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 
SExtractor classification statistic in Z_1 
real 
4 

0.9999995e9 
stat;em.opt.I 
z_1Ell 
vvvSource 
VVVDR5 
1b/a, where a/b=semimajor/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 
VVVDR4 
the extension number of this 1st epoch Z 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 
VVVDR4 
the UID of the relevant 1st epoch Z tile 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 
VVVDR4 
the MJD of the 1st epoch Z tile multiframe 
float 
8 


time;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_1Y_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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
z_1my_1PntErr 
vvvSource 
VVVDR5 
Error on point source colour Z_1Y_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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d 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 postprocessing 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 
SExtractor classification statistic in Z_2 
real 
4 

0.9999995e9 
stat;em.opt.I 
z_2Ell 
vvvSource 
VVVDR5 
1b/a, where a/b=semimajor/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 
VVVDR4 
the extension number of this 2nd epoch Z 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 
VVVDR4 
the UID of the relevant 2nd epoch Z tile 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 
VVVDR4 
the MJD of the 2nd epoch Z tile multiframe 
float 
8 


time;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_2Y_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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
z_2my_2PntErr 
vvvSource 
VVVDR5 
Error on point source colour Z_2Y_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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d 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 postprocessing 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 
crosscorrelation 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 zband measurements in photometry table 
smallint 
2 


meta.code 
Z_HELIO 
spectra 
SIXDF 
heliocentric redshift 
real 
4 



z_nch 
masterDR2 
SKYMAPPER 
Number of zband child sources combined into this object_id 
smallint 
2 


meta.number 
z_nclip 
masterDR2 
SKYMAPPER 
Number of zband observations with magnitudes clipped from the final PSF magnitude estimate 
smallint 
2 


meta.number 
z_ngood 
masterDR2 
SKYMAPPER 
Number of zband observations used 
smallint 
2 


meta.number 
z_nimaflags 
masterDR2 
SKYMAPPER 
Number of flagged pixels from bad, saturated, and crosstalk pixel masks from zband 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 zband Petrosian magnitude 
real 
4 
mag 

phot.mag;stat.mean 
z_psf 
masterDR2 
SKYMAPPER 
Mean zband PSF magnitude 
real 
4 
mag 

phot.mag;stat.mean 
z_rchi2var 
masterDR2 
SKYMAPPER 
Reduced chisquared for a constantmagnitude model of the zband 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 
VVVDR4 
Point source Z aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
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 
VVVDR4 
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 
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 
zAperMag2 
vvvSynopticSource 
VVVDR4 
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 
zAperMag2Err 
vvvSynopticSource 
VVVDR4 
Error in extended source Z mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.opt.I 
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 
videoSource 
VIDEOv20201103 
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 
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 
VIKINGDR5 
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 
VVVDR4 
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 
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 
vvvSynopticSource 
VVVDR4 
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 
VVVDR4 
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 

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 
videoSource 
VIDEOv20201103 
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 
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 
VIKINGDR5 
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 
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 
VVVDR4 
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 
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 
VVVDR4 
Error in default point source Z mag, from VVVDR4 {catalogue TType keyword: zAperMag3Err} 
real 
4 
mag 
9.999995e8 

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 
videoSource 
VIDEOv20201103 
Point source Z aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
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 
VIKINGDR5 
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 
VVVDR4 
Point 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 
videoSource 
VIDEOv20201103 
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 
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 
VIKINGDR5 
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 
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 
VVVDR4 
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 
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 
zAperMag5 
vvvSynopticSource 
VVVDR4 
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 
zAperMag5Err 
vvvSynopticSource 
VVVDR4 
Error in extended source Z mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.opt.I 
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 
videoSource 
VIDEOv20201103 
Point source Z aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
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 
VIKINGDR5 
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 
videoSource 
VIDEOv20201103 
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 
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 
VIKINGDR5 
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 
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 
videoSource 
VIDEOv20201103 
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 
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 
VIKINGDR5 
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 
videoSource 
VIDEOv20201103 
Extended source Z aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
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 
VIKINGDR5 
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 
videoSource 
VIDEOv20201103 
Extended source Z aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
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 
VIKINGDR5 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
zaStratAst 
videoVarFrameSetInfo 
VIDEOv20201103 
Parameter, c0 from FerreiraLopes & 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
zaStratAst 
vvvVarFrameSetInfo 
VVVDR5 
Parameter, c0 from FerreiraLopes & 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
zaStratPht 
videoVarFrameSetInfo 
VIDEOv20201103 
Parameter, c0 from FerreiraLopes & 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 FerreiraLopes & 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 
VIKINGDR5 
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 
VVVDR4 
average confidence in 2 arcsec diameter default aperture (aper3) Z 
real 
4 

0.9999995e9 
stat.likelihood;em.opt.I 
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 (16) for photometric statistics in the Z band 
int 
4 

9999 

Aperture magnitude (16) 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 (16) for photometric statistics in the Z band 
int 
4 

9999 
meta.code.class;em.IR.NIR 
Aperture magnitude (16) 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 (16) for photometric statistics in the Z band 
int 
4 

9999 
meta.code.class;em.opt.I 
Aperture magnitude (16) 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 (16) for photometric statistics in the Z band 
int 
4 

9999 
meta.code.class;em.opt.I 
Aperture magnitude (16) 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 (16) for photometric statistics in the Z band 
int 
4 

9999 

Aperture magnitude (16) 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 
VIDEOv20201103 
Best aperture (16) for photometric statistics in the Z band 
int 
4 

9999 
meta.code.class;em.opt.I 
Aperture magnitude (16) 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 (16) for photometric statistics in the Z band 
int 
4 

9999 

Aperture magnitude (16) 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 (16) for photometric statistics in the Z band 
int 
4 

9999 
meta.code.class;em.opt.I 
Aperture magnitude (16) 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
zbStratAst 
videoVarFrameSetInfo 
VIDEOv20201103 
Parameter, c1 from FerreiraLopes & 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
zbStratAst 
vvvVarFrameSetInfo 
VVVDR5 
Parameter, c1 from FerreiraLopes & 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
zbStratPht 
videoVarFrameSetInfo 
VIDEOv20201103 
Parameter, c1 from FerreiraLopes & 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 FerreiraLopes & 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
zchiSqAst 
videoVarFrameSetInfo 
VIDEOv20201103 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 
VIDEOv20201103 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
zchiSqPht 
videoVarFrameSetInfo 
VIDEOv20201103 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
Zclass 
vvvParallaxCatalogue 
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 
vvvParallaxCatalogue, vvvProperMotionCatalogue 
VVVDR4 
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 
VIDEOv20201103 
discrete image classification flag in Z 
smallint 
2 

9999 
src.class;em.opt.I 
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 
VIKINGDR5 
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 
VVVDR4 
discrete image classification flag in Z 
smallint 
2 

9999 
src.class;em.opt.I 
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 
SExtractor classification statistic in Z 
real 
4 

0.9999995e9 
stat 
zClassStat 
videoSource 
VIDEODR3 
SExtractor classification statistic in Z 
real 
4 

0.9999995e9 
stat 
zClassStat 
videoSource 
VIDEODR4 
SExtractor classification statistic in Z 
real 
4 

0.9999995e9 
stat;em.opt.I 
zClassStat 
videoSource 
VIDEODR5 
SExtractor classification statistic in Z 
real 
4 

0.9999995e9 
stat;em.opt.I 
zClassStat 
videoSource 
VIDEOv20100513 
SExtractor classification statistic in Z 
real 
4 

0.9999995e9 
stat 
zClassStat 
videoSource 
VIDEOv20111208 
SExtractor classification statistic in Z 
real 
4 

0.9999995e9 
stat 
zClassStat 
videoSource 
VIDEOv20201103 
SExtractor classification statistic in Z 
real 
4 

0.9999995e9 
stat;em.opt.I 
zClassStat 
videoSourceRemeasurement 
VIDEOv20100513 
N(0,1) stellarnessofprofile statistic in Z 
real 
4 

0.9999995e9 
stat 
zClassStat 
vikingSource 
VIKINGDR2 
N(0,1) stellarnessofprofile statistic in Z 
real 
4 

0.9999995e9 
stat 
zClassStat 
vikingSource 
VIKINGDR3 
N(0,1) stellarnessofprofile statistic in Z 
real 
4 

0.9999995e9 
stat 
zClassStat 
vikingSource 
VIKINGDR4 
N(0,1) stellarnessofprofile statistic in Z 
real 
4 

0.9999995e9 
stat;em.opt.I 
zClassStat 
vikingSource 
VIKINGDR5 
N(0,1) stellarnessofprofile statistic in Z 
real 
4 

0.9999995e9 
stat;em.opt.I 
zClassStat 
vikingSource 
VIKINGv20111019 
N(0,1) stellarnessofprofile statistic in Z 
real 
4 

0.9999995e9 
stat 
zClassStat 
vikingSource 
VIKINGv20130417 
N(0,1) stellarnessofprofile statistic in Z 
real 
4 

0.9999995e9 
stat 
zClassStat 
vikingSource 
VIKINGv20140402 
N(0,1) stellarnessofprofile statistic in Z 
real 
4 

0.9999995e9 
stat 
zClassStat 
vikingSource 
VIKINGv20150421 
N(0,1) stellarnessofprofile statistic in Z 
real 
4 

0.9999995e9 
stat;em.opt.I 
zClassStat 
vikingSource 
VIKINGv20151230 
N(0,1) stellarnessofprofile statistic in Z 
real 
4 

0.9999995e9 
stat;em.opt.I 
zClassStat 
vikingSource 
VIKINGv20160406 
N(0,1) stellarnessofprofile statistic in Z 
real 
4 

0.9999995e9 
stat;em.opt.I 
zClassStat 
vikingSource 
VIKINGv20161202 
N(0,1) stellarnessofprofile statistic in Z 
real 
4 

0.9999995e9 
stat;em.opt.I 
zClassStat 
vikingSource 
VIKINGv20170715 
N(0,1) stellarnessofprofile statistic in Z 
real 
4 

0.9999995e9 
stat;em.opt.I 
zClassStat 
vikingSource, vikingSourceRemeasurement 
VIKINGv20110714 
N(0,1) stellarnessofprofile statistic in Z 
real 
4 

0.9999995e9 
stat 
zClassStat 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
N(0,1) stellarnessofprofile statistic in Z 
real 
4 

0.9999995e9 
stat 
zClassStat 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
N(0,1) stellarnessofprofile statistic in Z 
real 
4 

0.9999995e9 
stat 
zClassStat 
vvvSource 
VVVDR1 
SExtractor classification statistic in Z 
real 
4 

0.9999995e9 
stat 
zClassStat 
vvvSource 
VVVDR2 
SExtractor classification statistic in Z 
real 
4 

0.9999995e9 
stat 
zClassStat 
vvvSource 
VVVDR4 
SExtractor classification statistic in Z 
real 
4 

0.9999995e9 
stat;em.opt.I 
zClassStat 
vvvSource 
VVVDR5 
SExtractor classification statistic in Z 
real 
4 

0.9999995e9 
stat;em.opt.I 
zClassStat 
vvvSource 
VVVv20100531 
SExtractor classification statistic in Z 
real 
4 

0.9999995e9 
stat 
zClassStat 
vvvSource 
VVVv20110718 
SExtractor classification statistic in Z 
real 
4 

0.9999995e9 
stat 
zClassStat 
vvvSourceRemeasurement 
VVVv20100531 
N(0,1) stellarnessofprofile statistic in Z 
real 
4 

0.9999995e9 
stat 
zClassStat 
vvvSourceRemeasurement 
VVVv20110718 
N(0,1) stellarnessofprofile statistic in Z 
real 
4 

0.9999995e9 
stat 
zClassStat 
vvvSynopticSource 
VVVDR1 
N(0,1) stellarnessofprofile statistic in Z 
real 
4 

0.9999995e9 
stat 
zClassStat 
vvvSynopticSource 
VVVDR2 
N(0,1) stellarnessofprofile statistic in Z 
real 
4 

0.9999995e9 
stat 
zClassStat 
vvvSynopticSource 
VVVDR4 
N(0,1) stellarnessofprofile statistic in Z 
real 
4 

0.9999995e9 
stat;em.opt.I 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
zcStratAst 
videoVarFrameSetInfo 
VIDEOv20201103 
Parameter, c2 from FerreiraLopes & 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
zcStratAst 
vvvVarFrameSetInfo 
VVVDR5 
Parameter, c2 from FerreiraLopes & 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
zcStratPht 
videoVarFrameSetInfo 
VIDEOv20201103 
Parameter, c2 from FerreiraLopes & 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 FerreiraLopes & 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 
VVVDR5 
Ellipticity of the DR4 Z detection. {catalogue TType keyword: Zell} 
real 
4 

999999500.0 

Zell 
vvvParallaxCatalogue, vvvProperMotionCatalogue 
VVVDR4 
Ellipticity of the DR4 Z detection. {catalogue TType keyword: Zell} 
real 
4 

999999500.0 

zEll 
videoSource 
VIDEODR2 
1b/a, where a/b=semimajor/minor axes in Z 
real 
4 

0.9999995e9 
src.ellipticity 
zEll 
videoSource 
VIDEODR3 
1b/a, where a/b=semimajor/minor axes in Z 
real 
4 

0.9999995e9 
src.ellipticity 
zEll 
videoSource 
VIDEODR4 
1b/a, where a/b=semimajor/minor axes in Z 
real 
4 

0.9999995e9 
src.ellipticity;em.opt.I 
zEll 
videoSource 
VIDEODR5 
1b/a, where a/b=semimajor/minor axes in Z 
real 
4 

0.9999995e9 
src.ellipticity;em.opt.I 
zEll 
videoSource 
VIDEOv20111208 
1b/a, where a/b=semimajor/minor axes in Z 
real 
4 

0.9999995e9 
src.ellipticity 
zEll 
videoSource 
VIDEOv20201103 
1b/a, where a/b=semimajor/minor axes in Z 
real 
4 

0.9999995e9 
src.ellipticity;em.opt.I 
zEll 
videoSource, videoSourceRemeasurement 
VIDEOv20100513 
1b/a, where a/b=semimajor/minor axes in Z 
real 
4 

0.9999995e9 
src.ellipticity 
zEll 
vikingSource 
VIKINGDR2 
1b/a, where a/b=semimajor/minor axes in Z 
real 
4 

0.9999995e9 
src.ellipticity 
zEll 
vikingSource 
VIKINGDR3 
1b/a, where a/b=semimajor/minor axes in Z 
real 
4 

0.9999995e9 
src.ellipticity 
zEll 
vikingSource 
VIKINGDR4 
1b/a, where a/b=semimajor/minor axes in Z 
real 
4 

0.9999995e9 
src.ellipticity;em.opt.I 
zEll 
vikingSource 
VIKINGDR5 
1b/a, where a/b=semimajor/minor axes in Z 
real 
4 

0.9999995e9 
src.ellipticity;em.opt.I 
zEll 
vikingSource 
VIKINGv20111019 
1b/a, where a/b=semimajor/minor axes in Z 
real 
4 

0.9999995e9 
src.ellipticity 
zEll 
vikingSource 
VIKINGv20130417 
1b/a, where a/b=semimajor/minor axes in Z 
real 
4 

0.9999995e9 
src.ellipticity 
zEll 
vikingSource 
VIKINGv20140402 
1b/a, where a/b=semimajor/minor axes in Z 
real 
4 

0.9999995e9 
src.ellipticity 
zEll 
vikingSource 
VIKINGv20150421 
1b/a, where a/b=semimajor/minor axes in Z 
real 
4 

0.9999995e9 
src.ellipticity;em.opt.I 
zEll 
vikingSource 
VIKINGv20151230 
1b/a, where a/b=semimajor/minor axes in Z 
real 
4 

0.9999995e9 
src.ellipticity;em.opt.I 
zEll 
vikingSource 
VIKINGv20160406 
1b/a, where a/b=semimajor/minor axes in Z 
real 
4 

0.9999995e9 
src.ellipticity;em.opt.I 
zEll 
vikingSource 
VIKINGv20161202 
1b/a, where a/b=semimajor/minor axes in Z 
real 
4 

0.9999995e9 
src.ellipticity;em.opt.I 
zEll 
vikingSource 
VIKINGv20170715 
1b/a, where a/b=semimajor/minor axes in Z 
real 
4 

0.9999995e9 
src.ellipticity;em.opt.I 
zEll 
vikingSource, vikingSourceRemeasurement 
VIKINGv20110714 
1b/a, where a/b=semimajor/minor axes in Z 
real 
4 

0.9999995e9 
src.ellipticity 
zEll 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
1b/a, where a/b=semimajor/minor axes in Z 
real 
4 

0.9999995e9 
src.ellipticity 
zEll 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
1b/a, where a/b=semimajor/minor axes in Z 
real 
4 

0.9999995e9 
src.ellipticity 
zEll 
vvvSource 
VVVDR2 
1b/a, where a/b=semimajor/minor axes in Z 
real 
4 

0.9999995e9 
src.ellipticity 
zEll 
vvvSource 
VVVDR4 
1b/a, where a/b=semimajor/minor axes in Z 
real 
4 

0.9999995e9 
src.ellipticity;em.opt.I 
zEll 
vvvSource 
VVVDR5 
1b/a, where a/b=semimajor/minor axes in Z 
real 
4 

0.9999995e9 
src.ellipticity;em.opt.I 
zEll 
vvvSource 
VVVv20110718 
1b/a, where a/b=semimajor/minor axes in Z 
real 
4 

0.9999995e9 
src.ellipticity 
zEll 
vvvSource, vvvSourceRemeasurement 
VVVv20100531 
1b/a, where a/b=semimajor/minor axes in Z 
real 
4 

0.9999995e9 
src.ellipticity 
zEll 
vvvSource, vvvSynopticSource 
VVVDR1 
1b/a, where a/b=semimajor/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 
videoMergeLog 
VIDEOv20201103 
the extension number of this Z frame 
tinyint 
1 


meta.id;em.opt.I 
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 
VIKINGDR5 
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 
VVVDR4 
the extension number of this Z frame 
tinyint 
1 


meta.number;em.opt.I 
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 zband 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 
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 
VIDEOv20201103 
Zeropoint of each product 
real 
4 

0.9999995e9 

zeroPoint 
ExternalProduct 
VIKINGDR4 
Zeropoint of each product 
real 
4 

0.9999995e9 

zeroPoint 
ExternalProduct 
VIKINGDR5 
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 
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 
VVVDR4 
Zeropoint of each product 
real 
4 

0.9999995e9 

zeroPoint 
ExternalProduct 
VVVDR5 
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 
VIDEOv20201103 
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 
VVVDR5 
Zeropoint of each product 
real 
4 

0.9999995e9 

zerr 
decapsSource 
DECAPS 
Uncertainty in mean zband flux (statistical only) {catalogue TType keyword: err[4]} 
real 
4 
3631Jy 
9.999995e8 
stat.error;phot.flux;em.opt.I 
zerr_lbs 
decapsSource 
DECAPS 
Uncertainty in mean local background subtracted zband 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 
videoSource 
VIDEOv20201103 
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 
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 
VIKINGDR5 
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 
VVVDR4 
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 
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 
videoSource 
VIDEOv20201103 
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 
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 
VIKINGDR5 
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 
VVVDR4 
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 
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 
videoVarFrameSetInfo 
VIDEOv20201103 
Expected magnitude limit of frameSet in this in Z band. 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I;stat.max 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 
VIDEOv20201103 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 
PSFweighted fraction of zband 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 
VIDEOv20201103 
RMS of axes of ellipse fit in Z 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.opt.I 
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 
VIKINGDR5 
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 
VVVDR4 
RMS of axes of ellipse fit in Z 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.opt.I 
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 halflight radius in Z band 
real 
4 
pixels 
0.9999995e9 
phys.angSize;em.opt.I 
zHalfRad 
videoSource 
VIDEODR5 
SExtractor halflight radius in Z band 
real 
4 
pixels 
0.9999995e9 
phys.angSize;em.opt.I 
zHalfRad 
videoSource 
VIDEOv20201103 
SExtractor halflight radius in Z band 
real 
4 
pixels 
0.9999995e9 
phys.angSize;em.opt.I 
zHlCorSMjRadAs 
videoSource 
VIDEODR2 
Seeing corrected halflight, semimajor axis in Z band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
zHlCorSMjRadAs 
videoSource 
VIDEODR3 
Seeing corrected halflight, semimajor axis in Z band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
zHlCorSMjRadAs 
videoSource 
VIDEODR4 
Seeing corrected halflight, semimajor axis in Z band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.opt.I 
zHlCorSMjRadAs 
videoSource 
VIDEODR5 
Seeing corrected halflight, semimajor axis in Z band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.opt.I 
zHlCorSMjRadAs 
videoSource 
VIDEOv20100513 
Seeing corrected halflight, semimajor axis in Z band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
zHlCorSMjRadAs 
videoSource 
VIDEOv20111208 
Seeing corrected halflight, semimajor axis in Z band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
zHlCorSMjRadAs 
videoSource 
VIDEOv20201103 
Seeing corrected halflight, semimajor axis in Z band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.opt.I 
zHlCorSMjRadAs 
vikingSource 
VIKINGDR2 
Seeing corrected halflight, semimajor axis in Z band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
zHlCorSMjRadAs 
vikingSource 
VIKINGDR3 
Seeing corrected halflight, semimajor axis in Z band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
zHlCorSMjRadAs 
vikingSource 
VIKINGDR4 
Seeing corrected halflight, semimajor axis in Z band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.opt.I 
zHlCorSMjRadAs 
vikingSource 
VIKINGDR5 
Seeing corrected halflight, semimajor axis in Z band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.opt.I 
zHlCorSMjRadAs 
vikingSource 
VIKINGv20110714 
Seeing corrected halflight, semimajor axis in Z band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
zHlCorSMjRadAs 
vikingSource 
VIKINGv20111019 
Seeing corrected halflight, semimajor axis in Z band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
zHlCorSMjRadAs 
vikingSource 
VIKINGv20130417 
Seeing corrected halflight, semimajor axis in Z band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
zHlCorSMjRadAs 
vikingSource 
VIKINGv20140402 
Seeing corrected halflight, semimajor axis in Z band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
zHlCorSMjRadAs 
vikingSource 
VIKINGv20150421 
Seeing corrected halflight, semimajor axis in Z band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.opt.I 
zHlCorSMjRadAs 
vikingSource 
VIKINGv20151230 
Seeing corrected halflight, semimajor axis in Z band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.opt.I 
zHlCorSMjRadAs 
vikingSource 
VIKINGv20160406 
Seeing corrected halflight, semimajor axis in Z band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.opt.I 
zHlCorSMjRadAs 
vikingSource 
VIKINGv20161202 
Seeing corrected halflight, semimajor axis in Z band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.opt.I 
zHlCorSMjRadAs 
vikingSource 
VIKINGv20170715 
Seeing corrected halflight, semimajor 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 Zband 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 Zband 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 Zband 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 Zband 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 Zband 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 
VIDEOv20201103 
Intrinsic rms in Zband 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 Zband 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 Zband 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 
videoVarFrameSetInfo 
VIDEOv20201103 
Use a default model for the astrometric noise in Z band. 
tinyint 
1 

0 
meta.code;em.opt.I 
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 
videoVarFrameSetInfo 
VIDEOv20201103 
Use a default model for the photometric noise in Z band. 
tinyint 
1 

0 
meta.code;em.opt.I 
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 
zKronMag 
videoSource 
VIDEOv20201103 
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 
zKronMagErr 
videoSource 
VIDEOv20201103 
Extended source Z mag error (Kron  SExtractor MAG_AUTO) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.opt.I 
zKronRad 
StackObjectAttributes 
PS1DR2 
Kron (1980) radius from z filter stack detection. 
real 
4 
arcsec 
999 

Zmag 
vvvParallaxCatalogue 
VVVDR5 
VVV DR4 Z photometry {catalogue TType keyword: Zmag} 
real 
4 
mag 
999999500.0 

Zmag 
vvvParallaxCatalogue, vvvProperMotionCatalogue 
VVVDR4 
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 
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 zband 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 
VIDEOv20201103 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 
VIDEOv20201103 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 
videoVariability 
VIDEOv20201103 
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 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 
VIDEOv20201103 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 
zband 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 zband 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 
VIDEOv20201103 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 
VVVDR4 
Is there a Z band measurment for this frame 
tinyint 
1 



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 
videoVariability 
VIDEOv20201103 
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 
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 zband 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 zband 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 
VIDEOv20201103 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 
videoMergeLog 
VIDEOv20201103 
the UID of the relevant Z multiframe 
bigint 
8 


meta.id;obs.field;em.opt.I 
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 
VIKINGDR5 
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 
VVVDR4 
the UID of the relevant Z multiframe 
bigint 
8 


meta.id;obs.field;em.opt.I 
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 
videoVariability 
VIDEOv20201103 
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 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 
VIDEOv20201103 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zMjd 
videoSource 
VIDEOv20201103 
Modified Julian Day in Z band 
float 
8 
days 
0.9999995e9 
time.epoch;em.opt.I 
zMjd 
vikingSource 
VIKINGDR5 
Modified Julian Day in Z band 
float 
8 
days 
0.9999995e9 
time.epoch;em.opt.I 
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 
zMjd 
vvvSynopticSource 
VVVDR4 
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 ZY (using appropriate mags) 
real 
4 
mag 

PHOT_COLOR 
zmy 
vikingSourceRemeasurement 
VIKINGv20110714 
Default colour ZY (using appropriate mags) 
real 
4 
mag 

PHOT_COLOR 
zmy 
vikingSourceRemeasurement 
VIKINGv20111019 
Default colour ZY (using appropriate mags) 
real 
4 
mag 

PHOT_COLOR 
zmy 
vvvSourceRemeasurement 
VVVv20100531 
Default colour ZY (using appropriate mags) 
real 
4 
mag 

PHOT_COLOR 
zmy 
vvvSourceRemeasurement 
VVVv20110718 
Default colour ZY (using appropriate mags) 
real 
4 
mag 

PHOT_COLOR 
zmyErr 
videoSourceRemeasurement 
VIDEOv20100513 
Error on colour ZY 
real 
4 
mag 

stat.error 
zmyErr 
vikingSourceRemeasurement 
VIKINGv20110714 
Error on colour ZY 
real 
4 
mag 

stat.error 
zmyErr 
vikingSourceRemeasurement 
VIKINGv20111019 
Error on colour ZY 
real 
4 
mag 

stat.error 
zmyErr 
vvvSourceRemeasurement 
VVVv20100531 
Error on colour ZY 
real 
4 
mag 

stat.error 
zmyErr 
vvvSourceRemeasurement 
VVVv20110718 
Error on colour ZY 
real 
4 
mag 

stat.error 
zmyExt 
videoSource 
VIDEODR2 
Extended source colour ZY (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
videoSource 
VIDEODR3 
Extended source colour ZY (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
videoSource 
VIDEODR4 
Extended source colour ZY (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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
videoSource 
VIDEODR5 
Extended source colour ZY (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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
videoSource 
VIDEOv20100513 
Extended source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
videoSource 
VIDEOv20111208 
Extended source colour ZY (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
videoSource 
VIDEOv20201103 
Extended source colour ZY (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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
vikingSource 
VIKINGDR2 
Extended source colour ZY (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
vikingSource 
VIKINGDR3 
Extended source colour ZY (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
vikingSource 
VIKINGDR4 
Extended source colour ZY (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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
vikingSource 
VIKINGDR5 
Extended source colour ZY (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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
vikingSource 
VIKINGv20110714 
Extended source colour ZY (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
vikingSource 
VIKINGv20111019 
Extended source colour ZY (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
vikingSource 
VIKINGv20130417 
Extended source colour ZY (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
vikingSource 
VIKINGv20140402 
Extended source colour ZY (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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
vikingSource 
VIKINGv20150421 
Extended source colour ZY (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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
vikingSource 
VIKINGv20151230 
Extended source colour ZY (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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
vikingSource 
VIKINGv20160406 
Extended source colour ZY (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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
vikingSource 
VIKINGv20161202 
Extended source colour ZY (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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
vikingSource 
VIKINGv20170715 
Extended source colour ZY (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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Extended source colour ZY (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Extended source colour ZY (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
vvvSource 
VVVv20100531 
Extended source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
videoSource 
VIDEODR2 
Error on extended source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
videoSource 
VIDEODR3 
Error on extended source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
videoSource 
VIDEODR4 
Error on extended source colour ZY 
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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
videoSource 
VIDEODR5 
Error on extended source colour ZY 
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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
videoSource 
VIDEOv20100513 
Error on extended source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
videoSource 
VIDEOv20111208 
Error on extended source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
videoSource 
VIDEOv20201103 
Error on extended source colour ZY 
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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
vikingSource 
VIKINGDR2 
Error on extended source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
vikingSource 
VIKINGDR3 
Error on extended source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
vikingSource 
VIKINGDR4 
Error on extended source colour ZY 
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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
vikingSource 
VIKINGDR5 
Error on extended source colour ZY 
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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
vikingSource 
VIKINGv20110714 
Error on extended source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
vikingSource 
VIKINGv20111019 
Error on extended source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
vikingSource 
VIKINGv20130417 
Error on extended source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
vikingSource 
VIKINGv20140402 
Error on extended source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
vikingSource 
VIKINGv20150421 
Error on extended source colour ZY 
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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
vikingSource 
VIKINGv20151230 
Error on extended source colour ZY 
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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
vikingSource 
VIKINGv20160406 
Error on extended source colour ZY 
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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
vikingSource 
VIKINGv20161202 
Error on extended source colour ZY 
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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
vikingSource 
VIKINGv20170715 
Error on extended source colour ZY 
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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Error on extended source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Error on extended source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
vvvSource 
VVVv20100531 
Error on extended source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d 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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d 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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d 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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d 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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtLup 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Extended source colour luptitudeZY (using aperLupNoAperCorr3) 
real 
4 
lup 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtLup 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Extended source colour luptitudeZY (using aperLupNoAperCorr3) 
real 
4 
lup 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtLupErr 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Error on extended source colour luptitude ZY 
real 
4 
lup 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtLupErr 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Error on extended source colour luptitude ZY 
real 
4 
lup 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
videoSource 
VIDEODR2 
Point source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
videoSource 
VIDEODR3 
Point source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
videoSource 
VIDEODR4 
Point source colour ZY (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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
videoSource 
VIDEODR5 
Point source colour ZY (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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
videoSource 
VIDEOv20100513 
Point source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
videoSource 
VIDEOv20111208 
Point source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
videoSource 
VIDEOv20201103 
Point source colour ZY (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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vikingSource 
VIKINGDR2 
Point source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vikingSource 
VIKINGDR3 
Point source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vikingSource 
VIKINGDR4 
Point source colour ZY (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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vikingSource 
VIKINGDR5 
Point source colour ZY (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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vikingSource 
VIKINGv20110714 
Point source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vikingSource 
VIKINGv20111019 
Point source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vikingSource 
VIKINGv20130417 
Point source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vikingSource 
VIKINGv20140402 
Point source colour ZY (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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vikingSource 
VIKINGv20150421 
Point source colour ZY (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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vikingSource 
VIKINGv20151230 
Point source colour ZY (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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vikingSource 
VIKINGv20160406 
Point source colour ZY (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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vikingSource 
VIKINGv20161202 
Point source colour ZY (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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vikingSource 
VIKINGv20170715 
Point source colour ZY (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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Point source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Point source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vvvPsfDophotZYJHKsSource 
VVVDR4 
Point source colour ZY (using PsfMag) 
real 
4 
mag 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vvvPsfDophotZYJHKsSource 
VVVDR5 
Point source colour ZY (using PsfMag) 
real 
4 
mag 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vvvSource 
VVVDR2 
Point source colour ZY (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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vvvSource 
VVVDR4 
Point source colour ZY (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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vvvSource 
VVVDR5 
Point source colour ZY (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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vvvSource 
VVVv20100531 
Point source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vvvSource 
VVVv20110718 
Point source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vvvSource, vvvSynopticSource 
VVVDR1 
Point source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
videoSource 
VIDEODR2 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
videoSource 
VIDEODR3 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
videoSource 
VIDEODR4 
Error on point source colour ZY 
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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
videoSource 
VIDEODR5 
Error on point source colour ZY 
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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
videoSource 
VIDEOv20100513 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
videoSource 
VIDEOv20111208 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
videoSource 
VIDEOv20201103 
Error on point source colour ZY 
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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vikingSource 
VIKINGDR2 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vikingSource 
VIKINGDR3 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vikingSource 
VIKINGDR4 
Error on point source colour ZY 
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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vikingSource 
VIKINGDR5 
Error on point source colour ZY 
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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vikingSource 
VIKINGv20110714 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vikingSource 
VIKINGv20111019 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vikingSource 
VIKINGv20130417 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vikingSource 
VIKINGv20140402 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vikingSource 
VIKINGv20150421 
Error on point source colour ZY 
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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vikingSource 
VIKINGv20151230 
Error on point source colour ZY 
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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vikingSource 
VIKINGv20160406 
Error on point source colour ZY 
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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vikingSource 
VIKINGv20161202 
Error on point source colour ZY 
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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vikingSource 
VIKINGv20170715 
Error on point source colour ZY 
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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vvvPsfDophotZYJHKsSource 
VVVDR4 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vvvPsfDophotZYJHKsSource 
VVVDR5 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vvvSource 
VVVDR2 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vvvSource 
VVVDR4 
Error on point source colour ZY 
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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vvvSource 
VVVDR5 
Error on point source colour ZY 
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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vvvSource 
VVVv20100531 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vvvSource 
VVVv20110718 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vvvSource, vvvSynopticSource 
VVVDR1 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d 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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d 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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d 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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d 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. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntLup 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Point source colour luptitude ZY (using aperLup3) 
real 
4 
lup 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntLup 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Point source colour luptitude ZY (using aperLup3) 
real 
4 
lup 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntLupErr 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Error on point source colour luptitude ZY 
real 
4 
lup 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntLupErr 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Error on point source colour luptitude ZY 
real 
4 
lup 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 
VIDEOv20201103 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
znDofAst 
videoVarFrameSetInfo 
VIDEOv20201103 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
znDofPht 
videoVarFrameSetInfo 
VIDEOv20201103 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared 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 
videoVariability 
VIDEOv20201103 
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 
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 
videoVariability 
VIDEOv20201103 
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 
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 Zband 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 Zband 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 Zband 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 Zband 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 Zband 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 
VIDEOv20201103 
Number of good detections in Zband that are more than 3 sigma deviations (zAperMagN < (zMeanMag3*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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 Zband 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 Zband that are more than 3 sigma deviations (zAperMagN < (zMeanMag3*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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 
videoVariability 
VIDEOv20201103 
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 
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 
VIDEOv20201103 
ellipse fit celestial orientation in Z 
real 
4 
Degrees 
0.9999995e9 
pos.posAng;em.opt.I 
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 
VIKINGDR5 
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 
VVVDR4 
ellipse fit celestial orientation in Z 
real 
4 
Degrees 
0.9999995e9 
pos.posAng;em.opt.I 
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 
videoSource 
VIDEOv20201103 
Extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
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 
VIKINGDR5 
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 
videoSource 
VIDEOv20201103 
Error in extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.opt.I 
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 
VIKINGDR5 
Error in extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;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 postprocessing error bits in Z 
int 
4 

0 
meta.code 
zppErrBits 
videoSource 
VIDEODR3 
additional WFAU postprocessing error bits in Z 
int 
4 

0 
meta.code 
zppErrBits 
videoSource 
VIDEODR4 
additional WFAU postprocessing error bits in Z 
int 
4 

0 
meta.code;em.opt.I 
zppErrBits 
videoSource 
VIDEODR5 
additional WFAU postprocessing error bits in Z 
int 
4 

0 
meta.code;em.opt.I 
zppErrBits 
videoSource 
VIDEOv20111208 
additional WFAU postprocessing error bits in Z 
int 
4 

0 
meta.code 
zppErrBits 
videoSource 
VIDEOv20201103 
additional WFAU postprocessing error bits in Z 
int 
4 

0 
meta.code;em.opt.I 
zppErrBits 
videoSource, videoSourceRemeasurement 
VIDEOv20100513 
additional WFAU postprocessing error bits in Z 
int 
4 

0 
meta.code 
zppErrBits 
vikingSource 
VIKINGDR2 
additional WFAU postprocessing error bits in Z 
int 
4 

0 
meta.code 
Postprocessing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4byte 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 postprocessing error bits in Z 
int 
4 

0 
meta.code 
Postprocessing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4byte 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 postprocessing error bits in Z 
int 
4 

0 
meta.code;em.opt.I 
Postprocessing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4byte 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 
VIKINGDR5 
additional WFAU postprocessing error bits in Z 
int 
4 

0 
meta.code;em.opt.I 
Postprocessing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4byte 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 postprocessing error bits in Z 
int 
4 

0 
meta.code 
Postprocessing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4byte 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 postprocessing error bits in Z 
int 
4 

0 
meta.code 
Postprocessing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4byte 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 postprocessing error bits in Z 
int 
4 

0 
meta.code 
Postprocessing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4byte 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 postprocessing error bits in Z 
int 
4 

0 
meta.code 
Postprocessing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4byte 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 postprocessing error bits in Z 
int 
4 

0 
meta.code;em.opt.I 
Postprocessing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4byte 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 postprocessing error bits in Z 
int 
4 

0 
meta.code;em.opt.I 
Postprocessing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4byte 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 postprocessing error bits in Z 
int 
4 

0 
meta.code;em.opt.I 
Postprocessing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4byte 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 postprocessing error bits in Z 
int 
4 

0 
meta.code;em.opt.I 
Postprocessing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4byte 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 postprocessing error bits in Z 
int 
4 

0 
meta.code;em.opt.I 
Postprocessing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4byte 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 postprocessing error bits in Z 
int 
4 

0 
meta.code 
zppErrBits 
vikingSourceRemeasurement 
VIKINGv20111019 
additional WFAU postprocessing error bits in Z 
int 
4 

0 
meta.code 
zppErrBits 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
additional WFAU postprocessing error bits in Z 
int 
4 

0 
meta.code 
Postprocessing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4byte 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 postprocessing error bits in Z 
int 
4 

0 
meta.code 
Postprocessing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4byte 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 postprocessing error bits in Z 
int 
4 

0 
meta.code 
zppErrBits 
vvvSource 
VVVDR2 
additional WFAU postprocessing error bits in Z 
int 
4 

0 
meta.code 
zppErrBits 
vvvSource 
VVVDR4 
additional WFAU postprocessing error bits in Z 
int 
4 

0 
meta.code;em.opt.I 
zppErrBits 
vvvSource 
VVVDR5 
additional WFAU postprocessing error bits in Z 
int 
4 

0 
meta.code;em.opt.I 
zppErrBits 
vvvSource 
VVVv20110718 
additional WFAU postprocessing error bits in Z 
int 
4 

0 
meta.code 
zppErrBits 
vvvSource, vvvSourceRemeasurement 
VVVv20100531 
additional WFAU postprocessing error bits in Z 
int 
4 

0 
meta.code 
zppErrBits 
vvvSynopticSource 
VVVDR1 
additional WFAU postprocessing error bits in Z 
int 
4 

0 
meta.code 
Postprocessing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4byte 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 postprocessing error bits in Z 
int 
4 

0 
meta.code 
Postprocessing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4byte 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 
VVVDR4 
additional WFAU postprocessing error bits in Z 
int 
4 

0 
meta.code;em.opt.I 
Postprocessing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4byte 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 chisquare (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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquare (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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquare (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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquare (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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquare (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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 
VIDEOv20201103 
Probability of variable from chisquare (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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquare (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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquare (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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
phot.mag 
zPsfMag 
vikingSource 
VIKINGDR3 
Point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
phot.mag 
zPsfMag 
vikingSource 
VIKINGDR4 
Point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zPsfMag 
vikingSource 
VIKINGDR5 
Point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zPsfMag 
vikingSource 
VIKINGv20110714 
Point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
phot.mag 
zPsfMag 
vikingSource 
VIKINGv20111019 
Point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
phot.mag 
zPsfMag 
vikingSource 
VIKINGv20130417 
Point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
phot.mag 
zPsfMag 
vikingSource 
VIKINGv20140402 
Point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zPsfMag 
vikingSource 
VIKINGv20150421 
Point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zPsfMag 
vikingSource 
VIKINGv20151230 
Point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zPsfMag 
vikingSource 
VIKINGv20160406 
Point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zPsfMag 
vikingSource 
VIKINGv20161202 
Point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zPsfMag 
vikingSource 
VIKINGv20170715 
Point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zPsfMag 
vvvPsfDophotZYJHKsSource 
VVVDR4 
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 
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 profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
stat.error 
zPsfMagErr 
vikingSource 
VIKINGDR3 
Error in point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
stat.error 
zPsfMagErr 
vikingSource 
VIKINGDR4 
Error in point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
stat.error;em.opt.I 
zPsfMagErr 
vikingSource 
VIKINGDR5 
Error in point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.opt.I 
zPsfMagErr 
vikingSource 
VIKINGv20110714 
Error in point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
stat.error 
zPsfMagErr 
vikingSource 
VIKINGv20111019 
Error in point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
stat.error 
zPsfMagErr 
vikingSource 
VIKINGv20130417 
Error in point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
stat.error 
zPsfMagErr 
vikingSource 
VIKINGv20140402 
Error in point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
stat.error 
zPsfMagErr 
vikingSource 
VIKINGv20150421 
Error in point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
stat.error;em.opt.I;phot.mag 
zPsfMagErr 
vikingSource 
VIKINGv20151230 
Error in point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.opt.I 
zPsfMagErr 
vikingSource 
VIKINGv20160406 
Error in point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.opt.I 
zPsfMagErr 
vikingSource 
VIKINGv20161202 
Error in point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.opt.I 
zPsfMagErr 
vikingSource 
VIKINGv20170715 
Error in point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.opt.I 
zPsfMagErr 
vvvPsfDophotZYJHKsSource 
VVVDR4 
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 
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 
PSFweighted 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 
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 
VIDEOv20201103 
System of zeropoint (Vega/AB) 
varchar 
16 

'NONE' 

zpSystem 
ExternalProduct 
VIKINGDR4 
System of zeropoint (Vega/AB) 
varchar 
16 

'NONE' 

zpSystem 
ExternalProduct 
VIKINGDR5 
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 
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 
VVVDR4 
System of zeropoint (Vega/AB) 
varchar 
16 

'NONE' 

zpSystem 
ExternalProduct 
VVVDR5 
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 
VIDEOv20201103 
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 
VVVDR5 
System of zeropoint (Vega/AB) 
varchar 
8 

'NONE' 

zq25 
decapsSource 
DECAPS 
25th percentile zband 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 zband 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 zband 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 zband 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 

Zsep 
vvvProperMotionCatalogue 
VVVDR4 
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 

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 
videoSource 
VIDEOv20201103 
the running number of the Z detection 
int 
4 

99999999 
meta.id;em.opt.I 
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 
VIKINGDR5 
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 
VVVDR4 
the running number of the Z detection 
int 
4 

99999999 
meta.number;em.opt.I 
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 (profilefitted) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zSerMag2D 
vikingSource 
VIKINGDR3 
Extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zSerMag2D 
vikingSource 
VIKINGDR4 
Extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zSerMag2D 
vikingSource 
VIKINGDR5 
Extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zSerMag2D 
vikingSource 
VIKINGv20110714 
Extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zSerMag2D 
vikingSource 
VIKINGv20111019 
Extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zSerMag2D 
vikingSource 
VIKINGv20130417 
Extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zSerMag2D 
vikingSource 
VIKINGv20140402 
Extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zSerMag2D 
vikingSource 
VIKINGv20150421 
Extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zSerMag2D 
vikingSource 
VIKINGv20151230 
Extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zSerMag2D 
vikingSource 
VIKINGv20160406 
Extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zSerMag2D 
vikingSource 
VIKINGv20161202 
Extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zSerMag2D 
vikingSource 
VIKINGv20170715 
Extended source Z mag (profilefitted) 
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 (profilefitted) 
real 
4 
mag 
0.9999995e9 
stat.error 
zSerMag2DErr 
vikingSource 
VIKINGDR3 
Error in extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
stat.error 
zSerMag2DErr 
vikingSource 
VIKINGDR4 
Error in extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
stat.error;em.opt.I 
zSerMag2DErr 
vikingSource 
VIKINGDR5 
Error in extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.opt.I 
zSerMag2DErr 
vikingSource 
VIKINGv20110714 
Error in extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
stat.error 
zSerMag2DErr 
vikingSource 
VIKINGv20111019 
Error in extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
stat.error 
zSerMag2DErr 
vikingSource 
VIKINGv20130417 
Error in extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
stat.error 
zSerMag2DErr 
vikingSource 
VIKINGv20140402 
Error in extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
stat.error 
zSerMag2DErr 
vikingSource 
VIKINGv20150421 
Error in extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
stat.error;em.opt.I;phot.mag 
zSerMag2DErr 
vikingSource 
VIKINGv20151230 
Error in extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.opt.I 
zSerMag2DErr 
vikingSource 
VIKINGv20160406 
Error in extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.opt.I 
zSerMag2DErr 
vikingSource 
VIKINGv20161202 
Error in extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.opt.I 
zSerMag2DErr 
vikingSource 
VIKINGv20170715 
Error in extended source Z mag (profilefitted) 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 
VIDEOv20201103 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 zband 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 zband 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 obsfirst 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 obsfirst 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 obsfirst 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 obsfirst 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 obsfirst 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 
VIDEOv20201103 
total period of observations (last obsfirst 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 
vikingVariability 
VIKINGv20110714 
total period of observations (last obsfirst 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 obsfirst 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 
VIDEOv20201103 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 
videoSource 
VIDEOv20201103 
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 
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 
VIKINGDR5 
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 
VVVDR4 
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 
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 
