.	real	4	seconds	-999
zExtNSigma	StackObjectAttributes	PS1DR2	An extendedness measure for the z filter stack detection based on the deviation between PSF and Kron (1980) magnitudes, normalized by the PSF magnitude uncertainty.	real	4		-999
ZFINALERR	spectra	SIXDF	error on final quoted redshift, 0.0 if not measured	real	4
zFlags	MeanObject	PS1DR2	Information flag bitmask for mean object from z filter detections. Values listed in ObjectFilterFlags.	int	4		0
zfracflux	decapsSource	DECAPS	PSF-weighted fraction of z-band flux coming from this object (i.e., one minus the the fraction of flux in this object's PSF that comes from neighbouring objects?) {catalogue TType keyword: fracflux[4]}	real	4		-9.999995e8	stat.value;em.opt.I
zGausig	videoSource	VIDEODR2	RMS of axes of ellipse fit in Z	real	4	pixels	-0.9999995e9	src.morph.param
zGausig	videoSource	VIDEODR3	RMS of axes of ellipse fit in Z	real	4	pixels	-0.9999995e9	src.morph.param
zGausig	videoSource	VIDEODR4	RMS of axes of ellipse fit in Z	real	4	pixels	-0.9999995e9	src.morph.param;em.opt.I
zGausig	videoSource	VIDEODR5	RMS of axes of ellipse fit in Z	real	4	pixels	-0.9999995e9	src.morph.param;em.opt.I
zGausig	videoSource	VIDEOv20111208	RMS of axes of ellipse fit in Z	real	4	pixels	-0.9999995e9	src.morph.param
zGausig	videoSource, videoSourceRemeasurement	VIDEOv20100513	RMS of axes of ellipse fit in Z	real	4	pixels	-0.9999995e9	src.morph.param
zGausig	vikingSource	VIKINGDR2	RMS of axes of ellipse fit in Z	real	4	pixels	-0.9999995e9	src.morph.param
zGausig	vikingSource	VIKINGDR3	RMS of axes of ellipse fit in Z	real	4	pixels	-0.9999995e9	src.morph.param
zGausig	vikingSource	VIKINGDR4	RMS of axes of ellipse fit in Z	real	4	pixels	-0.9999995e9	src.morph.param;em.opt.I
zGausig	vikingSource	VIKINGv20111019	RMS of axes of ellipse fit in Z	real	4	pixels	-0.9999995e9	src.morph.param
zGausig	vikingSource	VIKINGv20130417	RMS of axes of ellipse fit in Z	real	4	pixels	-0.9999995e9	src.morph.param
zGausig	vikingSource	VIKINGv20140402	RMS of axes of ellipse fit in Z	real	4	pixels	-0.9999995e9	src.morph.param
zGausig	vikingSource	VIKINGv20150421	RMS of axes of ellipse fit in Z	real	4	pixels	-0.9999995e9	src.morph.param;em.opt.I
zGausig	vikingSource	VIKINGv20151230	RMS of axes of ellipse fit in Z	real	4	pixels	-0.9999995e9	src.morph.param;em.opt.I
zGausig	vikingSource	VIKINGv20160406	RMS of axes of ellipse fit in Z	real	4	pixels	-0.9999995e9	src.morph.param;em.opt.I
zGausig	vikingSource	VIKINGv20161202	RMS of axes of ellipse fit in Z	real	4	pixels	-0.9999995e9	src.morph.param;em.opt.I
zGausig	vikingSource	VIKINGv20170715	RMS of axes of ellipse fit in Z	real	4	pixels	-0.9999995e9	src.morph.param;em.opt.I
zGausig	vikingSource, vikingSourceRemeasurement	VIKINGv20110714	RMS of axes of ellipse fit in Z	real	4	pixels	-0.9999995e9	src.morph.param
zGausig	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	RMS of axes of ellipse fit in Z	real	4	pixels	-0.9999995e9	src.morph.param
zGausig	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	RMS of axes of ellipse fit in Z	real	4	pixels	-0.9999995e9	src.morph.param
zGausig	vvvSource	VVVDR2	RMS of axes of ellipse fit in Z	real	4	pixels	-0.9999995e9	src.morph.param
zGausig	vvvSource	VVVDR5	RMS of axes of ellipse fit in Z	real	4	pixels	-0.9999995e9	src.morph.param;em.opt.I
zGausig	vvvSource	VVVv20110718	RMS of axes of ellipse fit in Z	real	4	pixels	-0.9999995e9	src.morph.param
zGausig	vvvSource, vvvSourceRemeasurement	VVVv20100531	RMS of axes of ellipse fit in Z	real	4	pixels	-0.9999995e9	src.morph.param
zGausig	vvvSource, vvvSynopticSource	VVVDR1	RMS of axes of ellipse fit in Z	real	4	pixels	-0.9999995e9	src.morph.param
zHalfRad	videoSource	VIDEODR4	SExtractor half-light radius in Z band	real	4	pixels	-0.9999995e9	phys.angSize;em.opt.I
zHalfRad	videoSource	VIDEODR5	SExtractor half-light radius in Z band	real	4	pixels	-0.9999995e9	phys.angSize;em.opt.I
zHlCorSMjRadAs	videoSource	VIDEODR2	Seeing corrected half-light, semi-major axis in Z band	real	4	arcsec	-0.9999995e9	phys.angSize;src
zHlCorSMjRadAs	videoSource	VIDEODR3	Seeing corrected half-light, semi-major axis in Z band	real	4	arcsec	-0.9999995e9	phys.angSize
zHlCorSMjRadAs	videoSource	VIDEODR4	Seeing corrected half-light, semi-major axis in Z band	real	4	arcsec	-0.9999995e9	phys.angSize;em.opt.I
zHlCorSMjRadAs	videoSource	VIDEODR5	Seeing corrected half-light, semi-major axis in Z band	real	4	arcsec	-0.9999995e9	phys.angSize;em.opt.I
zHlCorSMjRadAs	videoSource	VIDEOv20100513	Seeing corrected half-light, semi-major axis in Z band	real	4	arcsec	-0.9999995e9	phys.angSize;src
zHlCorSMjRadAs	videoSource	VIDEOv20111208	Seeing corrected half-light, semi-major axis in Z band	real	4	arcsec	-0.9999995e9	phys.angSize;src
zHlCorSMjRadAs	vikingSource	VIKINGDR2	Seeing corrected half-light, semi-major axis in Z band	real	4	arcsec	-0.9999995e9	phys.angSize;src
zHlCorSMjRadAs	vikingSource	VIKINGDR3	Seeing corrected half-light, semi-major axis in Z band	real	4	arcsec	-0.9999995e9	phys.angSize
zHlCorSMjRadAs	vikingSource	VIKINGDR4	Seeing corrected half-light, semi-major axis in Z band	real	4	arcsec	-0.9999995e9	phys.angSize;em.opt.I
zHlCorSMjRadAs	vikingSource	VIKINGv20110714	Seeing corrected half-light, semi-major axis in Z band	real	4	arcsec	-0.9999995e9	phys.angSize;src
zHlCorSMjRadAs	vikingSource	VIKINGv20111019	Seeing corrected half-light, semi-major axis in Z band	real	4	arcsec	-0.9999995e9	phys.angSize;src
zHlCorSMjRadAs	vikingSource	VIKINGv20130417	Seeing corrected half-light, semi-major axis in Z band	real	4	arcsec	-0.9999995e9	phys.angSize
zHlCorSMjRadAs	vikingSource	VIKINGv20140402	Seeing corrected half-light, semi-major axis in Z band	real	4	arcsec	-0.9999995e9	phys.angSize
zHlCorSMjRadAs	vikingSource	VIKINGv20150421	Seeing corrected half-light, semi-major axis in Z band	real	4	arcsec	-0.9999995e9	phys.angSize;em.opt.I
zHlCorSMjRadAs	vikingSource	VIKINGv20151230	Seeing corrected half-light, semi-major axis in Z band	real	4	arcsec	-0.9999995e9	phys.angSize;em.opt.I
zHlCorSMjRadAs	vikingSource	VIKINGv20160406	Seeing corrected half-light, semi-major axis in Z band	real	4	arcsec	-0.9999995e9	phys.angSize;em.opt.I
zHlCorSMjRadAs	vikingSource	VIKINGv20161202	Seeing corrected half-light, semi-major axis in Z band	real	4	arcsec	-0.9999995e9	phys.angSize;em.opt.I
zHlCorSMjRadAs	vikingSource	VIKINGv20170715	Seeing corrected half-light, semi-major axis in Z band	real	4	arcsec	-0.9999995e9	phys.angSize;em.opt.I
zinfoFlag	StackObjectThin	PS1DR2	Information flag bitmask indicating details of the z filter stack photometry. Values listed in DetectionFlags.	bigint	8		0
zinfoFlag2	StackObjectThin	PS1DR2	Information flag bitmask indicating details of the z filter stack photometry. Values listed in DetectionFlags2.	int	4		0
zinfoFlag3	StackObjectThin	PS1DR2	Information flag bitmask indicating details of the z filter stack photometry. Values listed in DetectionFlags3.	int	4		0
zIntRms	videoVariability	VIDEODR2	Intrinsic rms in Z-band	real	4	mag	-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zIntRms	videoVariability	VIDEODR3	Intrinsic rms in Z-band	real	4	mag	-0.9999995e9	stat.error;em.IR.NIR
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zIntRms	videoVariability	VIDEODR4	Intrinsic rms in Z-band	real	4	mag	-0.9999995e9	stat.error;em.opt.I
			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.
zIntRms	videoVariability	VIDEODR5	Intrinsic rms in Z-band	real	4	mag	-0.9999995e9	stat.error;em.opt.I
			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.
zIntRms	videoVariability	VIDEOv20111208	Intrinsic rms in Z-band	real	4	mag	-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zIntRms	vikingVariability	VIKINGv20110714	Intrinsic rms in Z-band	real	4	mag	-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zIntRms	vvvVariability	VVVDR5	Intrinsic rms in Z-band	real	4	mag	-0.9999995e9	stat.error;em.opt.I
			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.
zippDetectID	StackObjectAttributes, StackObjectThin	PS1DR2	IPP internal detection identifier.	bigint	8
zisDefAst	videoVarFrameSetInfo	VIDEODR2	Use a default model for the astrometric noise in Z band.	tinyint	1		0
zisDefAst	videoVarFrameSetInfo	VIDEODR3	Use a default model for the astrometric noise in Z band.	tinyint	1		0	meta.code;em.IR.NIR
zisDefAst	videoVarFrameSetInfo	VIDEODR4	Use a default model for the astrometric noise in Z band.	tinyint	1		0	meta.code;em.opt.I
zisDefAst	videoVarFrameSetInfo	VIDEODR5	Use a default model for the astrometric noise in Z band.	tinyint	1		0	meta.code;em.opt.I
zisDefAst	videoVarFrameSetInfo	VIDEOv20111208	Use a default model for the astrometric noise in Z band.	tinyint	1		0
zisDefAst	vvvVarFrameSetInfo	VVVDR5	Use a default model for the astrometric noise in Z band.	tinyint	1		0	meta.code;em.opt.I
zisDefPht	videoVarFrameSetInfo	VIDEODR2	Use a default model for the photometric noise in Z band.	tinyint	1		0
zisDefPht	videoVarFrameSetInfo	VIDEODR3	Use a default model for the photometric noise in Z band.	tinyint	1		0	meta.code;em.IR.NIR
zisDefPht	videoVarFrameSetInfo	VIDEODR4	Use a default model for the photometric noise in Z band.	tinyint	1		0	meta.code;em.opt.I
zisDefPht	videoVarFrameSetInfo	VIDEODR5	Use a default model for the photometric noise in Z band.	tinyint	1		0	meta.code;em.opt.I
zisDefPht	videoVarFrameSetInfo	VIDEOv20111208	Use a default model for the photometric noise in Z band.	tinyint	1		0
zisDefPht	vvvVarFrameSetInfo	VVVDR5	Use a default model for the photometric noise in Z band.	tinyint	1		0	meta.code;em.opt.I
zIsMeas	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Is pass band Z measured? 0 no, 1 yes	tinyint	1		0	meta.code
zIsMeas	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Is pass band Z measured? 0 no, 1 yes	tinyint	1		0	meta.code
zKronFlux	StackObjectAttributes	PS1DR2	Kron (1980) flux from z filter stack detection.	real	4	Janskys	-999
zKronFluxErr	StackObjectAttributes	PS1DR2	Error in Kron (1980) flux from z filter stack detection.	real	4	Janskys	-999
zKronMag	StackObjectThin	PS1DR2	Kron (1980) magnitude from z filter stack detection.	real	4	AB magnitudes	-999
zKronMag	videoSource	VIDEODR4	Extended source Z mag (Kron - SExtractor MAG_AUTO)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zKronMag	videoSource	VIDEODR5	Extended source Z mag (Kron - SExtractor MAG_AUTO)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zKronMagErr	StackObjectThin	PS1DR2	Error in Kron (1980) magnitude from z filter stack detection.	real	4	AB magnitudes	-999
zKronMagErr	videoSource	VIDEODR4	Extended source Z mag error (Kron - SExtractor MAG_AUTO)	real	4	mag	-0.9999995e9	stat.error;em.opt.I;phot.mag
zKronMagErr	videoSource	VIDEODR5	Extended source Z mag error (Kron - SExtractor MAG_AUTO)	real	4	mag	-0.9999995e9	stat.error;em.opt.I;phot.mag
zKronRad	StackObjectAttributes	PS1DR2	Kron (1980) radius from z filter stack detection.	real	4	arcsec	-999
Zmag	vvvParallaxCatalogue, vvvProperMotionCatalogue	VVVDR5	VVV DR4 Z photometry {catalogue TType keyword: Zmag}	real	4	mag	-999999500.0
zMag	videoSourceRemeasurement	VIDEOv20100513	Z mag (as appropriate for this merged source)	real	4	mag	-0.9999995e9	phot.mag
zMag	vikingSourceRemeasurement	VIKINGv20110714	Z mag (as appropriate for this merged source)	real	4	mag	-0.9999995e9	phot.mag
zMag	vikingSourceRemeasurement	VIKINGv20111019	Z mag (as appropriate for this merged source)	real	4	mag	-0.9999995e9	phot.mag
zMag	vvvSourceRemeasurement	VVVv20100531	Z mag (as appropriate for this merged source)	real	4	mag	-0.9999995e9	phot.mag
zMag	vvvSourceRemeasurement	VVVv20110718	Z mag (as appropriate for this merged source)	real	4	mag	-0.9999995e9	phot.mag
zmag	smashdr2_deep, smashdr2_object	SMASH	Weighted-avarege, calibrated z-band magnitude, 99.99 if no detection	real	4
zMagErr	videoSourceRemeasurement	VIDEOv20100513	Error in Z mag	real	4	mag	-0.9999995e9	stat.error
zMagErr	vikingSourceRemeasurement	VIKINGv20110714	Error in Z mag	real	4	mag	-0.9999995e9	stat.error
zMagErr	vikingSourceRemeasurement	VIKINGv20111019	Error in Z mag	real	4	mag	-0.9999995e9	stat.error
zMagErr	vvvSourceRemeasurement	VVVv20100531	Error in Z mag	real	4	mag	-0.9999995e9	stat.error
zMagErr	vvvSourceRemeasurement	VVVv20110718	Error in Z mag	real	4	mag	-0.9999995e9	stat.error
zmaglimit	decapsSource	DECAPS	5 sigma z-band magnitude limit for deepest detection of this object (AB mag) {catalogue TType keyword: maglimit[4]}	real	4	mag	-9.999995e8	phot.mag;em.opt.I
zMagMAD	videoVariability	VIDEODR2	Median Absolute Deviation of Z magnitude	real	4	mag	-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zMagMAD	videoVariability	VIDEODR3	Median Absolute Deviation of Z magnitude	real	4	mag	-0.9999995e9	stat.error;em.IR.NIR
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zMagMAD	videoVariability	VIDEODR4	Median Absolute Deviation of Z magnitude	real	4	mag	-0.9999995e9	stat.err;em.opt.I;phot.mag
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zMagMAD	videoVariability	VIDEODR5	Median Absolute Deviation of Z magnitude	real	4	mag	-0.9999995e9	stat.err;em.opt.I;phot.mag
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zMagMAD	videoVariability	VIDEOv20111208	Median Absolute Deviation of Z magnitude	real	4	mag	-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zMagMAD	vikingVariability	VIKINGv20110714	Median Absolute Deviation of Z magnitude	real	4	mag	-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zMagMAD	vvvVariability	VVVDR5	Median Absolute Deviation of Z magnitude	real	4	mag	-0.9999995e9	stat.err;em.opt.I;phot.mag
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zMagRms	videoVariability	VIDEODR2	rms of Z magnitude	real	4	mag	-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zMagRms	videoVariability	VIDEODR3	rms of Z magnitude	real	4	mag	-0.9999995e9	stat.error;em.IR.NIR
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zMagRms	videoVariability	VIDEODR4	rms of Z magnitude	real	4	mag	-0.9999995e9	stat.error;em.opt.I;phot.mag
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zMagRms	videoVariability	VIDEODR5	rms of Z magnitude	real	4	mag	-0.9999995e9	stat.error;em.opt.I;phot.mag
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zMagRms	videoVariability	VIDEOv20111208	rms of Z magnitude	real	4	mag	-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zMagRms	vikingVariability	VIKINGv20110714	rms of Z magnitude	real	4	mag	-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zMagRms	vvvVariability	VVVDR5	rms of Z magnitude	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.I
			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.
zmaxCadence	videoVariability	VIDEODR2	maximum gap between observations	real	4	days	-0.9999995e9
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
zmaxCadence	videoVariability	VIDEODR3	maximum gap between observations	real	4	days	-0.9999995e9	time.interval;obs;stat.max
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
zmaxCadence	videoVariability	VIDEODR4	maximum gap between observations	real	4	days	-0.9999995e9	time.interval;obs;stat.max
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
zmaxCadence	videoVariability	VIDEODR5	maximum gap between observations	real	4	days	-0.9999995e9	time.interval;obs;stat.max
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
zmaxCadence	videoVariability	VIDEOv20111208	maximum gap between observations	real	4	days	-0.9999995e9
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
zmaxCadence	vikingVariability	VIKINGv20110714	maximum gap between observations	real	4	days	-0.9999995e9
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
zmaxCadence	vvvVariability	VVVDR5	maximum gap between observations	real	4	days	-0.9999995e9	time.interval;obs;stat.max
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
zMaxMag	videoVariability	VIDEODR2	Maximum magnitude in Z band, of good detections	real	4		-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zMaxMag	videoVariability	VIDEODR3	Maximum magnitude in Z band, of good detections	real	4		-0.9999995e9	phot.mag;stat.max;em.IR.NIR
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zMaxMag	videoVariability	VIDEODR4	Maximum magnitude in Z band, of good detections	real	4	mag	-0.9999995e9	phot.mag;em.opt.I;stat.max
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zMaxMag	videoVariability	VIDEODR5	Maximum magnitude in Z band, of good detections	real	4	mag	-0.9999995e9	phot.mag;em.opt.I;stat.max
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zMaxMag	videoVariability	VIDEOv20111208	Maximum magnitude in Z band, of good detections	real	4		-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zMaxMag	vikingVariability	VIKINGv20110714	Maximum magnitude in Z band, of good detections	real	4		-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zMaxMag	vvvVariability	VVVDR5	Maximum magnitude in Z band, of good detections	real	4	mag	-0.9999995e9	phot.mag;em.opt.I;stat.max
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zmean	decapsSource	DECAPS	z-band mean flux, good detections only (3631 Jy) {catalogue TType keyword: mean[4]}	real	4	3631Jy		phot.flux;em.opt.I
zmean_lbs	decapsSource	DECAPS	Mean z-band flux, using a local background subtraction (3631 Jy) {catalogue TType keyword: mean_lbs[4]}	real	4	3631Jy	-9.999995e8	stat.mean;phot.flux;em.opt.I
zMeanApMag	MeanObject	PS1DR2	Mean aperture magnitude from z filter detections.	real	4	AB magnitudes	-999
zMeanApMagErr	MeanObject	PS1DR2	Error in mean aperture magnitude from z filter detections.	real	4	AB magnitudes	-999
zMeanApMagNpt	MeanObject	PS1DR2	Number of measurements included in mean aperture magnitude from z filter detections.	smallint	2		-999
zMeanApMagStd	MeanObject	PS1DR2	Standard deviation of aperture magnitudes from z filter detections.	real	4	AB magnitudes	-999
zMeanKronMag	MeanObject	PS1DR2	Mean Kron (1980) magnitude from z filter detections.	real	4	AB magnitudes	-999
zMeanKronMagErr	MeanObject	PS1DR2	Error in mean Kron (1980) magnitude from z filter detections.	real	4	AB magnitudes	-999
zMeanKronMagNpt	MeanObject	PS1DR2	Number of measurements included in mean Kron (1980) magnitude from z filter detections.	smallint	2		-999
zMeanKronMagStd	MeanObject	PS1DR2	Standard deviation of Kron (1980) magnitudes from z filter detections.	real	4	AB magnitudes	-999
zmeanMag	videoVariability	VIDEODR2	Mean Z magnitude	real	4	mag	-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zmeanMag	videoVariability	VIDEODR3	Mean Z magnitude	real	4	mag	-0.9999995e9	phot.mag;stat.mean;em.IR.NIR
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zmeanMag	videoVariability	VIDEODR4	Mean Z magnitude	real	4	mag	-0.9999995e9	phot.mag;em.opt.I;stat.mean;em.opt.I
			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.
zmeanMag	videoVariability	VIDEODR5	Mean Z magnitude	real	4	mag	-0.9999995e9	phot.mag;em.opt.I;stat.mean;em.opt.I
			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.
zmeanMag	videoVariability	VIDEOv20111208	Mean Z magnitude	real	4	mag	-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zmeanMag	vikingVariability	VIKINGv20110714	Mean Z magnitude	real	4	mag	-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zmeanMag	vvvVariability	VVVDR5	Mean Z magnitude	real	4	mag	-0.9999995e9	phot.mag;em.opt.I;stat.mean;em.opt.I
			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.
zMeanPSFMag	MeanObject	PS1DR2	Mean PSF magnitude from z filter detections.	real	4	AB magnitudes	-999
zMeanPSFMagErr	MeanObject	PS1DR2	Error in mean PSF magnitude from z filter detections.	real	4	AB magnitudes	-999
zMeanPSFMagMax	MeanObject	PS1DR2	Maximum PSF magnitude from z filter detections.	real	4	AB magnitudes	-999
zMeanPSFMagMin	MeanObject	PS1DR2	Minimum PSF magnitude from z filter detections.	real	4	AB magnitudes	-999
zMeanPSFMagNpt	MeanObject	PS1DR2	Number of measurements included in mean PSF magnitude from z filter detections.	smallint	2		-999
zMeanPSFMagStd	MeanObject	PS1DR2	Standard deviation of PSF magnitudes from z filter detections.	real	4	AB magnitudes	-999
Zmeas	vvvProperMotionCatalogue	VVVDR5	Is there a Z band measurment for this frame	tinyint	1
zmedCadence	videoVariability	VIDEODR2	median gap between observations	real	4	days	-0.9999995e9
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
zmedCadence	videoVariability	VIDEODR3	median gap between observations	real	4	days	-0.9999995e9	time.interval;obs;stat.median
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
zmedCadence	videoVariability	VIDEODR4	median gap between observations	real	4	days	-0.9999995e9	time.interval;obs;stat.median
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
zmedCadence	videoVariability	VIDEODR5	median gap between observations	real	4	days	-0.9999995e9	time.interval;obs;stat.median
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
zmedCadence	videoVariability	VIDEOv20111208	median gap between observations	real	4	days	-0.9999995e9
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
zmedCadence	vikingVariability	VIKINGv20110714	median gap between observations	real	4	days	-0.9999995e9
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
zmedCadence	vvvVariability	VVVDR5	median gap between observations	real	4	days	-0.9999995e9	time.interval;obs;stat.median
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
zmedian	decapsSource	DECAPS	Median z-band flux (3631 Jy) {catalogue TType keyword: median[4]}	real	4	3631Jy	-9.999995e8	stat.median;phot.flux;em.opt.I
zmedian_lbs	decapsSource	DECAPS	Median local background subtracted z-band flux (3631 Jy) {catalogue TType keyword: median_lbs[4]}	real	4	3631Jy	-9.999995e8	stat.median;phot.flux;em.opt.I
zmedianMag	videoVariability	VIDEODR2	Median Z magnitude	real	4	mag	-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zmedianMag	videoVariability	VIDEODR3	Median Z magnitude	real	4	mag	-0.9999995e9	phot.mag;stat.median;em.IR.NIR
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zmedianMag	videoVariability	VIDEODR4	Median Z magnitude	real	4	mag	-0.9999995e9	phot.mag;em.opt.I;stat.median;em.opt.I
			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.
zmedianMag	videoVariability	VIDEODR5	Median Z magnitude	real	4	mag	-0.9999995e9	phot.mag;em.opt.I;stat.median;em.opt.I
			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.
zmedianMag	videoVariability	VIDEOv20111208	Median Z magnitude	real	4	mag	-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zmedianMag	vikingVariability	VIKINGv20110714	Median Z magnitude	real	4	mag	-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zmedianMag	vvvVariability	VVVDR5	Median Z magnitude	real	4	mag	-0.9999995e9	phot.mag;em.opt.I;stat.median;em.opt.I
			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.
zmfID	videoMergeLog	VIDEODR2	the UID of the relevant Z multiframe	bigint	8			obs.field
zmfID	videoMergeLog	VIDEODR3	the UID of the relevant Z multiframe	bigint	8			meta.id;obs.field
zmfID	videoMergeLog	VIDEODR4	the UID of the relevant Z multiframe	bigint	8			meta.id;obs.field;em.opt.I
zmfID	videoMergeLog	VIDEODR5	the UID of the relevant Z multiframe	bigint	8			meta.id;obs.field;em.opt.I
zmfID	videoMergeLog	VIDEOv20100513	the UID of the relevant Z multiframe	bigint	8			obs.field
zmfID	videoMergeLog	VIDEOv20111208	the UID of the relevant Z multiframe	bigint	8			obs.field
zmfID	vikingMergeLog	VIKINGDR2	the UID of the relevant Z multiframe	bigint	8			obs.field
zmfID	vikingMergeLog	VIKINGDR3	the UID of the relevant Z multiframe	bigint	8			meta.id;obs.field
zmfID	vikingMergeLog	VIKINGDR4	the UID of the relevant Z multiframe	bigint	8			meta.id;obs.field;em.opt.I
zmfID	vikingMergeLog	VIKINGv20110714	the UID of the relevant Z multiframe	bigint	8			obs.field
zmfID	vikingMergeLog	VIKINGv20111019	the UID of the relevant Z multiframe	bigint	8			obs.field
zmfID	vikingMergeLog	VIKINGv20130417	the UID of the relevant Z multiframe	bigint	8			meta.id;obs.field
zmfID	vikingMergeLog	VIKINGv20140402	the UID of the relevant Z multiframe	bigint	8			meta.id;obs.field
zmfID	vikingMergeLog	VIKINGv20150421	the UID of the relevant Z multiframe	bigint	8			meta.id;obs.field;em.opt.I
zmfID	vikingMergeLog	VIKINGv20151230	the UID of the relevant Z multiframe	bigint	8			meta.id;obs.field;em.opt.I
zmfID	vikingMergeLog	VIKINGv20160406	the UID of the relevant Z multiframe	bigint	8			meta.id;obs.field;em.opt.I
zmfID	vikingMergeLog	VIKINGv20161202	the UID of the relevant Z multiframe	bigint	8			meta.id;obs.field;em.opt.I
zmfID	vikingMergeLog	VIKINGv20170715	the UID of the relevant Z multiframe	bigint	8			meta.id;obs.field;em.opt.I
zmfID	vikingZY_selJ_RemeasMergeLog	VIKINGZYSELJv20160909	the UID of the relevant Z multiframe	bigint	8			obs.field
zmfID	vikingZY_selJ_RemeasMergeLog	VIKINGZYSELJv20170124	the UID of the relevant Z multiframe	bigint	8			obs.field
zmfID	vvvMergeLog	VVVDR2	the UID of the relevant Z multiframe	bigint	8			meta.id;obs.field
zmfID	vvvMergeLog	VVVDR5	the UID of the relevant Z multiframe	bigint	8			meta.id;obs.field;em.opt.I
zmfID	vvvMergeLog	VVVv20100531	the UID of the relevant Z multiframe	bigint	8			obs.field
zmfID	vvvMergeLog	VVVv20110718	the UID of the relevant Z multiframe	bigint	8			obs.field
zmfID	vvvMergeLog, vvvSynopticMergeLog	VVVDR1	the UID of the relevant Z multiframe	bigint	8			meta.id;obs.field
zminCadence	videoVariability	VIDEODR2	minimum gap between observations	real	4	days	-0.9999995e9
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
zminCadence	videoVariability	VIDEODR3	minimum gap between observations	real	4	days	-0.9999995e9	time.interval;obs;stat.min
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
zminCadence	videoVariability	VIDEODR4	minimum gap between observations	real	4	days	-0.9999995e9	time.interval;obs;stat.min
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
zminCadence	videoVariability	VIDEODR5	minimum gap between observations	real	4	days	-0.9999995e9	time.interval;obs;stat.min
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
zminCadence	videoVariability	VIDEOv20111208	minimum gap between observations	real	4	days	-0.9999995e9
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
zminCadence	vikingVariability	VIKINGv20110714	minimum gap between observations	real	4	days	-0.9999995e9
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
zminCadence	vvvVariability	VVVDR5	minimum gap between observations	real	4	days	-0.9999995e9	time.interval;obs;stat.min
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
zMinMag	videoVariability	VIDEODR2	Minimum magnitude in Z band, of good detections	real	4		-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zMinMag	videoVariability	VIDEODR3	Minimum magnitude in Z band, of good detections	real	4		-0.9999995e9	phot.mag;stat.min;em.IR.NIR
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zMinMag	videoVariability	VIDEODR4	Minimum magnitude in Z band, of good detections	real	4	mag	-0.9999995e9	phot.mag;em.opt.I;stat.min
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zMinMag	videoVariability	VIDEODR5	Minimum magnitude in Z band, of good detections	real	4	mag	-0.9999995e9	phot.mag;em.opt.I;stat.min
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zMinMag	videoVariability	VIDEOv20111208	Minimum magnitude in Z band, of good detections	real	4		-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zMinMag	vikingVariability	VIKINGv20110714	Minimum magnitude in Z band, of good detections	real	4		-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zMinMag	vvvVariability	VVVDR5	Minimum magnitude in Z band, of good detections	real	4	mag	-0.9999995e9	phot.mag;em.opt.I;stat.min
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zMjd	vikingSource	VIKINGv20151230	Modified Julian Day in Z band	float	8	days	-0.9999995e9	time.epoch
zMjd	vikingSource	VIKINGv20160406	Modified Julian Day in Z band	float	8	days	-0.9999995e9	time.epoch
zMjd	vikingSource	VIKINGv20161202	Modified Julian Day in Z band	float	8	days	-0.9999995e9	time.epoch
zMjd	vikingSource	VIKINGv20170715	Modified Julian Day in Z band	float	8	days	-0.9999995e9	time.epoch
zMjd	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Modified Julian Day in Z band	float	8	days	-0.9999995e9	time.epoch
zMjd	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Modified Julian Day in Z band	float	8	days	-0.9999995e9	time.epoch
zMjd	vvvSource	VVVDR5	Modified Julian Day in Z band	float	8	days	-0.9999995e9	time.epoch;em.opt.I
zMjd	vvvSynopticSource	VVVDR1	Modified Julian Day in Z band	float	8	days	-0.9999995e9	time.epoch
zMjd	vvvSynopticSource	VVVDR2	Modified Julian Day in Z band	float	8	days	-0.9999995e9	time.epoch
zmomentR1	StackObjectAttributes	PS1DR2	First radial moment for z filter stack detection.	real	4	arcsec	-999
zmomentRH	StackObjectAttributes	PS1DR2	Half radial moment (r^0.5 weighting) for z filter stack detection.	real	4	arcsec^0.5	-999
zmomentXX	StackObjectAttributes	PS1DR2	Second moment M_xx for z filter stack detection.	real	4	arcsec^2	-999
zmomentXY	StackObjectAttributes	PS1DR2	Second moment M_xy for z filter stack detection.	real	4	arcsec^2	-999
zmomentYY	StackObjectAttributes	PS1DR2	Second moment M_yy for z filter stack detection.	real	4	arcsec^2	-999
zmy	videoSourceRemeasurement	VIDEOv20100513	Default colour Z-Y (using appropriate mags)	real	4	mag		PHOT_COLOR
zmy	vikingSourceRemeasurement	VIKINGv20110714	Default colour Z-Y (using appropriate mags)	real	4	mag		PHOT_COLOR
zmy	vikingSourceRemeasurement	VIKINGv20111019	Default colour Z-Y (using appropriate mags)	real	4	mag		PHOT_COLOR
zmy	vvvSourceRemeasurement	VVVv20100531	Default colour Z-Y (using appropriate mags)	real	4	mag		PHOT_COLOR
zmy	vvvSourceRemeasurement	VVVv20110718	Default colour Z-Y (using appropriate mags)	real	4	mag		PHOT_COLOR
zmyErr	videoSourceRemeasurement	VIDEOv20100513	Error on colour Z-Y	real	4	mag		stat.error
zmyErr	vikingSourceRemeasurement	VIKINGv20110714	Error on colour Z-Y	real	4	mag		stat.error
zmyErr	vikingSourceRemeasurement	VIKINGv20111019	Error on colour Z-Y	real	4	mag		stat.error
zmyErr	vvvSourceRemeasurement	VVVv20100531	Error on colour Z-Y	real	4	mag		stat.error
zmyErr	vvvSourceRemeasurement	VVVv20110718	Error on colour Z-Y	real	4	mag		stat.error
zmyExt	videoSource	VIDEODR2	Extended source colour Z-Y (using aperMagNoAperCorr3)	real	4	mag	-0.9999995e9	PHOT_COLOR
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyExt	videoSource	VIDEODR3	Extended source colour Z-Y (using aperMagNoAperCorr3)	real	4	mag	-0.9999995e9	phot.color
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyExt	videoSource	VIDEODR4	Extended source colour Z-Y (using aperMagNoAperCorr3)	real	4	mag	-0.9999995e9	phot.color;em.opt.I;em.IR.NIR
			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.
zmyExt	videoSource	VIDEODR5	Extended source colour Z-Y (using aperMagNoAperCorr3)	real	4	mag	-0.9999995e9	phot.color;em.opt.I;em.IR.NIR
			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.
zmyExt	videoSource	VIDEOv20100513	Extended source colour Z-Y (using aperMag3)	real	4	mag	-0.9999995e9	PHOT_COLOR
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyExt	videoSource	VIDEOv20111208	Extended source colour Z-Y (using aperMagNoAperCorr3)	real	4	mag	-0.9999995e9	PHOT_COLOR
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyExt	vikingSource	VIKINGDR2	Extended source colour Z-Y (using aperMagNoAperCorr3)	real	4	mag	-0.9999995e9	PHOT_COLOR
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyExt	vikingSource	VIKINGDR3	Extended source colour Z-Y (using aperMagNoAperCorr3)	real	4	mag	-0.9999995e9	phot.color
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyExt	vikingSource	VIKINGDR4	Extended source colour Z-Y (using aperMagNoAperCorr3)	real	4	mag	-0.9999995e9	phot.color;em.opt.I;em.IR.NIR
			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.
zmyExt	vikingSource	VIKINGv20110714	Extended source colour Z-Y (using aperMagNoAperCorr3)	real	4	mag	-0.9999995e9	PHOT_COLOR
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyExt	vikingSource	VIKINGv20111019	Extended source colour Z-Y (using aperMagNoAperCorr3)	real	4	mag	-0.9999995e9	PHOT_COLOR
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyExt	vikingSource	VIKINGv20130417	Extended source colour Z-Y (using aperMagNoAperCorr3)	real	4	mag	-0.9999995e9	phot.color
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyExt	vikingSource	VIKINGv20140402	Extended source colour Z-Y (using aperMagNoAperCorr3)	real	4	mag	-0.9999995e9	phot.color;em.opt.I;em.IR.NIR
			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.
zmyExt	vikingSource	VIKINGv20150421	Extended source colour Z-Y (using aperMagNoAperCorr3)	real	4	mag	-0.9999995e9	phot.color;em.opt.I;em.IR.NIR
			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.
zmyExt	vikingSource	VIKINGv20151230	Extended source colour Z-Y (using aperMagNoAperCorr3)	real	4	mag	-0.9999995e9	phot.color;em.opt.I;em.IR.NIR
			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.
zmyExt	vikingSource	VIKINGv20160406	Extended source colour Z-Y (using aperMagNoAperCorr3)	real	4	mag	-0.9999995e9	phot.color;em.opt.I;em.IR.NIR
			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.
zmyExt	vikingSource	VIKINGv20161202	Extended source colour Z-Y (using aperMagNoAperCorr3)	real	4	mag	-0.9999995e9	phot.color;em.opt.I;em.IR.NIR
			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.
zmyExt	vikingSource	VIKINGv20170715	Extended source colour Z-Y (using aperMagNoAperCorr3)	real	4	mag	-0.9999995e9	phot.color;em.opt.I;em.IR.NIR
			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.
zmyExt	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Extended source colour Z-Y (using aperMagNoAperCorr3)	real	4	mag	-0.9999995e9	phot.color
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyExt	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Extended source colour Z-Y (using aperMagNoAperCorr3)	real	4	mag	-0.9999995e9	phot.color
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyExt	vvvSource	VVVv20100531	Extended source colour Z-Y (using aperMag3)	real	4	mag	-0.9999995e9	PHOT_COLOR
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyExtErr	videoSource	VIDEODR2	Error on extended source colour Z-Y	real	4	mag	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyExtErr	videoSource	VIDEODR3	Error on extended source colour Z-Y	real	4	mag	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyExtErr	videoSource	VIDEODR4	Error on extended source colour Z-Y	real	4	mag	-0.9999995e9	stat.error;em.opt.I;em.IR.NIR
			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.
zmyExtErr	videoSource	VIDEODR5	Error on extended source colour Z-Y	real	4	mag	-0.9999995e9	stat.error;em.opt.I;em.IR.NIR
			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.
zmyExtErr	videoSource	VIDEOv20100513	Error on extended source colour Z-Y	real	4	mag	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyExtErr	videoSource	VIDEOv20111208	Error on extended source colour Z-Y	real	4	mag	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyExtErr	vikingSource	VIKINGDR2	Error on extended source colour Z-Y	real	4	mag	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyExtErr	vikingSource	VIKINGDR3	Error on extended source colour Z-Y	real	4	mag	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyExtErr	vikingSource	VIKINGDR4	Error on extended source colour Z-Y	real	4	mag	-0.9999995e9	stat.error;em.opt.I;em.IR.NIR
			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.
zmyExtErr	vikingSource	VIKINGv20110714	Error on extended source colour Z-Y	real	4	mag	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyExtErr	vikingSource	VIKINGv20111019	Error on extended source colour Z-Y	real	4	mag	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyExtErr	vikingSource	VIKINGv20130417	Error on extended source colour Z-Y	real	4	mag	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyExtErr	vikingSource	VIKINGv20140402	Error on extended source colour Z-Y	real	4	mag	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyExtErr	vikingSource	VIKINGv20150421	Error on extended source colour Z-Y	real	4	mag	-0.9999995e9	stat.error;em.opt.I;em.IR.NIR
			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.
zmyExtErr	vikingSource	VIKINGv20151230	Error on extended source colour Z-Y	real	4	mag	-0.9999995e9	stat.error;em.opt.I;em.IR.NIR
			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.
zmyExtErr	vikingSource	VIKINGv20160406	Error on extended source colour Z-Y	real	4	mag	-0.9999995e9	stat.error;em.opt.I;em.IR.NIR
			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.
zmyExtErr	vikingSource	VIKINGv20161202	Error on extended source colour Z-Y	real	4	mag	-0.9999995e9	stat.error;em.opt.I;em.IR.NIR
			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.
zmyExtErr	vikingSource	VIKINGv20170715	Error on extended source colour Z-Y	real	4	mag	-0.9999995e9	stat.error;em.opt.I;em.IR.NIR
			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.
zmyExtErr	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Error on extended source colour Z-Y	real	4	mag	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyExtErr	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Error on extended source colour Z-Y	real	4	mag	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyExtErr	vvvSource	VVVv20100531	Error on extended source colour Z-Y	real	4	mag	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyExtJky	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Extended source colour calibrated flux Y/Z (using aperJkyNoAperCorr3)	real	4	jansky	-0.9999995e9	phot.color
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyExtJky	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Extended source colour calibrated flux Y/Z (using aperJkyNoAperCorr3)	real	4	jansky	-0.9999995e9	phot.color
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyExtJkyErr	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Error on extended source colour calibrated flux Y/Z	real	4	jansky	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyExtJkyErr	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Error on extended source colour calibrated flux Y/Z	real	4	jansky	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyExtLup	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Extended source colour luptitudeZ-Y (using aperLupNoAperCorr3)	real	4	lup	-0.9999995e9	phot.color
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyExtLup	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Extended source colour luptitudeZ-Y (using aperLupNoAperCorr3)	real	4	lup	-0.9999995e9	phot.color
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyExtLupErr	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Error on extended source colour luptitude Z-Y	real	4	lup	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyExtLupErr	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Error on extended source colour luptitude Z-Y	real	4	lup	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPnt	videoSource	VIDEODR2	Point source colour Z-Y (using aperMag3)	real	4	mag	-0.9999995e9	PHOT_COLOR
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPnt	videoSource	VIDEODR3	Point source colour Z-Y (using aperMag3)	real	4	mag	-0.9999995e9	phot.color
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPnt	videoSource	VIDEODR4	Point source colour Z-Y (using aperMag3)	real	4	mag	-0.9999995e9	phot.color;em.opt.I;em.IR.NIR
			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.
zmyPnt	videoSource	VIDEODR5	Point source colour Z-Y (using aperMag3)	real	4	mag	-0.9999995e9	phot.color;em.opt.I;em.IR.NIR
			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.
zmyPnt	videoSource	VIDEOv20100513	Point source colour Z-Y (using aperMag3)	real	4	mag	-0.9999995e9	PHOT_COLOR
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPnt	videoSource	VIDEOv20111208	Point source colour Z-Y (using aperMag3)	real	4	mag	-0.9999995e9	PHOT_COLOR
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPnt	vikingSource	VIKINGDR2	Point source colour Z-Y (using aperMag3)	real	4	mag	-0.9999995e9	PHOT_COLOR
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPnt	vikingSource	VIKINGDR3	Point source colour Z-Y (using aperMag3)	real	4	mag	-0.9999995e9	phot.color
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPnt	vikingSource	VIKINGDR4	Point source colour Z-Y (using aperMag3)	real	4	mag	-0.9999995e9	phot.color;em.opt.I;em.IR.NIR
			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.
zmyPnt	vikingSource	VIKINGv20110714	Point source colour Z-Y (using aperMag3)	real	4	mag	-0.9999995e9	PHOT_COLOR
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPnt	vikingSource	VIKINGv20111019	Point source colour Z-Y (using aperMag3)	real	4	mag	-0.9999995e9	PHOT_COLOR
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPnt	vikingSource	VIKINGv20130417	Point source colour Z-Y (using aperMag3)	real	4	mag	-0.9999995e9	phot.color
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPnt	vikingSource	VIKINGv20140402	Point source colour Z-Y (using aperMag3)	real	4	mag	-0.9999995e9	phot.color;em.opt.I;em.IR.NIR
			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.
zmyPnt	vikingSource	VIKINGv20150421	Point source colour Z-Y (using aperMag3)	real	4	mag	-0.9999995e9	phot.color;em.opt.I;em.IR.NIR
			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.
zmyPnt	vikingSource	VIKINGv20151230	Point source colour Z-Y (using aperMag3)	real	4	mag	-0.9999995e9	phot.color;em.opt.I;em.IR.NIR
			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.
zmyPnt	vikingSource	VIKINGv20160406	Point source colour Z-Y (using aperMag3)	real	4	mag	-0.9999995e9	phot.color;em.opt.I;em.IR.NIR
			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.
zmyPnt	vikingSource	VIKINGv20161202	Point source colour Z-Y (using aperMag3)	real	4	mag	-0.9999995e9	phot.color;em.opt.I;em.IR.NIR
			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.
zmyPnt	vikingSource	VIKINGv20170715	Point source colour Z-Y (using aperMag3)	real	4	mag	-0.9999995e9	phot.color;em.opt.I;em.IR.NIR
			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.
zmyPnt	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Point source colour Z-Y (using aperMag3)	real	4	mag	-0.9999995e9	phot.color
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPnt	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Point source colour Z-Y (using aperMag3)	real	4	mag	-0.9999995e9	phot.color
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPnt	vvvPsfDophotZYJHKsSource	VVVDR5	Point source colour Z-Y (using PsfMag)	real	4	mag	-0.9999995e9	phot.color
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPnt	vvvSource	VVVDR2	Point source colour Z-Y (using aperMag3)	real	4	mag	-0.9999995e9	phot.color;em.opt.I;em.IR.NIR
			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.
zmyPnt	vvvSource	VVVDR5	Point source colour Z-Y (using aperMag3)	real	4	mag	-0.9999995e9	phot.color;em.opt.I;em.IR.NIR
			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.
zmyPnt	vvvSource	VVVv20100531	Point source colour Z-Y (using aperMag3)	real	4	mag	-0.9999995e9	PHOT_COLOR
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPnt	vvvSource	VVVv20110718	Point source colour Z-Y (using aperMag3)	real	4	mag	-0.9999995e9	PHOT_COLOR
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPnt	vvvSource, vvvSynopticSource	VVVDR1	Point source colour Z-Y (using aperMag3)	real	4	mag	-0.9999995e9	phot.color
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPntErr	videoSource	VIDEODR2	Error on point source colour Z-Y	real	4	mag	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPntErr	videoSource	VIDEODR3	Error on point source colour Z-Y	real	4	mag	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPntErr	videoSource	VIDEODR4	Error on point source colour Z-Y	real	4	mag	-0.9999995e9	stat.error;em.opt.I;em.IR.NIR
			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.
zmyPntErr	videoSource	VIDEODR5	Error on point source colour Z-Y	real	4	mag	-0.9999995e9	stat.error;em.opt.I;em.IR.NIR
			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.
zmyPntErr	videoSource	VIDEOv20100513	Error on point source colour Z-Y	real	4	mag	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPntErr	videoSource	VIDEOv20111208	Error on point source colour Z-Y	real	4	mag	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPntErr	vikingSource	VIKINGDR2	Error on point source colour Z-Y	real	4	mag	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPntErr	vikingSource	VIKINGDR3	Error on point source colour Z-Y	real	4	mag	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPntErr	vikingSource	VIKINGDR4	Error on point source colour Z-Y	real	4	mag	-0.9999995e9	stat.error;em.opt.I;em.IR.NIR
			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.
zmyPntErr	vikingSource	VIKINGv20110714	Error on point source colour Z-Y	real	4	mag	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPntErr	vikingSource	VIKINGv20111019	Error on point source colour Z-Y	real	4	mag	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPntErr	vikingSource	VIKINGv20130417	Error on point source colour Z-Y	real	4	mag	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPntErr	vikingSource	VIKINGv20140402	Error on point source colour Z-Y	real	4	mag	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPntErr	vikingSource	VIKINGv20150421	Error on point source colour Z-Y	real	4	mag	-0.9999995e9	stat.error;em.opt.I;em.IR.NIR
			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.
zmyPntErr	vikingSource	VIKINGv20151230	Error on point source colour Z-Y	real	4	mag	-0.9999995e9	stat.error;em.opt.I;em.IR.NIR
			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.
zmyPntErr	vikingSource	VIKINGv20160406	Error on point source colour Z-Y	real	4	mag	-0.9999995e9	stat.error;em.opt.I;em.IR.NIR
			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.
zmyPntErr	vikingSource	VIKINGv20161202	Error on point source colour Z-Y	real	4	mag	-0.9999995e9	stat.error;em.opt.I;em.IR.NIR
			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.
zmyPntErr	vikingSource	VIKINGv20170715	Error on point source colour Z-Y	real	4	mag	-0.9999995e9	stat.error;em.opt.I;em.IR.NIR
			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.
zmyPntErr	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Error on point source colour Z-Y	real	4	mag	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPntErr	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Error on point source colour Z-Y	real	4	mag	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPntErr	vvvPsfDophotZYJHKsSource	VVVDR5	Error on point source colour Z-Y	real	4	mag	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPntErr	vvvSource	VVVDR2	Error on point source colour Z-Y	real	4	mag	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPntErr	vvvSource	VVVDR5	Error on point source colour Z-Y	real	4	mag	-0.9999995e9	stat.error;em.opt.I;em.IR.NIR
			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.
zmyPntErr	vvvSource	VVVv20100531	Error on point source colour Z-Y	real	4	mag	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPntErr	vvvSource	VVVv20110718	Error on point source colour Z-Y	real	4	mag	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPntErr	vvvSource, vvvSynopticSource	VVVDR1	Error on point source colour Z-Y	real	4	mag	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPntJky	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Point source colour calibrated flux Y/Z (using aperJky3)	real	4	jansky	-0.9999995e9	phot.color
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPntJky	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Point source colour calibrated flux Y/Z (using aperJky3)	real	4	jansky	-0.9999995e9	phot.color
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPntJkyErr	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Error on point source colour calibrated flux Y/Z	real	4	jansky	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPntJkyErr	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Error on point source colour calibrated flux Y/Z	real	4	jansky	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPntLup	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Point source colour luptitude Z-Y (using aperLup3)	real	4	lup	-0.9999995e9	phot.color
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPntLup	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Point source colour luptitude Z-Y (using aperLup3)	real	4	lup	-0.9999995e9	phot.color
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPntLupErr	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	Error on point source colour luptitude Z-Y	real	4	lup	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zmyPntLupErr	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	Error on point source colour luptitude Z-Y	real	4	lup	-0.9999995e9	stat.error
			Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
zndof	videoVariability	VIDEODR2	Number of degrees of freedom for chisquare	smallint	2		-9999
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zndof	videoVariability	VIDEODR3	Number of degrees of freedom for chisquare	smallint	2		-9999	stat.fit.dof
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zndof	videoVariability	VIDEODR4	Number of degrees of freedom for chisquare	smallint	2		-9999	stat.fit.dof;em.opt.I
			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.
zndof	videoVariability	VIDEODR5	Number of degrees of freedom for chisquare	smallint	2		-9999	stat.fit.dof;em.opt.I
			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.
zndof	videoVariability	VIDEOv20111208	Number of degrees of freedom for chisquare	smallint	2		-9999
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zndof	vikingVariability	VIKINGv20110714	Number of degrees of freedom for chisquare	smallint	2		-9999
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zndof	vvvVariability	VVVDR5	Number of degrees of freedom for chisquare	smallint	2		-9999	stat.fit.dof;em.opt.I
			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.
znDofAst	videoVarFrameSetInfo	VIDEODR2	Number of degrees of freedom of astrometric fit in Z band.	smallint	2		-9999
			The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
znDofAst	videoVarFrameSetInfo	VIDEODR3	Number of degrees of freedom of astrometric fit in Z band.	smallint	2		-9999	stat.fit.dof;stat.param;em.IR.NIR
			The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
znDofAst	videoVarFrameSetInfo	VIDEODR4	Number of degrees of freedom of astrometric fit in Z band.	smallint	2		-9999	stat.fit.dof;stat.param;em.opt.I
			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.
znDofAst	videoVarFrameSetInfo	VIDEODR5	Number of degrees of freedom of astrometric fit in Z band.	smallint	2		-9999	stat.fit.dof;stat.param;em.opt.I
			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.
znDofAst	videoVarFrameSetInfo	VIDEOv20111208	Number of degrees of freedom of astrometric fit in Z band.	smallint	2		-9999
			The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
znDofAst	vikingVarFrameSetInfo	VIKINGv20110714	Number of degrees of freedom of astrometric fit in Z band.	smallint	2		-9999
			The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
znDofAst	vvvVarFrameSetInfo	VVVDR5	Number of degrees of freedom of astrometric fit in Z band.	smallint	2		-9999	stat.fit.dof;stat.param;em.opt.I
			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.
znDofPht	videoVarFrameSetInfo	VIDEODR2	Number of degrees of freedom of photometric fit in Z band.	smallint	2		-9999
			The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
znDofPht	videoVarFrameSetInfo	VIDEODR3	Number of degrees of freedom of photometric fit in Z band.	smallint	2		-9999	stat.fit.dof;stat.param;em.IR.NIR
			The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
znDofPht	videoVarFrameSetInfo	VIDEODR4	Number of degrees of freedom of photometric fit in Z band.	smallint	2		-9999	stat.fit.dof;stat.param;em.opt.I
			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.
znDofPht	videoVarFrameSetInfo	VIDEODR5	Number of degrees of freedom of photometric fit in Z band.	smallint	2		-9999	stat.fit.dof;stat.param;em.opt.I
			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.
znDofPht	videoVarFrameSetInfo	VIDEOv20111208	Number of degrees of freedom of photometric fit in Z band.	smallint	2		-9999
			The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
znDofPht	vikingVarFrameSetInfo	VIKINGv20110714	Number of degrees of freedom of photometric fit in Z band.	smallint	2		-9999
			The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
znDofPht	vvvVarFrameSetInfo	VVVDR5	Number of degrees of freedom of photometric fit in Z band.	smallint	2		-9999	stat.fit.dof;stat.param;em.opt.I
			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.
znFlaggedObs	videoVariability	VIDEODR2	Number of detections in Z band flagged as potentially spurious by videoDetection.ppErrBits	int	4		0
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
znFlaggedObs	videoVariability	VIDEODR3	Number of detections in Z band flagged as potentially spurious by videoDetection.ppErrBits	int	4		0	meta.number
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
znFlaggedObs	videoVariability	VIDEODR4	Number of detections in Z band flagged as potentially spurious by videoDetection.ppErrBits	int	4		0	meta.number;em.opt.I
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
znFlaggedObs	videoVariability	VIDEODR5	Number of detections in Z band flagged as potentially spurious by videoDetection.ppErrBits	int	4		0	meta.number;em.opt.I
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
znFlaggedObs	videoVariability	VIDEOv20111208	Number of detections in Z band flagged as potentially spurious by videoDetection.ppErrBits	int	4		0
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
znFlaggedObs	vikingVariability	VIKINGv20110714	Number of detections in Z band flagged as potentially spurious by vikingDetection.ppErrBits	int	4		0
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
znFlaggedObs	vvvVariability	VVVDR5	Number of detections in Z band flagged as potentially spurious by vvvDetection.ppErrBits	int	4		0	meta.number;em.opt.I
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
znFrames	StackObjectThin	PS1DR2	Number of input frames/exposures contributing to the z filter stack detection.	int	4		-999
znGoodObs	videoVariability	VIDEODR2	Number of good detections in Z band	int	4		0
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
znGoodObs	videoVariability	VIDEODR3	Number of good detections in Z band	int	4		0	meta.number;em.IR.NIR
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
znGoodObs	videoVariability	VIDEODR4	Number of good detections in Z band	int	4		0	meta.number;em.opt.I
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
znGoodObs	videoVariability	VIDEODR5	Number of good detections in Z band	int	4		0	meta.number;em.opt.I
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
znGoodObs	videoVariability	VIDEOv20111208	Number of good detections in Z band	int	4		0
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
znGoodObs	vikingVariability	VIKINGv20110714	Number of good detections in Z band	int	4		0
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
znGoodObs	vvvVariability	VVVDR5	Number of good detections in Z band	int	4		0	meta.number;em.opt.I
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
zNgt3sig	videoVariability	VIDEODR2	Number of good detections in Z-band that are more than 3 sigma deviations	smallint	2		-9999
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zNgt3sig	videoVariability	VIDEODR3	Number of good detections in Z-band that are more than 3 sigma deviations	smallint	2		-9999	meta.number;em.IR.NIR
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zNgt3sig	videoVariability	VIDEODR4	Number of good detections in Z-band that are more than 3 sigma deviations	smallint	2		-9999	meta.number;em.opt.I
			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.
zNgt3sig	videoVariability	VIDEODR5	Number of good detections in Z-band that are more than 3 sigma deviations	smallint	2		-9999	meta.number;em.opt.I
			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.
zNgt3sig	videoVariability	VIDEOv20111208	Number of good detections in Z-band that are more than 3 sigma deviations	smallint	2		-9999
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zNgt3sig	vikingVariability	VIKINGv20110714	Number of good detections in Z-band that are more than 3 sigma deviations	smallint	2		-9999
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zNgt3sig	vvvVariability	VVVDR5	Number of good detections in Z-band that are more than 3 sigma deviations (zAperMagN < (zMeanMag-3*zMagRms)	smallint	2		-9999	meta.number;em.opt.I
			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.
znmag	decapsSource	DECAPS	Number of detections in z band {catalogue TType keyword: nmag[4]}	smallint	2			meta.number;em.opt.I
znmag_lbs	decapsSource	DECAPS	Number of detections in z band {catalogue TType keyword: nmag_lbs[4]}	smallint	2		-9999	meta.number;em.opt.I
znmag_lbs_ok	decapsSource	DECAPS	Number of good detections in z band {catalogue TType keyword: nmag_lbs_ok[4]}	smallint	2		-9999	meta.number;em.opt.I
znmag_ok	decapsSource	DECAPS	Number of good detections in z band {catalogue TType keyword: nmag_ok[4]}	smallint	2			meta.number;em.opt.I
znMissingObs	videoVariability	VIDEODR2	Number of Z band frames that this object should have been detected on and was not	int	4		0
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
znMissingObs	videoVariability	VIDEODR3	Number of Z band frames that this object should have been detected on and was not	int	4		0	meta.number;em.IR.NIR
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
znMissingObs	videoVariability	VIDEODR4	Number of Z band frames that this object should have been detected on and was not	int	4		0	meta.number;em.opt.I
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
znMissingObs	videoVariability	VIDEODR5	Number of Z band frames that this object should have been detected on and was not	int	4		0	meta.number;em.opt.I
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
znMissingObs	videoVariability	VIDEOv20111208	Number of Z band frames that this object should have been detected on and was not	int	4		0
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
znMissingObs	vikingVariability	VIKINGv20110714	Number of Z band frames that this object should have been detected on and was not	int	4		0
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
znMissingObs	vvvVariability	VVVDR5	Number of Z band frames that this object should have been detected on and was not	int	4		0	meta.number;em.opt.I
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
zoneID	ObjectThin	PS1DR2	Local zone index, found by dividing the sky into bands of declination 1/2 arcminute in height: zoneID = floor((90 + declination)/0.0083333).	int	4			meta.id
zp	Detection	PS1DR2	Photometric zeropoint. Necessary for converting listed fluxes and magnitudes back to measured ADU counts.	real	4	magnitudes	0
zPA	videoSource	VIDEODR2	ellipse fit celestial orientation in Z	real	4	Degrees	-0.9999995e9	pos.posAng
zPA	videoSource	VIDEODR3	ellipse fit celestial orientation in Z	real	4	Degrees	-0.9999995e9	pos.posAng
zPA	videoSource	VIDEODR4	ellipse fit celestial orientation in Z	real	4	Degrees	-0.9999995e9	pos.posAng;em.opt.I
zPA	videoSource	VIDEODR5	ellipse fit celestial orientation in Z	real	4	Degrees	-0.9999995e9	pos.posAng;em.opt.I
zPA	videoSource	VIDEOv20111208	ellipse fit celestial orientation in Z	real	4	Degrees	-0.9999995e9	pos.posAng
zPA	videoSource, videoSourceRemeasurement	VIDEOv20100513	ellipse fit celestial orientation in Z	real	4	Degrees	-0.9999995e9	pos.posAng
zPA	vikingSource	VIKINGDR2	ellipse fit celestial orientation in Z	real	4	Degrees	-0.9999995e9	pos.posAng
zPA	vikingSource	VIKINGDR3	ellipse fit celestial orientation in Z	real	4	Degrees	-0.9999995e9	pos.posAng
zPA	vikingSource	VIKINGDR4	ellipse fit celestial orientation in Z	real	4	Degrees	-0.9999995e9	pos.posAng;em.opt.I
zPA	vikingSource	VIKINGv20111019	ellipse fit celestial orientation in Z	real	4	Degrees	-0.9999995e9	pos.posAng
zPA	vikingSource	VIKINGv20130417	ellipse fit celestial orientation in Z	real	4	Degrees	-0.9999995e9	pos.posAng
zPA	vikingSource	VIKINGv20140402	ellipse fit celestial orientation in Z	real	4	Degrees	-0.9999995e9	pos.posAng
zPA	vikingSource	VIKINGv20150421	ellipse fit celestial orientation in Z	real	4	Degrees	-0.9999995e9	pos.posAng;em.opt.I
zPA	vikingSource	VIKINGv20151230	ellipse fit celestial orientation in Z	real	4	Degrees	-0.9999995e9	pos.posAng;em.opt.I
zPA	vikingSource	VIKINGv20160406	ellipse fit celestial orientation in Z	real	4	Degrees	-0.9999995e9	pos.posAng;em.opt.I
zPA	vikingSource	VIKINGv20161202	ellipse fit celestial orientation in Z	real	4	Degrees	-0.9999995e9	pos.posAng;em.opt.I
zPA	vikingSource	VIKINGv20170715	ellipse fit celestial orientation in Z	real	4	Degrees	-0.9999995e9	pos.posAng;em.opt.I
zPA	vikingSource, vikingSourceRemeasurement	VIKINGv20110714	ellipse fit celestial orientation in Z	real	4	Degrees	-0.9999995e9	pos.posAng
zPA	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	ellipse fit celestial orientation in Z	real	4	Degrees	-0.9999995e9	pos.posAng
zPA	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	ellipse fit celestial orientation in Z	real	4	Degrees	-0.9999995e9	pos.posAng
zPA	vvvSource	VVVDR2	ellipse fit celestial orientation in Z	real	4	Degrees	-0.9999995e9	pos.posAng
zPA	vvvSource	VVVDR5	ellipse fit celestial orientation in Z	real	4	Degrees	-0.9999995e9	pos.posAng;em.opt.I
zPA	vvvSource	VVVv20110718	ellipse fit celestial orientation in Z	real	4	Degrees	-0.9999995e9	pos.posAng
zPA	vvvSource, vvvSourceRemeasurement	VVVv20100531	ellipse fit celestial orientation in Z	real	4	Degrees	-0.9999995e9	pos.posAng
zPA	vvvSource, vvvSynopticSource	VVVDR1	ellipse fit celestial orientation in Z	real	4	Degrees	-0.9999995e9	pos.posAng
zPetroMag	videoSource	VIDEODR2	Extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	phot.mag
zPetroMag	videoSource	VIDEODR3	Extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	phot.mag
zPetroMag	videoSource	VIDEODR4	Extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zPetroMag	videoSource	VIDEODR5	Extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zPetroMag	videoSource	VIDEOv20100513	Extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	phot.mag
zPetroMag	videoSource	VIDEOv20111208	Extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	phot.mag
zPetroMag	vikingSource	VIKINGDR2	Extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	phot.mag
zPetroMag	vikingSource	VIKINGDR3	Extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	phot.mag
zPetroMag	vikingSource	VIKINGDR4	Extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zPetroMag	vikingSource	VIKINGv20110714	Extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	phot.mag
zPetroMag	vikingSource	VIKINGv20111019	Extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	phot.mag
zPetroMag	vikingSource	VIKINGv20130417	Extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	phot.mag
zPetroMag	vikingSource	VIKINGv20140402	Extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zPetroMag	vikingSource	VIKINGv20150421	Extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zPetroMag	vikingSource	VIKINGv20151230	Extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zPetroMag	vikingSource	VIKINGv20160406	Extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zPetroMag	vikingSource	VIKINGv20161202	Extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zPetroMag	vikingSource	VIKINGv20170715	Extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zPetroMagErr	videoSource	VIDEODR2	Error in extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	stat.error
zPetroMagErr	videoSource	VIDEODR3	Error in extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	stat.error
zPetroMagErr	videoSource	VIDEODR4	Error in extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	stat.error;em.opt.I;phot.mag
zPetroMagErr	videoSource	VIDEODR5	Error in extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	stat.error;em.opt.I;phot.mag
zPetroMagErr	videoSource	VIDEOv20100513	Error in extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	stat.error
zPetroMagErr	videoSource	VIDEOv20111208	Error in extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	stat.error
zPetroMagErr	vikingSource	VIKINGDR2	Error in extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	stat.error
zPetroMagErr	vikingSource	VIKINGDR3	Error in extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	stat.error
zPetroMagErr	vikingSource	VIKINGDR4	Error in extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	stat.error;em.opt.I
zPetroMagErr	vikingSource	VIKINGv20110714	Error in extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	stat.error
zPetroMagErr	vikingSource	VIKINGv20111019	Error in extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	stat.error
zPetroMagErr	vikingSource	VIKINGv20130417	Error in extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	stat.error
zPetroMagErr	vikingSource	VIKINGv20140402	Error in extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	stat.error
zPetroMagErr	vikingSource	VIKINGv20150421	Error in extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	stat.error;em.opt.I;phot.mag
zPetroMagErr	vikingSource	VIKINGv20151230	Error in extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.I
zPetroMagErr	vikingSource	VIKINGv20160406	Error in extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.I
zPetroMagErr	vikingSource	VIKINGv20161202	Error in extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.I
zPetroMagErr	vikingSource	VIKINGv20170715	Error in extended source Z mag (Petrosian)	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.I
zPhoto	twompzPhotoz	TWOMPZ	Photometric redshift obtained with the ANNz framework {image primary HDU keyword: zphoto}	real	4		-0.9999995e9
zPhoto_ANN	wiseScosPhotoz, wiseScosPhotozRejects, wiseScosSvm	WISExSCOSPZ	Photometric redshift obtained with the ANNz framework {image primary HDU keyword: zAnnz}	real	4		-0.9999995e9
zPhoto_Corr	wiseScosPhotoz, wiseScosPhotozRejects, wiseScosSvm	WISExSCOSPZ	Photometric redshift corrected at dec(1950)>2.5 for a hemispherical offset {image primary HDU keyword: zCorr}	real	4		-0.9999995e9
zPlateScale	StackObjectAttributes	PS1DR2	Local plate scale for the z filter stack.	real	4	arcsec/pixel	0
zppErrBits	videoSource	VIDEODR2	additional WFAU post-processing error bits in Z	int	4		0	meta.code
zppErrBits	videoSource	VIDEODR3	additional WFAU post-processing error bits in Z	int	4		0	meta.code
zppErrBits	videoSource	VIDEODR4	additional WFAU post-processing error bits in Z	int	4		0	meta.code;em.opt.I
zppErrBits	videoSource	VIDEODR5	additional WFAU post-processing error bits in Z	int	4		0	meta.code;em.opt.I
zppErrBits	videoSource	VIDEOv20111208	additional WFAU post-processing error bits in Z	int	4		0	meta.code
zppErrBits	videoSource, videoSourceRemeasurement	VIDEOv20100513	additional WFAU post-processing error bits in Z	int	4		0	meta.code
zppErrBits	vikingSource	VIKINGDR2	additional WFAU post-processing error bits in Z	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.
zppErrBits	vikingSource	VIKINGDR3	additional WFAU post-processing error bits in Z	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.
zppErrBits	vikingSource	VIKINGDR4	additional WFAU post-processing error bits in Z	int	4		0	meta.code;em.opt.I
			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.
zppErrBits	vikingSource	VIKINGv20110714	additional WFAU post-processing error bits in Z	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.
zppErrBits	vikingSource	VIKINGv20111019	additional WFAU post-processing error bits in Z	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.
zppErrBits	vikingSource	VIKINGv20130417	additional WFAU post-processing error bits in Z	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.
zppErrBits	vikingSource	VIKINGv20140402	additional WFAU post-processing error bits in Z	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.
zppErrBits	vikingSource	VIKINGv20150421	additional WFAU post-processing error bits in Z	int	4		0	meta.code;em.opt.I
			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.
zppErrBits	vikingSource	VIKINGv20151230	additional WFAU post-processing error bits in Z	int	4		0	meta.code;em.opt.I
			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.
zppErrBits	vikingSource	VIKINGv20160406	additional WFAU post-processing error bits in Z	int	4		0	meta.code;em.opt.I
			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.
zppErrBits	vikingSource	VIKINGv20161202	additional WFAU post-processing error bits in Z	int	4		0	meta.code;em.opt.I
			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.
zppErrBits	vikingSource	VIKINGv20170715	additional WFAU post-processing error bits in Z	int	4		0	meta.code;em.opt.I
			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.
zppErrBits	vikingSourceRemeasurement	VIKINGv20110714	additional WFAU post-processing error bits in Z	int	4		0	meta.code
zppErrBits	vikingSourceRemeasurement	VIKINGv20111019	additional WFAU post-processing error bits in Z	int	4		0	meta.code
zppErrBits	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20160909	additional WFAU post-processing error bits in Z	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.
zppErrBits	vikingZY_selJ_SourceRemeasurement	VIKINGZYSELJv20170124	additional WFAU post-processing error bits in Z	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.
zppErrBits	vvvSource	VVVDR1	additional WFAU post-processing error bits in Z	int	4		0	meta.code
zppErrBits	vvvSource	VVVDR2	additional WFAU post-processing error bits in Z	int	4		0	meta.code
zppErrBits	vvvSource	VVVDR5	additional WFAU post-processing error bits in Z	int	4		0	meta.code;em.opt.I
zppErrBits	vvvSource	VVVv20110718	additional WFAU post-processing error bits in Z	int	4		0	meta.code
zppErrBits	vvvSource, vvvSourceRemeasurement	VVVv20100531	additional WFAU post-processing error bits in Z	int	4		0	meta.code
zppErrBits	vvvSynopticSource	VVVDR1	additional WFAU post-processing error bits in Z	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.
zppErrBits	vvvSynopticSource	VVVDR2	additional WFAU post-processing error bits in Z	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.
zprobVar	videoVariability	VIDEODR2	Probability of variable from chi-square (and other data)	real	4		-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zprobVar	videoVariability	VIDEODR3	Probability of variable from chi-square (and other data)	real	4		-0.9999995e9	stat.probability
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zprobVar	videoVariability	VIDEODR4	Probability of variable from chi-square (and other data)	real	4		-0.9999995e9	stat.probability;em.opt.I
			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.
zprobVar	videoVariability	VIDEODR5	Probability of variable from chi-square (and other data)	real	4		-0.9999995e9	stat.probability;em.opt.I
			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.
zprobVar	videoVariability	VIDEOv20111208	Probability of variable from chi-square (and other data)	real	4		-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zprobVar	vikingVariability	VIKINGv20110714	Probability of variable from chi-square (and other data)	real	4		-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zprobVar	vvvVariability	VVVDR5	Probability of variable from chi-square (and other data)	real	4		-0.9999995e9	stat.probability;em.opt.I
			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.
zpsfChiSq	StackObjectAttributes	PS1DR2	Reduced chi squared value of the PSF model fit for z filter stack detection.	real	4		-999
zpsfCore	StackObjectAttributes	PS1DR2	PSF core parameter k from z filter stack detection, where F = F0 / (1 + k r^2 + r^3.33).	real	4		-999
zPSFFlux	StackObjectAttributes	PS1DR2	PSF flux from z filter stack detection.	real	4	Janskys	-999
zPSFFluxErr	StackObjectAttributes	PS1DR2	Error in PSF flux from z filter stack detection.	real	4	Janskys	-999
zpsfLikelihood	StackObjectAttributes	PS1DR2	Likelihood that this z filter stack detection is best fit by a PSF.	real	4		-999
zPSFMag	StackObjectThin	PS1DR2	PSF magnitude from z filter stack detection.	real	4	AB magnitudes	-999
zPsfMag	videoSource	VIDEOv20100513	Not available in SE output	real	4	mag	-0.9999995e9	phot.mag
zPsfMag	vikingSource	VIKINGDR2	Point source profile-fitted Z mag	real	4	mag	-0.9999995e9	phot.mag
zPsfMag	vikingSource	VIKINGDR3	Point source profile-fitted Z mag	real	4	mag	-0.9999995e9	phot.mag
zPsfMag	vikingSource	VIKINGDR4	Point source profile-fitted Z mag	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zPsfMag	vikingSource	VIKINGv20110714	Point source profile-fitted Z mag	real	4	mag	-0.9999995e9	phot.mag
zPsfMag	vikingSource	VIKINGv20111019	Point source profile-fitted Z mag	real	4	mag	-0.9999995e9	phot.mag
zPsfMag	vikingSource	VIKINGv20130417	Point source profile-fitted Z mag	real	4	mag	-0.9999995e9	phot.mag
zPsfMag	vikingSource	VIKINGv20140402	Point source profile-fitted Z mag	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zPsfMag	vikingSource	VIKINGv20150421	Point source profile-fitted Z mag	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zPsfMag	vikingSource	VIKINGv20151230	Point source profile-fitted Z mag	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zPsfMag	vikingSource	VIKINGv20160406	Point source profile-fitted Z mag	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zPsfMag	vikingSource	VIKINGv20161202	Point source profile-fitted Z mag	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zPsfMag	vikingSource	VIKINGv20170715	Point source profile-fitted Z mag	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zPsfMag	vvvPsfDophotZYJHKsSource	VVVDR5	Mean PSF magnitude in Z band {catalogue TType keyword: mag_Z}	real	4	mag	-0.9999995e9	instr.det.psf;phot.mag;em.opt.I;meta.main
zPSFMagErr	StackObjectThin	PS1DR2	Error in PSF magnitude from z filter stack detection.	real	4	AB magnitudes	-999
zPsfMagErr	videoSource	VIDEOv20100513	Not available in SE output	real	4	mag	-0.9999995e9	stat.error
zPsfMagErr	vikingSource	VIKINGDR2	Error in point source profile-fitted Z mag	real	4	mag	-0.9999995e9	stat.error
zPsfMagErr	vikingSource	VIKINGDR3	Error in point source profile-fitted Z mag	real	4	mag	-0.9999995e9	stat.error
zPsfMagErr	vikingSource	VIKINGDR4	Error in point source profile-fitted Z mag	real	4	mag	-0.9999995e9	stat.error;em.opt.I
zPsfMagErr	vikingSource	VIKINGv20110714	Error in point source profile-fitted Z mag	real	4	mag	-0.9999995e9	stat.error
zPsfMagErr	vikingSource	VIKINGv20111019	Error in point source profile-fitted Z mag	real	4	mag	-0.9999995e9	stat.error
zPsfMagErr	vikingSource	VIKINGv20130417	Error in point source profile-fitted Z mag	real	4	mag	-0.9999995e9	stat.error
zPsfMagErr	vikingSource	VIKINGv20140402	Error in point source profile-fitted Z mag	real	4	mag	-0.9999995e9	stat.error
zPsfMagErr	vikingSource	VIKINGv20150421	Error in point source profile-fitted Z mag	real	4	mag	-0.9999995e9	stat.error;em.opt.I;phot.mag
zPsfMagErr	vikingSource	VIKINGv20151230	Error in point source profile-fitted Z mag	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.I
zPsfMagErr	vikingSource	VIKINGv20160406	Error in point source profile-fitted Z mag	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.I
zPsfMagErr	vikingSource	VIKINGv20161202	Error in point source profile-fitted Z mag	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.I
zPsfMagErr	vikingSource	VIKINGv20170715	Error in point source profile-fitted Z mag	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.I
zPsfMagErr	vvvPsfDophotZYJHKsSource	VVVDR5	Error on mean PSF magnitude in Z band {catalogue TType keyword: er_Z}	real	4	mag	-0.9999995e9	stat.error;instr.det.psf;em.opt.I
zpsfMajorFWHM	StackObjectAttributes	PS1DR2	PSF major axis FWHM from z filter stack detection.	real	4	arcsec	-999
zpsfMinorFWHM	StackObjectAttributes	PS1DR2	PSF minor axis FWHM from z filter stack detection.	real	4	arcsec	-999
zpsfQf	StackObjectAttributes	PS1DR2	PSF coverage factor for z filter stack detection.	real	4		-999
zpsfQfPerfect	StackObjectAttributes	PS1DR2	PSF-weighted fraction of pixels totally unmasked for z filter stack detection.	real	4		-999
zpsfTheta	StackObjectAttributes	PS1DR2	PSF major axis orientation from z filter stack detection.	real	4	degrees	-999
zpSystem	ExternalProduct	SHARKSv20210222	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	SHARKSv20210421	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	ULTRAVISTADR4	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VHSDR3	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VHSDR4	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VHSDR5	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VHSDR6	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VHSv20150108	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VHSv20160114	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VHSv20160507	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VHSv20170630	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VHSv20180419	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VHSv20201209	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VHSv20231101	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VIDEODR4	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VIDEODR5	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VIDEOv20111208	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VIKINGDR4	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VIKINGv20150421	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VIKINGv20151230	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VIKINGv20160406	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VIKINGv20161202	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VIKINGv20170715	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VMCDEEPv20230713	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VMCDR3	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VMCDR4	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VMCDR5	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VMCv20140428	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VMCv20140903	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VMCv20150309	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VMCv20151218	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VMCv20160311	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VMCv20160822	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VMCv20170109	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VMCv20170411	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VMCv20171101	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VMCv20180702	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VMCv20181120	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VMCv20191212	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VMCv20210708	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VMCv20230816	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VMCv20240226	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VVVDR5	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	ExternalProduct	VVVXDR1	System of zeropoint (Vega/AB)	varchar	16		'NONE'
zpSystem	RequiredMosaicTopLevel	SHARKSv20210222	System of zeropoint (Vega/AB)	varchar	8		'NONE'
zpSystem	RequiredMosaicTopLevel	SHARKSv20210421	System of zeropoint (Vega/AB)	varchar	8		'NONE'
zpSystem	RequiredMosaicTopLevel	ULTRAVISTADR4	System of zeropoint (Vega/AB)	varchar	8		'NONE'
zpSystem	RequiredMosaicTopLevel	VHSv20201209	System of zeropoint (Vega/AB)	varchar	8		'NONE'
zpSystem	RequiredMosaicTopLevel	VHSv20231101	System of zeropoint (Vega/AB)	varchar	8		'NONE'
zpSystem	RequiredMosaicTopLevel	VMCDEEPv20230713	System of zeropoint (Vega/AB)	varchar	8		'NONE'
zpSystem	RequiredMosaicTopLevel	VMCDR5	System of zeropoint (Vega/AB)	varchar	8		'NONE'
zpSystem	RequiredMosaicTopLevel	VMCv20191212	System of zeropoint (Vega/AB)	varchar	8		'NONE'
zpSystem	RequiredMosaicTopLevel	VMCv20210708	System of zeropoint (Vega/AB)	varchar	8		'NONE'
zpSystem	RequiredMosaicTopLevel	VMCv20230816	System of zeropoint (Vega/AB)	varchar	8		'NONE'
zpSystem	RequiredMosaicTopLevel	VMCv20240226	System of zeropoint (Vega/AB)	varchar	8		'NONE'
zpSystem	RequiredMosaicTopLevel	VVVDR5	System of zeropoint (Vega/AB)	varchar	8		'NONE'
zpSystem	RequiredMosaicTopLevel	VVVXDR1	System of zeropoint (Vega/AB)	varchar	8		'NONE'
zq25	decapsSource	DECAPS	25th percentile z-band flux (3631 Jy) {catalogue TType keyword: q25[4]}	real	4	3631Jy	-9.999995e8	stat.value;phot.flux;em.opt.I
zq25_lbs	decapsSource	DECAPS	25th percentile local background subtracted z-band flux (3631 Jy) {catalogue TType keyword: q25_lbs[4]}	real	4	3631Jy	-9.999995e8	stat.value;phot.flux;em.opt.I
zq75	decapsSource	DECAPS	75th percentile z-band flux (3631 Jy) {catalogue TType keyword: q75[4]}	real	4	3631Jy	-9.999995e8	stat.value;phot.flux;em.opt.I
zq75_lbs	decapsSource	DECAPS	75th percentile local background subtracted z-band flux (3631 Jy) {catalogue TType keyword: q75_lbs[4]}	real	4	3631Jy	-9.999995e8	stat.value;phot.flux;em.opt.I
zQfPerfect	MeanObject	PS1DR2	Maximum PSF weighted fraction of pixels totally unmasked from z filter detections.	real	4		-999
zra	StackObjectThin	PS1DR2	Right ascension from z filter stack detection.	float	8	degrees	-999
zraErr	StackObjectThin	PS1DR2	Right ascension error from z filter stack detection.	real	4	arcsec	-999
zscatter	smashdr2_deep, smashdr2_object	SMASH	RMS scatter in z from multiple measurements of this object	real	4
Zsep	vvvProperMotionCatalogue	VVVDR5	Sky distance between VVV DR4 Z detection and the projected source position at the Z observation epoch taking the pipeline proper motion into account. {catalogue TType keyword: Zsep}	real	4	arcsec	-999999500.0
zSeqNum	videoSource	VIDEODR2	the running number of the Z detection	int	4		-99999999	meta.id
zSeqNum	videoSource	VIDEODR3	the running number of the Z detection	int	4		-99999999	meta.number
zSeqNum	videoSource	VIDEODR4	the running number of the Z detection	int	4		-99999999	meta.number;em.opt.I
zSeqNum	videoSource	VIDEODR5	the running number of the Z detection	int	4		-99999999	meta.number;em.opt.I
zSeqNum	videoSource	VIDEOv20100513	the running number of the Z detection	int	4		-99999999	meta.id
zSeqNum	videoSource	VIDEOv20111208	the running number of the Z detection	int	4		-99999999	meta.id
zSeqNum	videoSourceRemeasurement	VIDEOv20100513	the running number of the Z remeasurement	int	4		-99999999	meta.id
zSeqNum	vikingSource	VIKINGDR2	the running number of the Z detection	int	4		-99999999	meta.id
zSeqNum	vikingSource	VIKINGDR3	the running number of the Z detection	int	4		-99999999	meta.number
zSeqNum	vikingSource	VIKINGDR4	the running number of the Z detection	int	4		-99999999	meta.number;em.opt.I
zSeqNum	vikingSource	VIKINGv20110714	the running number of the Z detection	int	4		-99999999	meta.id
zSeqNum	vikingSource	VIKINGv20111019	the running number of the Z detection	int	4		-99999999	meta.id
zSeqNum	vikingSource	VIKINGv20130417	the running number of the Z detection	int	4		-99999999	meta.number
zSeqNum	vikingSource	VIKINGv20140402	the running number of the Z detection	int	4		-99999999	meta.number
zSeqNum	vikingSource	VIKINGv20150421	the running number of the Z detection	int	4		-99999999	meta.number;em.opt.I
zSeqNum	vikingSource	VIKINGv20151230	the running number of the Z detection	int	4		-99999999	meta.number;em.opt.I
zSeqNum	vikingSource	VIKINGv20160406	the running number of the Z detection	int	4		-99999999	meta.number;em.opt.I
zSeqNum	vikingSource	VIKINGv20161202	the running number of the Z detection	int	4		-99999999	meta.number;em.opt.I
zSeqNum	vikingSource	VIKINGv20170715	the running number of the Z detection	int	4		-99999999	meta.number;em.opt.I
zSeqNum	vikingSourceRemeasurement	VIKINGv20110714	the running number of the Z remeasurement	int	4		-99999999	meta.id
zSeqNum	vikingSourceRemeasurement	VIKINGv20111019	the running number of the Z remeasurement	int	4		-99999999	meta.id
zSeqNum	vvvSource	VVVDR2	the running number of the Z detection	int	4		-99999999	meta.number
zSeqNum	vvvSource	VVVDR5	the running number of the Z detection	int	4		-99999999	meta.number;em.opt.I
zSeqNum	vvvSource	VVVv20100531	the running number of the Z detection	int	4		-99999999	meta.id
zSeqNum	vvvSource	VVVv20110718	the running number of the Z detection	int	4		-99999999	meta.id
zSeqNum	vvvSource, vvvSynopticSource	VVVDR1	the running number of the Z detection	int	4		-99999999	meta.number
zSeqNum	vvvSourceRemeasurement	VVVv20100531	the running number of the Z remeasurement	int	4		-99999999	meta.id
zSeqNum	vvvSourceRemeasurement	VVVv20110718	the running number of the Z remeasurement	int	4		-99999999	meta.id
zSerMag2D	videoSource	VIDEOv20100513	Not available in SE output	real	4	mag	-0.9999995e9	phot.mag
zSerMag2D	vikingSource	VIKINGDR2	Extended source Z mag (profile-fitted)	real	4	mag	-0.9999995e9	phot.mag
zSerMag2D	vikingSource	VIKINGDR3	Extended source Z mag (profile-fitted)	real	4	mag	-0.9999995e9	phot.mag
zSerMag2D	vikingSource	VIKINGDR4	Extended source Z mag (profile-fitted)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zSerMag2D	vikingSource	VIKINGv20110714	Extended source Z mag (profile-fitted)	real	4	mag	-0.9999995e9	phot.mag
zSerMag2D	vikingSource	VIKINGv20111019	Extended source Z mag (profile-fitted)	real	4	mag	-0.9999995e9	phot.mag
zSerMag2D	vikingSource	VIKINGv20130417	Extended source Z mag (profile-fitted)	real	4	mag	-0.9999995e9	phot.mag
zSerMag2D	vikingSource	VIKINGv20140402	Extended source Z mag (profile-fitted)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zSerMag2D	vikingSource	VIKINGv20150421	Extended source Z mag (profile-fitted)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zSerMag2D	vikingSource	VIKINGv20151230	Extended source Z mag (profile-fitted)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zSerMag2D	vikingSource	VIKINGv20160406	Extended source Z mag (profile-fitted)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zSerMag2D	vikingSource	VIKINGv20161202	Extended source Z mag (profile-fitted)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zSerMag2D	vikingSource	VIKINGv20170715	Extended source Z mag (profile-fitted)	real	4	mag	-0.9999995e9	phot.mag;em.opt.I
zSerMag2DErr	videoSource	VIDEOv20100513	Not available in SE output	real	4	mag	-0.9999995e9	stat.error
zSerMag2DErr	vikingSource	VIKINGDR2	Error in extended source Z mag (profile-fitted)	real	4	mag	-0.9999995e9	stat.error
zSerMag2DErr	vikingSource	VIKINGDR3	Error in extended source Z mag (profile-fitted)	real	4	mag	-0.9999995e9	stat.error
zSerMag2DErr	vikingSource	VIKINGDR4	Error in extended source Z mag (profile-fitted)	real	4	mag	-0.9999995e9	stat.error;em.opt.I
zSerMag2DErr	vikingSource	VIKINGv20110714	Error in extended source Z mag (profile-fitted)	real	4	mag	-0.9999995e9	stat.error
zSerMag2DErr	vikingSource	VIKINGv20111019	Error in extended source Z mag (profile-fitted)	real	4	mag	-0.9999995e9	stat.error
zSerMag2DErr	vikingSource	VIKINGv20130417	Error in extended source Z mag (profile-fitted)	real	4	mag	-0.9999995e9	stat.error
zSerMag2DErr	vikingSource	VIKINGv20140402	Error in extended source Z mag (profile-fitted)	real	4	mag	-0.9999995e9	stat.error
zSerMag2DErr	vikingSource	VIKINGv20150421	Error in extended source Z mag (profile-fitted)	real	4	mag	-0.9999995e9	stat.error;em.opt.I;phot.mag
zSerMag2DErr	vikingSource	VIKINGv20151230	Error in extended source Z mag (profile-fitted)	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.I
zSerMag2DErr	vikingSource	VIKINGv20160406	Error in extended source Z mag (profile-fitted)	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.I
zSerMag2DErr	vikingSource	VIKINGv20161202	Error in extended source Z mag (profile-fitted)	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.I
zSerMag2DErr	vikingSource	VIKINGv20170715	Error in extended source Z mag (profile-fitted)	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.I
zskewness	videoVariability	VIDEODR2	Skewness in Z band (see Sesar et al. 2007)	real	4		-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zskewness	videoVariability	VIDEODR3	Skewness in Z band (see Sesar et al. 2007)	real	4		-0.9999995e9	stat.param;em.IR.NIR
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zskewness	videoVariability	VIDEODR4	Skewness in Z band (see Sesar et al. 2007)	real	4	mag	-0.9999995e9	stat.param;em.opt.I
			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.
zskewness	videoVariability	VIDEODR5	Skewness in Z band (see Sesar et al. 2007)	real	4	mag	-0.9999995e9	stat.param;em.opt.I
			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.
zskewness	videoVariability	VIDEOv20111208	Skewness in Z band (see Sesar et al. 2007)	real	4		-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zskewness	vikingVariability	VIKINGv20110714	Skewness in Z band (see Sesar et al. 2007)	real	4		-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zskewness	vvvVariability	VVVDR5	Skewness in Z band (see Sesar et al. 2007)	real	4	mag	-0.9999995e9	stat.param;em.opt.I
			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.
zsky	StackObjectAttributes	PS1DR2	Residual background sky level at the z filter stack detection.	real	4	Janskys/arcsec^2	-999
zskyErr	StackObjectAttributes	PS1DR2	Error in residual background sky level at the z filter stack detection.	real	4	Janskys/arcsec^2	-999
ZSOURCE	mgcBrightSpec	MGC	Identifier for best redshift and quality	varchar	10
zSpec	twompzPhotoz	TWOMPZ	Spectroscopic redshift {image primary HDU keyword: zspec}	real	4		-0.9999995e9
zstackDetectID	StackObjectAttributes, StackObjectThin	PS1DR2	Unique stack detection identifier.	bigint	8
zstackImageID	StackObjectAttributes, StackObjectThin	PS1DR2	Unique stack identifier for z filter detection.	bigint	8
zstdev	decapsSource	DECAPS	Standard deviation in z-band flux; may be default in rare cases of objects with 1 measurement {catalogue TType keyword: stdev[4]}	real	4	3631Jy	-9.999995e8	stat.stdev;phot.flux;em.opt.I
zstdev_lbs	decapsSource	DECAPS	Standard deviation in local background subtracted z-band fluxes; may be default in rare cases of objects with 1 measurement {catalogue TType keyword: stdev_lbs[4]}	real	4	3631Jy	-9.999995e8	stat.stdev;phot.flux;em.opt.I
ztotalPeriod	videoVariability	VIDEODR2	total period of observations (last obs-first obs)	real	4	days	-0.9999995e9
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
ztotalPeriod	videoVariability	VIDEODR3	total period of observations (last obs-first obs)	real	4	days	-0.9999995e9	time.duration
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
ztotalPeriod	videoVariability	VIDEODR4	total period of observations (last obs-first obs)	real	4	days	-0.9999995e9	time.duration
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
ztotalPeriod	videoVariability	VIDEODR5	total period of observations (last obs-first obs)	real	4	days	-0.9999995e9	time.duration
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
ztotalPeriod	videoVariability	VIDEOv20111208	total period of observations (last obs-first obs)	real	4	days	-0.9999995e9
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
ztotalPeriod	vikingVariability	VIKINGv20110714	total period of observations (last obs-first obs)	real	4	days	-0.9999995e9
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
ztotalPeriod	vvvVariability	VVVDR5	total period of observations (last obs-first obs)	real	4	days	-0.9999995e9	time.duration
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
zVarClass	videoVariability	VIDEODR2	Classification of variability in this band	smallint	2		-9999
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zVarClass	videoVariability	VIDEODR3	Classification of variability in this band	smallint	2		-9999	meta.code.class;src.var
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zVarClass	videoVariability	VIDEODR4	Classification of variability in this band	smallint	2		-9999	meta.code.class;src.var;em.opt.I
			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.
zVarClass	videoVariability	VIDEODR5	Classification of variability in this band	smallint	2		-9999	meta.code.class;src.var;em.opt.I
			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.
zVarClass	videoVariability	VIDEOv20111208	Classification of variability in this band	smallint	2		-9999
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zVarClass	vikingVariability	VIKINGv20110714	Classification of variability in this band	smallint	2		-9999
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
zVarClass	vvvVariability	VVVDR5	Classification of variability in this band	smallint	2		-9999	meta.code.class;src.var;em.opt.I
			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.
zXi	videoSource	VIDEODR2	Offset of Z 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.
zXi	videoSource	VIDEODR3	Offset of Z 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.
zXi	videoSource	VIDEODR4	Offset of Z detection from master position (+east/-west)	real	4	arcsec	-0.9999995e9	pos.eq.ra;arith.diff;em.opt.I
			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.
zXi	videoSource	VIDEODR5	Offset of Z detection from master position (+east/-west)	real	4	arcsec	-0.9999995e9	pos.eq.ra;arith.diff;em.opt.I
			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.
zXi	videoSource	VIDEOv20100513	Offset of Z 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.
zXi	videoSource	VIDEOv20111208	Offset of Z 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.
zXi	vikingSource	VIKINGDR2	Offset of Z 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.
zXi	vikingSource	VIKINGDR3	Offset of Z 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.
zXi	vikingSource	VIKINGDR4	Offset of Z detection from master position (+east/-west)	real	4	arcsec	-0.9999995e9	pos.eq.ra;arith.diff;em.opt.I
			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.
zXi	vikingSource	VIKINGv20110714	Offset of Z 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.
zXi	vikingSource	VIKINGv20111019	Offset of Z 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.
zXi	vikingSource	VIKINGv20130417	Offset of Z 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.
zXi	vikingSource	VIKINGv20140402	Offset of Z 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.
zXi	vikingSource	VIKINGv20150421	Offset of Z detection from master position (+east/-west)	real	4	arcsec	-0.9999995e9	pos.eq.ra;arith.diff;em.opt.I
			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.
zXi	vikingSource	VIKINGv20151230	Offset of Z detection from master position (+east/-west)	real	4	arcsec	-0.9999995e9	pos.eq.ra;arith.diff;em.opt.I
			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.
zXi	vikingSource	VIKINGv20160406	Offset of Z detection from master position (+east/-west)	real	4	arcsec	-0.9999995e9	pos.eq.ra;arith.diff;em.opt.I
			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.
zXi	vikingSource	VIKINGv20161202	Offset of Z detection from master position (+east/-west)	real	4	arcsec	-0.9999995e9	pos.eq.ra;arith.diff;em.opt.I
			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.
zXi	vikingSource	VIKINGv20170715	Offset of Z detection from master position (+east/-west)	real	4	arcsec	-0.9999995e9	pos.eq.ra;arith.diff;em.opt.I
			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.
zXi	vvvSource	VVVDR2	Offset of Z 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.
zXi	vvvSource	VVVDR5	Offset of Z detection from master position (+east/-west)	real	4	arcsec	-0.9999995e9	pos.eq.ra;arith.diff;em.opt.I
			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.
zXi	vvvSource	VVVv20100531	Offset of Z 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.
zXi	vvvSource	VVVv20110718	Offset of Z 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.
zXi	vvvSource, vvvSynopticSource	VVVDR1	Offset of Z 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.
zxPos	StackObjectAttributes	PS1DR2	PSF x center location from z filter stack detection.	real	4	sky pixels	-999
zxPosErr	StackObjectAttributes	PS1DR2	Error in PSF x center location from z filter stack detection.	real	4	sky pixels	-999
zyPos	StackObjectAttributes	PS1DR2	PSF y center location from z filter stack detection.	real	4	sky pixels	-999
zyPosErr	StackObjectAttributes	PS1DR2	Error in PSF y center location from z filter stack detection.	real	4	sky pixels	-999
zzp	StackObjectAttributes	PS1DR2	Photometric zeropoint for the z filter stack. Necessary for converting listed fluxes and magnitudes back to measured ADU counts.	real	4	magnitudes	0