J 
Name  Schema Table  Database  Description  Type  Length  Unit  Default Value  Unified Content Descriptor 
J 
twomass 
SIXDF 
J magnitude (JEXT) used for J selection 
real 
4 
mag 


j_1AperMag1 
vvvSource 
VVVDR5 
Point source J_1 aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
j_1AperMag1Err 
vvvSource 
VVVDR5 
Error in point source J_1 mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
j_1AperMag3 
vikingSource 
VIKINGv20151230 
Default point source J_1 aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1AperMag3 
vikingSource 
VIKINGv20160406 
Default point source J_1 aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1AperMag3 
vikingSource 
VIKINGv20161202 
Default point source J_1 aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1AperMag3 
vikingSource 
VIKINGv20170715 
Default point source J_1 aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1AperMag3 
vvvSource 
VVVDR5 
Default point source J_1 aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
j_1AperMag3Err 
vikingSource 
VIKINGv20151230 
Error in default point/extended source J_1 mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_1AperMag3Err 
vikingSource 
VIKINGv20160406 
Error in default point/extended source J_1 mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_1AperMag3Err 
vikingSource 
VIKINGv20161202 
Error in default point/extended source J_1 mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_1AperMag3Err 
vikingSource 
VIKINGv20170715 
Error in default point/extended source J_1 mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_1AperMag3Err 
vvvSource 
VVVDR5 
Error in default point source J_1 mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
j_1AperMag4 
vikingSource 
VIKINGv20151230 
Point source J_1 aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1AperMag4 
vikingSource 
VIKINGv20160406 
Point source J_1 aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1AperMag4 
vikingSource 
VIKINGv20161202 
Point source J_1 aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1AperMag4 
vikingSource 
VIKINGv20170715 
Point source J_1 aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1AperMag4 
vvvSource 
VVVDR5 
Point source J_1 aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
j_1AperMag4Err 
vikingSource 
VIKINGv20151230 
Error in point/extended source J_1 mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_1AperMag4Err 
vikingSource 
VIKINGv20160406 
Error in point/extended source J_1 mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_1AperMag4Err 
vikingSource 
VIKINGv20161202 
Error in point/extended source J_1 mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_1AperMag4Err 
vikingSource 
VIKINGv20170715 
Error in point/extended source J_1 mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_1AperMag4Err 
vvvSource 
VVVDR5 
Error in point source J_1 mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
j_1AperMag6 
vikingSource 
VIKINGv20151230 
Point source J_1 aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1AperMag6 
vikingSource 
VIKINGv20160406 
Point source J_1 aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1AperMag6 
vikingSource 
VIKINGv20161202 
Point source J_1 aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1AperMag6 
vikingSource 
VIKINGv20170715 
Point source J_1 aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1AperMag6Err 
vikingSource 
VIKINGv20151230 
Error in point/extended source J_1 mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_1AperMag6Err 
vikingSource 
VIKINGv20160406 
Error in point/extended source J_1 mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_1AperMag6Err 
vikingSource 
VIKINGv20161202 
Error in point/extended source J_1 mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_1AperMag6Err 
vikingSource 
VIKINGv20170715 
Error in point/extended source J_1 mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_1AperMagNoAperCorr3 
vikingSource 
VIKINGv20151230 
Default extended source J_1 aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1AperMagNoAperCorr3 
vikingSource 
VIKINGv20160406 
Default extended source J_1 aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1AperMagNoAperCorr3 
vikingSource 
VIKINGv20161202 
Default extended source J_1 aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1AperMagNoAperCorr3 
vikingSource 
VIKINGv20170715 
Default extended source J_1 aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1AperMagNoAperCorr4 
vikingSource 
VIKINGv20151230 
Extended source J_1 aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1AperMagNoAperCorr4 
vikingSource 
VIKINGv20160406 
Extended source J_1 aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1AperMagNoAperCorr4 
vikingSource 
VIKINGv20161202 
Extended source J_1 aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1AperMagNoAperCorr4 
vikingSource 
VIKINGv20170715 
Extended source J_1 aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1AperMagNoAperCorr6 
vikingSource 
VIKINGv20151230 
Extended source J_1 aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1AperMagNoAperCorr6 
vikingSource 
VIKINGv20160406 
Extended source J_1 aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1AperMagNoAperCorr6 
vikingSource 
VIKINGv20161202 
Extended source J_1 aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1AperMagNoAperCorr6 
vikingSource 
VIKINGv20170715 
Extended source J_1 aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1AverageConf 
vikingSource 
VIKINGv20151230 
average confidence in 2 arcsec diameter default aperture (aper3) J_1 
real 
4 

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

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

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

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

0.9999995e9 
stat.likelihood;em.IR.J 
j_1Class 
vikingSource 
VIKINGv20151230 
discrete image classification flag in J_1 
smallint 
2 

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

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

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

9999 
src.class 
j_1Class 
vvvSource 
VVVDR5 
discrete image classification flag in J_1 
smallint 
2 

9999 
src.class;em.IR.J 
j_1ClassStat 
vikingSource 
VIKINGv20151230 
N(0,1) stellarnessofprofile statistic in J_1 
real 
4 

0.9999995e9 
stat 
j_1ClassStat 
vikingSource 
VIKINGv20160406 
N(0,1) stellarnessofprofile statistic in J_1 
real 
4 

0.9999995e9 
stat 
j_1ClassStat 
vikingSource 
VIKINGv20161202 
N(0,1) stellarnessofprofile statistic in J_1 
real 
4 

0.9999995e9 
stat 
j_1ClassStat 
vikingSource 
VIKINGv20170715 
N(0,1) stellarnessofprofile statistic in J_1 
real 
4 

0.9999995e9 
stat 
j_1ClassStat 
vvvSource 
VVVDR5 
SExtractor classification statistic in J_1 
real 
4 

0.9999995e9 
stat;em.IR.J 
j_1Ell 
vikingSource 
VIKINGv20151230 
1b/a, where a/b=semimajor/minor axes in J_1 
real 
4 

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

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

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

0.9999995e9 
src.ellipticity 
j_1Ell 
vvvSource 
VVVDR5 
1b/a, where a/b=semimajor/minor axes in J_1 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.J 
j_1eNum 
vikingMergeLog 
VIKINGv20151230 
the extension number of this J_1 frame 
tinyint 
1 


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


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


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


meta.number 
j_1eNum 
vvvMergeLog 
VVVDR5 
the extension number of this J_1 frame 
tinyint 
1 


meta.number;em.IR.J 
j_1eNum 
vvvPsfDophotZYJHKsMergeLog 
VVVDR4 
the extension number of this 1st epoch J frame 
tinyint 
1 


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


meta.number;em.IR.J 
j_1ErrBits 
vikingSource 
VIKINGv20151230 
processing warning/error bitwise flags in J_1 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
j_1ErrBits 
vikingSource 
VIKINGv20160406 
processing warning/error bitwise flags in J_1 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
j_1ErrBits 
vikingSource 
VIKINGv20161202 
processing warning/error bitwise flags in J_1 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
j_1ErrBits 
vikingSource 
VIKINGv20170715 
processing warning/error bitwise flags in J_1 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
j_1ErrBits 
vvvSource 
VVVDR5 
processing warning/error bitwise flags in J_1 
int 
4 

99999999 
meta.code;em.IR.J 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
j_1Eta 
vikingSource 
VIKINGv20151230 
Offset of J_1 detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
j_1Eta 
vikingSource 
VIKINGv20160406 
Offset of J_1 detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
j_1Eta 
vikingSource 
VIKINGv20161202 
Offset of J_1 detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
j_1Eta 
vikingSource 
VIKINGv20170715 
Offset of J_1 detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
j_1Eta 
vvvSource 
VVVDR5 
Offset of J_1 detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.J 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
j_1Gausig 
vikingSource 
VIKINGv20151230 
RMS of axes of ellipse fit in J_1 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
j_1Gausig 
vikingSource 
VIKINGv20160406 
RMS of axes of ellipse fit in J_1 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
j_1Gausig 
vikingSource 
VIKINGv20161202 
RMS of axes of ellipse fit in J_1 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
j_1Gausig 
vikingSource 
VIKINGv20170715 
RMS of axes of ellipse fit in J_1 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
j_1Gausig 
vvvSource 
VVVDR5 
RMS of axes of ellipse fit in J_1 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.IR.J 
j_1HlCorSMjRadAs 
vikingSource 
VIKINGv20151230 
Seeing corrected halflight, semimajor axis in J_1 band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
j_1HlCorSMjRadAs 
vikingSource 
VIKINGv20160406 
Seeing corrected halflight, semimajor axis in J_1 band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
j_1HlCorSMjRadAs 
vikingSource 
VIKINGv20161202 
Seeing corrected halflight, semimajor axis in J_1 band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
j_1HlCorSMjRadAs 
vikingSource 
VIKINGv20170715 
Seeing corrected halflight, semimajor axis in J_1 band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
j_1mfID 
vikingMergeLog 
VIKINGv20151230 
the UID of the relevant J_1 multiframe 
bigint 
8 


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


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


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


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


meta.id;obs.field;em.IR.J 
j_1mfID 
vvvPsfDophotZYJHKsMergeLog 
VVVDR4 
the UID of the relevant 1st epoch J tile multiframe 
bigint 
8 


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


meta.id;obs.field;em.IR.J 
j_1mh_1Pnt 
vvvSource 
VVVDR5 
Point source colour J_1H_1 (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.IR.J;em.IR.H 
Default colours from pairs of adjacent passbands within a given set (e.g. 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. 
j_1mh_1PntErr 
vvvSource 
VVVDR5 
Error on point source colour J_1H_1 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;em.IR.H 
Default colours from pairs of adjacent passbands within a given set (e.g. 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. 
j_1mhExt 
vikingSource 
VIKINGv20151230 
Extended source colour J_1H (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.IR.H 
Default colours from pairs of adjacent passbands within a given set (e.g. 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. 
j_1mhExt 
vikingSource 
VIKINGv20160406 
Extended source colour J_1H (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.IR.H 
Default colours from pairs of adjacent passbands within a given set (e.g. 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. 
j_1mhExt 
vikingSource 
VIKINGv20161202 
Extended source colour J_1H (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.IR.H 
Default colours from pairs of adjacent passbands within a given set (e.g. 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. 
j_1mhExt 
vikingSource 
VIKINGv20170715 
Extended source colour J_1H (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.IR.H 
Default colours from pairs of adjacent passbands within a given set (e.g. 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. 
j_1mhExtErr 
vikingSource 
VIKINGv20151230 
Error on extended source colour J_1H 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
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. 
j_1mhExtErr 
vikingSource 
VIKINGv20160406 
Error on extended source colour J_1H 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
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. 
j_1mhExtErr 
vikingSource 
VIKINGv20161202 
Error on extended source colour J_1H 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
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. 
j_1mhExtErr 
vikingSource 
VIKINGv20170715 
Error on extended source colour J_1H 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
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. 
j_1mhPnt 
vikingSource 
VIKINGv20151230 
Point source colour J_1H (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.IR.H 
Default colours from pairs of adjacent passbands within a given set (e.g. 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. 
j_1mhPnt 
vikingSource 
VIKINGv20160406 
Point source colour J_1H (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.IR.H 
Default colours from pairs of adjacent passbands within a given set (e.g. 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. 
j_1mhPnt 
vikingSource 
VIKINGv20161202 
Point source colour J_1H (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.IR.H 
Default colours from pairs of adjacent passbands within a given set (e.g. 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. 
j_1mhPnt 
vikingSource 
VIKINGv20170715 
Point source colour J_1H (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.IR.H 
Default colours from pairs of adjacent passbands within a given set (e.g. 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. 
j_1mhPntErr 
vikingSource 
VIKINGv20151230 
Error on point source colour J_1H 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
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. 
j_1mhPntErr 
vikingSource 
VIKINGv20160406 
Error on point source colour J_1H 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
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. 
j_1mhPntErr 
vikingSource 
VIKINGv20161202 
Error on point source colour J_1H 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
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. 
j_1mhPntErr 
vikingSource 
VIKINGv20170715 
Error on point source colour J_1H 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
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. 
j_1Mjd 
vikingSource 
VIKINGv20151230 
Modified Julian Day in J_1 band 
float 
8 
days 
0.9999995e9 
time.epoch 
j_1Mjd 
vikingSource 
VIKINGv20160406 
Modified Julian Day in J_1 band 
float 
8 
days 
0.9999995e9 
time.epoch 
j_1Mjd 
vikingSource 
VIKINGv20161202 
Modified Julian Day in J_1 band 
float 
8 
days 
0.9999995e9 
time.epoch 
j_1Mjd 
vikingSource 
VIKINGv20170715 
Modified Julian Day in J_1 band 
float 
8 
days 
0.9999995e9 
time.epoch 
j_1Mjd 
vvvPsfDophotZYJHKsMergeLog 
VVVDR4 
the MJD of the 1st epoch J tile multiframe 
float 
8 


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


time;em.IR.J 
j_1Mjd 
vvvSource 
VVVDR5 
Modified Julian Day in J_1 band 
float 
8 
days 
0.9999995e9 
time.epoch;em.IR.J 
j_1PA 
vikingSource 
VIKINGv20151230 
ellipse fit celestial orientation in J_1 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
j_1PA 
vikingSource 
VIKINGv20160406 
ellipse fit celestial orientation in J_1 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
j_1PA 
vikingSource 
VIKINGv20161202 
ellipse fit celestial orientation in J_1 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
j_1PA 
vikingSource 
VIKINGv20170715 
ellipse fit celestial orientation in J_1 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
j_1PA 
vvvSource 
VVVDR5 
ellipse fit celestial orientation in J_1 
real 
4 
Degrees 
0.9999995e9 
pos.posAng;em.IR.J 
j_1PetroMag 
vikingSource 
VIKINGv20151230 
Extended source J_1 mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1PetroMag 
vikingSource 
VIKINGv20160406 
Extended source J_1 mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1PetroMag 
vikingSource 
VIKINGv20161202 
Extended source J_1 mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1PetroMag 
vikingSource 
VIKINGv20170715 
Extended source J_1 mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1PetroMagErr 
vikingSource 
VIKINGv20151230 
Error in extended source J_1 mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_1PetroMagErr 
vikingSource 
VIKINGv20160406 
Error in extended source J_1 mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_1PetroMagErr 
vikingSource 
VIKINGv20161202 
Error in extended source J_1 mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_1PetroMagErr 
vikingSource 
VIKINGv20170715 
Error in extended source J_1 mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_1ppErrBits 
vikingSource 
VIKINGv20151230 
additional WFAU postprocessing error bits in J_1 
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. 
j_1ppErrBits 
vikingSource 
VIKINGv20160406 
additional WFAU postprocessing error bits in J_1 
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. 
j_1ppErrBits 
vikingSource 
VIKINGv20161202 
additional WFAU postprocessing error bits in J_1 
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. 
j_1ppErrBits 
vikingSource 
VIKINGv20170715 
additional WFAU postprocessing error bits in J_1 
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. 
j_1ppErrBits 
vvvSource 
VVVDR5 
additional WFAU postprocessing error bits in J_1 
int 
4 

0 
meta.code;em.IR.J 
j_1PsfMag 
vikingSource 
VIKINGv20151230 
Point source profilefitted J_1 mag 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1PsfMag 
vikingSource 
VIKINGv20160406 
Point source profilefitted J_1 mag 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1PsfMag 
vikingSource 
VIKINGv20161202 
Point source profilefitted J_1 mag 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1PsfMag 
vikingSource 
VIKINGv20170715 
Point source profilefitted J_1 mag 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1PsfMagErr 
vikingSource 
VIKINGv20151230 
Error in point source profilefitted J_1 mag 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_1PsfMagErr 
vikingSource 
VIKINGv20160406 
Error in point source profilefitted J_1 mag 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_1PsfMagErr 
vikingSource 
VIKINGv20161202 
Error in point source profilefitted J_1 mag 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_1PsfMagErr 
vikingSource 
VIKINGv20170715 
Error in point source profilefitted J_1 mag 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_1SeqNum 
vikingSource 
VIKINGv20151230 
the running number of the J_1 detection 
int 
4 

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

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

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

99999999 
meta.number 
j_1SeqNum 
vvvSource 
VVVDR5 
the running number of the J_1 detection 
int 
4 

99999999 
meta.number;em.IR.J 
j_1SerMag2D 
vikingSource 
VIKINGv20151230 
Extended source J_1 mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1SerMag2D 
vikingSource 
VIKINGv20160406 
Extended source J_1 mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1SerMag2D 
vikingSource 
VIKINGv20161202 
Extended source J_1 mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1SerMag2D 
vikingSource 
VIKINGv20170715 
Extended source J_1 mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_1SerMag2DErr 
vikingSource 
VIKINGv20151230 
Error in extended source J_1 mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_1SerMag2DErr 
vikingSource 
VIKINGv20160406 
Error in extended source J_1 mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_1SerMag2DErr 
vikingSource 
VIKINGv20161202 
Error in extended source J_1 mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_1SerMag2DErr 
vikingSource 
VIKINGv20170715 
Error in extended source J_1 mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_1Xi 
vikingSource 
VIKINGv20151230 
Offset of J_1 detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
j_1Xi 
vikingSource 
VIKINGv20160406 
Offset of J_1 detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
j_1Xi 
vikingSource 
VIKINGv20161202 
Offset of J_1 detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
j_1Xi 
vikingSource 
VIKINGv20170715 
Offset of J_1 detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
j_1Xi 
vvvSource 
VVVDR5 
Offset of J_1 detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff;em.IR.J 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
j_2AperMag1 
vvvSource 
VVVDR5 
Point source J_2 aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
j_2AperMag1Err 
vvvSource 
VVVDR5 
Error in point source J_2 mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
j_2AperMag3 
vikingSource 
VIKINGv20151230 
Default point source J_2 aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2AperMag3 
vikingSource 
VIKINGv20160406 
Default point source J_2 aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2AperMag3 
vikingSource 
VIKINGv20161202 
Default point source J_2 aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2AperMag3 
vikingSource 
VIKINGv20170715 
Default point source J_2 aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2AperMag3 
vvvSource 
VVVDR5 
Default point source J_2 aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
j_2AperMag3Err 
vikingSource 
VIKINGv20151230 
Error in default point/extended source J_2 mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_2AperMag3Err 
vikingSource 
VIKINGv20160406 
Error in default point/extended source J_2 mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_2AperMag3Err 
vikingSource 
VIKINGv20161202 
Error in default point/extended source J_2 mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_2AperMag3Err 
vikingSource 
VIKINGv20170715 
Error in default point/extended source J_2 mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_2AperMag3Err 
vvvSource 
VVVDR5 
Error in default point source J_2 mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
j_2AperMag4 
vikingSource 
VIKINGv20151230 
Point source J_2 aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2AperMag4 
vikingSource 
VIKINGv20160406 
Point source J_2 aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2AperMag4 
vikingSource 
VIKINGv20161202 
Point source J_2 aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2AperMag4 
vikingSource 
VIKINGv20170715 
Point source J_2 aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2AperMag4 
vvvSource 
VVVDR5 
Point source J_2 aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
j_2AperMag4Err 
vikingSource 
VIKINGv20151230 
Error in point/extended source J_2 mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_2AperMag4Err 
vikingSource 
VIKINGv20160406 
Error in point/extended source J_2 mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_2AperMag4Err 
vikingSource 
VIKINGv20161202 
Error in point/extended source J_2 mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_2AperMag4Err 
vikingSource 
VIKINGv20170715 
Error in point/extended source J_2 mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_2AperMag4Err 
vvvSource 
VVVDR5 
Error in point source J_2 mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
j_2AperMag6 
vikingSource 
VIKINGv20151230 
Point source J_2 aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2AperMag6 
vikingSource 
VIKINGv20160406 
Point source J_2 aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2AperMag6 
vikingSource 
VIKINGv20161202 
Point source J_2 aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2AperMag6 
vikingSource 
VIKINGv20170715 
Point source J_2 aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2AperMag6Err 
vikingSource 
VIKINGv20151230 
Error in point/extended source J_2 mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_2AperMag6Err 
vikingSource 
VIKINGv20160406 
Error in point/extended source J_2 mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_2AperMag6Err 
vikingSource 
VIKINGv20161202 
Error in point/extended source J_2 mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_2AperMag6Err 
vikingSource 
VIKINGv20170715 
Error in point/extended source J_2 mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_2AperMagNoAperCorr3 
vikingSource 
VIKINGv20151230 
Default extended source J_2 aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2AperMagNoAperCorr3 
vikingSource 
VIKINGv20160406 
Default extended source J_2 aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2AperMagNoAperCorr3 
vikingSource 
VIKINGv20161202 
Default extended source J_2 aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2AperMagNoAperCorr3 
vikingSource 
VIKINGv20170715 
Default extended source J_2 aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2AperMagNoAperCorr4 
vikingSource 
VIKINGv20151230 
Extended source J_2 aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2AperMagNoAperCorr4 
vikingSource 
VIKINGv20160406 
Extended source J_2 aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2AperMagNoAperCorr4 
vikingSource 
VIKINGv20161202 
Extended source J_2 aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2AperMagNoAperCorr4 
vikingSource 
VIKINGv20170715 
Extended source J_2 aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2AperMagNoAperCorr6 
vikingSource 
VIKINGv20151230 
Extended source J_2 aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2AperMagNoAperCorr6 
vikingSource 
VIKINGv20160406 
Extended source J_2 aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2AperMagNoAperCorr6 
vikingSource 
VIKINGv20161202 
Extended source J_2 aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2AperMagNoAperCorr6 
vikingSource 
VIKINGv20170715 
Extended source J_2 aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2AverageConf 
vikingSource 
VIKINGv20151230 
average confidence in 2 arcsec diameter default aperture (aper3) J_2 
real 
4 

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

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

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

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

0.9999995e9 
stat.likelihood;em.IR.J 
j_2Class 
vikingSource 
VIKINGv20151230 
discrete image classification flag in J_2 
smallint 
2 

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

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

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

9999 
src.class 
j_2Class 
vvvSource 
VVVDR5 
discrete image classification flag in J_2 
smallint 
2 

9999 
src.class;em.IR.J 
j_2ClassStat 
vikingSource 
VIKINGv20151230 
N(0,1) stellarnessofprofile statistic in J_2 
real 
4 

0.9999995e9 
stat 
j_2ClassStat 
vikingSource 
VIKINGv20160406 
N(0,1) stellarnessofprofile statistic in J_2 
real 
4 

0.9999995e9 
stat 
j_2ClassStat 
vikingSource 
VIKINGv20161202 
N(0,1) stellarnessofprofile statistic in J_2 
real 
4 

0.9999995e9 
stat 
j_2ClassStat 
vikingSource 
VIKINGv20170715 
N(0,1) stellarnessofprofile statistic in J_2 
real 
4 

0.9999995e9 
stat 
j_2ClassStat 
vvvSource 
VVVDR5 
SExtractor classification statistic in J_2 
real 
4 

0.9999995e9 
stat;em.IR.J 
j_2Ell 
vikingSource 
VIKINGv20151230 
1b/a, where a/b=semimajor/minor axes in J_2 
real 
4 

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

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

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

0.9999995e9 
src.ellipticity 
j_2Ell 
vvvSource 
VVVDR5 
1b/a, where a/b=semimajor/minor axes in J_2 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.J 
j_2eNum 
vikingMergeLog 
VIKINGv20151230 
the extension number of this J_2 frame 
tinyint 
1 


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


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


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


meta.number 
j_2eNum 
vvvMergeLog 
VVVDR5 
the extension number of this J_2 frame 
tinyint 
1 


meta.number;em.IR.J 
j_2eNum 
vvvPsfDophotZYJHKsMergeLog 
VVVDR4 
the extension number of this 2nd epoch J frame 
tinyint 
1 


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


meta.number;em.IR.J 
j_2ErrBits 
vikingSource 
VIKINGv20151230 
processing warning/error bitwise flags in J_2 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
j_2ErrBits 
vikingSource 
VIKINGv20160406 
processing warning/error bitwise flags in J_2 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
j_2ErrBits 
vikingSource 
VIKINGv20161202 
processing warning/error bitwise flags in J_2 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
j_2ErrBits 
vikingSource 
VIKINGv20170715 
processing warning/error bitwise flags in J_2 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
j_2ErrBits 
vvvSource 
VVVDR5 
processing warning/error bitwise flags in J_2 
int 
4 

99999999 
meta.code;em.IR.J 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
j_2Eta 
vikingSource 
VIKINGv20151230 
Offset of J_2 detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
j_2Eta 
vikingSource 
VIKINGv20160406 
Offset of J_2 detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
j_2Eta 
vikingSource 
VIKINGv20161202 
Offset of J_2 detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
j_2Eta 
vikingSource 
VIKINGv20170715 
Offset of J_2 detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
j_2Eta 
vvvSource 
VVVDR5 
Offset of J_2 detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.J 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
j_2Gausig 
vikingSource 
VIKINGv20151230 
RMS of axes of ellipse fit in J_2 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
j_2Gausig 
vikingSource 
VIKINGv20160406 
RMS of axes of ellipse fit in J_2 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
j_2Gausig 
vikingSource 
VIKINGv20161202 
RMS of axes of ellipse fit in J_2 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
j_2Gausig 
vikingSource 
VIKINGv20170715 
RMS of axes of ellipse fit in J_2 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
j_2Gausig 
vvvSource 
VVVDR5 
RMS of axes of ellipse fit in J_2 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.IR.J 
j_2HlCorSMjRadAs 
vikingSource 
VIKINGv20151230 
Seeing corrected halflight, semimajor axis in J_2 band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
j_2HlCorSMjRadAs 
vikingSource 
VIKINGv20160406 
Seeing corrected halflight, semimajor axis in J_2 band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
j_2HlCorSMjRadAs 
vikingSource 
VIKINGv20161202 
Seeing corrected halflight, semimajor axis in J_2 band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
j_2HlCorSMjRadAs 
vikingSource 
VIKINGv20170715 
Seeing corrected halflight, semimajor axis in J_2 band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
j_2mfID 
vikingMergeLog 
VIKINGv20151230 
the UID of the relevant J_2 multiframe 
bigint 
8 


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


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


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


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


meta.id;obs.field;em.IR.J 
j_2mfID 
vvvPsfDophotZYJHKsMergeLog 
VVVDR4 
the UID of the relevant 2nd epoch J tile multiframe 
bigint 
8 


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


meta.id;obs.field;em.IR.J 
j_2mh_2Pnt 
vvvSource 
VVVDR5 
Point source colour J_2H_2 (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.IR.J;em.IR.H 
Default colours from pairs of adjacent passbands within a given set (e.g. 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. 
j_2mh_2PntErr 
vvvSource 
VVVDR5 
Error on point source colour J_2H_2 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;em.IR.H 
Default colours from pairs of adjacent passbands within a given set (e.g. 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. 
j_2Mjd 
vikingSource 
VIKINGv20151230 
Modified Julian Day in J_2 band 
float 
8 
days 
0.9999995e9 
time.epoch 
j_2Mjd 
vikingSource 
VIKINGv20160406 
Modified Julian Day in J_2 band 
float 
8 
days 
0.9999995e9 
time.epoch 
j_2Mjd 
vikingSource 
VIKINGv20161202 
Modified Julian Day in J_2 band 
float 
8 
days 
0.9999995e9 
time.epoch 
j_2Mjd 
vikingSource 
VIKINGv20170715 
Modified Julian Day in J_2 band 
float 
8 
days 
0.9999995e9 
time.epoch 
j_2Mjd 
vvvPsfDophotZYJHKsMergeLog 
VVVDR4 
the MJD of the 2nd epoch J tile multiframe 
float 
8 


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


time;em.IR.J 
j_2Mjd 
vvvSource 
VVVDR5 
Modified Julian Day in J_2 band 
float 
8 
days 
0.9999995e9 
time.epoch;em.IR.J 
j_2mrat 
twomass_scn 
TWOMASS 
Jband average 2nd image moment ratio. 
real 
4 


stat.fit.param 
j_2mrat 
twomass_sixx2_scn 
TWOMASS 
J band average 2nd image moment ratio for scan 
real 
4 



j_2PA 
vikingSource 
VIKINGv20151230 
ellipse fit celestial orientation in J_2 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
j_2PA 
vikingSource 
VIKINGv20160406 
ellipse fit celestial orientation in J_2 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
j_2PA 
vikingSource 
VIKINGv20161202 
ellipse fit celestial orientation in J_2 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
j_2PA 
vikingSource 
VIKINGv20170715 
ellipse fit celestial orientation in J_2 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
j_2PA 
vvvSource 
VVVDR5 
ellipse fit celestial orientation in J_2 
real 
4 
Degrees 
0.9999995e9 
pos.posAng;em.IR.J 
j_2PetroMag 
vikingSource 
VIKINGv20151230 
Extended source J_2 mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2PetroMag 
vikingSource 
VIKINGv20160406 
Extended source J_2 mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2PetroMag 
vikingSource 
VIKINGv20161202 
Extended source J_2 mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2PetroMag 
vikingSource 
VIKINGv20170715 
Extended source J_2 mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2PetroMagErr 
vikingSource 
VIKINGv20151230 
Error in extended source J_2 mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_2PetroMagErr 
vikingSource 
VIKINGv20160406 
Error in extended source J_2 mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_2PetroMagErr 
vikingSource 
VIKINGv20161202 
Error in extended source J_2 mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_2PetroMagErr 
vikingSource 
VIKINGv20170715 
Error in extended source J_2 mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_2ppErrBits 
vikingSource 
VIKINGv20151230 
additional WFAU postprocessing error bits in J_2 
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. 
j_2ppErrBits 
vikingSource 
VIKINGv20160406 
additional WFAU postprocessing error bits in J_2 
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. 
j_2ppErrBits 
vikingSource 
VIKINGv20161202 
additional WFAU postprocessing error bits in J_2 
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. 
j_2ppErrBits 
vikingSource 
VIKINGv20170715 
additional WFAU postprocessing error bits in J_2 
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. 
j_2ppErrBits 
vvvSource 
VVVDR5 
additional WFAU postprocessing error bits in J_2 
int 
4 

0 
meta.code;em.IR.J 
j_2PsfMag 
vikingSource 
VIKINGv20151230 
Point source profilefitted J_2 mag 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2PsfMag 
vikingSource 
VIKINGv20160406 
Point source profilefitted J_2 mag 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2PsfMag 
vikingSource 
VIKINGv20161202 
Point source profilefitted J_2 mag 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2PsfMag 
vikingSource 
VIKINGv20170715 
Point source profilefitted J_2 mag 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2PsfMagErr 
vikingSource 
VIKINGv20151230 
Error in point source profilefitted J_2 mag 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_2PsfMagErr 
vikingSource 
VIKINGv20160406 
Error in point source profilefitted J_2 mag 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_2PsfMagErr 
vikingSource 
VIKINGv20161202 
Error in point source profilefitted J_2 mag 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_2PsfMagErr 
vikingSource 
VIKINGv20170715 
Error in point source profilefitted J_2 mag 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_2SeqNum 
vikingSource 
VIKINGv20151230 
the running number of the J_2 detection 
int 
4 

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

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

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

99999999 
meta.number 
j_2SeqNum 
vvvSource 
VVVDR5 
the running number of the J_2 detection 
int 
4 

99999999 
meta.number;em.IR.J 
j_2SerMag2D 
vikingSource 
VIKINGv20151230 
Extended source J_2 mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2SerMag2D 
vikingSource 
VIKINGv20160406 
Extended source J_2 mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2SerMag2D 
vikingSource 
VIKINGv20161202 
Extended source J_2 mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2SerMag2D 
vikingSource 
VIKINGv20170715 
Extended source J_2 mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
phot.mag 
j_2SerMag2DErr 
vikingSource 
VIKINGv20151230 
Error in extended source J_2 mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_2SerMag2DErr 
vikingSource 
VIKINGv20160406 
Error in extended source J_2 mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_2SerMag2DErr 
vikingSource 
VIKINGv20161202 
Error in extended source J_2 mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_2SerMag2DErr 
vikingSource 
VIKINGv20170715 
Error in extended source J_2 mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag 
j_2Xi 
vikingSource 
VIKINGv20151230 
Offset of J_2 detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
j_2Xi 
vikingSource 
VIKINGv20160406 
Offset of J_2 detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
j_2Xi 
vikingSource 
VIKINGv20161202 
Offset of J_2 detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
j_2Xi 
vikingSource 
VIKINGv20170715 
Offset of J_2 detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
j_2Xi 
vvvSource 
VVVDR5 
Offset of J_2 detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff;em.IR.J 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
j_5sig_ba 
twomass_xsc 
TWOMASS 
J minor/major axis ratio fit to the 5sigma isophote. 
real 
4 


phys.size.axisRatio 
j_5sig_phi 
twomass_xsc 
TWOMASS 
J angle to 5sigma major axis (E of N). 
smallint 
2 
degrees 

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

phot.mag.sb 
j_ba 
twomass_xsc 
TWOMASS 
J minor/major axis ratio fit to the 3sigma isophote. 
real 
4 


phys.size.axisRatio 
j_back 
twomass_xsc 
TWOMASS 
J coadd median background. 
real 
4 


meta.code 
j_bisym_chi 
twomass_xsc 
TWOMASS 
J bisymmetric crosscorrelation chi. 
real 
4 


stat.fit.param 
j_bisym_rat 
twomass_xsc 
TWOMASS 
J bisymmetric flux ratio. 
real 
4 


phot.flux;arith.ratio 
j_bndg_amp 
twomass_xsc 
TWOMASS 
J banding maximum FT amplitude on this side of coadd. 
real 
4 
DN 

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

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


stat.fit.param 
j_cmsig 
twomass_psc 
TWOMASS 
Corrected photometric uncertainty for the default Jband magnitude. 
real 
4 
mag 
Jband 
phot.flux 
j_con_indx 
twomass_xsc 
TWOMASS 
J concentration index r_75%/r_25%. 
real 
4 


phys.size;arith.ratio 
j_d_area 
twomass_xsc 
TWOMASS 
J 5sigma to 3sigma differential area. 
smallint 
2 


stat.fit.residual 
j_flg_10 
twomass_xsc 
TWOMASS 
J confusion flag for 10 arcsec circular ap. mag. 
smallint 
2 


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


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


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


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


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


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


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


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


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



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


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


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


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


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


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


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


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


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


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


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


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


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


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



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


meta.code 
j_h 
twomass_sixx2_psc 
TWOMASS 
The JH color, computed from the Jband and Hband magnitudes (j_m and h_m, respectively) of the source. In cases where the first or second digit in rd_flg is equal to either "0", "4", "6", or "9", no color is computed because the photometry in one or both bands is of lower quality or the source is not detected. 
real 
4 



j_k 
twomass_sixx2_psc 
TWOMASS 
The JKs color, computed from the Jband and Ksband magnitudes (j_m and k_m, respectively) of the source. In cases where the first or third digit in rd_flg is equal to either "0", "4", "6", or "9", no color is computed because the photometry in one or both bands is of lower quality or the source is not detected. 
real 
4 



j_m 
twomass_psc 
TWOMASS 
Default Jband magnitude 
real 
4 
mag 

phot.flux 
j_m 
twomass_sixx2_psc 
TWOMASS 
J selected "default" magnitude 
real 
4 
mag 


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

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

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

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

phot.flux 
j_m_2mass 
allwise_sc 
WISE 
2MASS Jband magnitude or magnitude upper limit of the associated 2MASS PSC source. This column is "null" if there is no associated 2MASS PSC source or if the 2MASS PSC Jband magnitude entry is "null". 
float 
8 
mag 


j_m_2mass 
wise_allskysc 
WISE 
2MASS Jband magnitude or magnitude upper limit of the associated 2MASS PSC source. This column is default if there is no associated 2MASS PSC source or if the 2MASS PSC Jband magnitude entry is default. 
real 
4 
mag 
0.9999995e9 

j_m_2mass 
wise_prelimsc 
WISE 
2MASS Jband magnitude or magnitude upper limit of the associated 2MASS PSC source This column is default if there is no associated 2MASS PSC source or if the 2MASS PSC Jband magnitude entry is default 
real 
4 
mag 
0.9999995e9 

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

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

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

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

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

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


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

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

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

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

phot.flux 
j_m_ext 
twomass_sixx2_xsc 
TWOMASS 
J mag from fit extrapolation 
real 
4 
mag 


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

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

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

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

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

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

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

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

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

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

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


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


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

phot.flux 
j_m_stdap 
twomass_psc 
TWOMASS 
Jband "standard" aperture magnitude. 
real 
4 
mag 

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

phot.flux 
j_mnsurfb_eff 
twomass_xsc 
TWOMASS 
J mean surface brightness at the halflight radius. 
real 
4 
mag 

phot.mag.sb 
j_msig 
twomass_sixx2_psc 
TWOMASS 
J "default" mag uncertainty 
real 
4 
mag 


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

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

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

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

stat.error 
j_msig_2mass 
allwise_sc 
WISE 
2MASS Jband corrected photometric uncertainty of the associated 2MASS PSC source. This column is "null" if there is no associated 2MASS PSC source or if the 2MASS PSC Jband uncertainty entry is "null". 
float 
8 
mag 


j_msig_2mass 
wise_allskysc 
WISE 
2MASS Jband corrected photometric uncertainty of the associated 2MASS PSC source. This column is default if there is no associated 2MASS PSC source or if the 2MASS PSC Jband uncertainty entry is default. 
real 
4 
mag 
0.9999995e9 

j_msig_2mass 
wise_prelimsc 
WISE 
2MASS Jband corrected photometric uncertainty of the associated 2MASS PSC source This column is default if there is no associated 2MASS PSC source or if the 2MASS PSC Jband uncertainty entry is default 
real 
4 
mag 
0.9999995e9 

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

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

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

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

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

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


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

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

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

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

stat.error 
j_msig_ext 
twomass_sixx2_xsc 
TWOMASS 
J 1sigma uncertainty in mag from fit extrapolation 
real 
4 
mag 


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

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

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

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

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

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

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

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

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

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

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

stat.error 
j_msig_stdap 
twomass_psc 
TWOMASS 
Uncertainty in the Jband standard aperture magnitude. 
real 
4 
mag 

phot.flux 
j_msig_sys 
twomass_xsc 
TWOMASS 
J 1sigma uncertainty in system photometry mag. 
real 
4 
mag 

stat.error 
j_msigcom 
twomass_psc 
TWOMASS 
Combined, or total photometric uncertainty for the default Jband magnitude. 
real 
4 
mag 
Jband 
phot.flux 
j_msigcom 
twomass_sixx2_psc 
TWOMASS 
combined (total) J band photometric uncertainty 
real 
4 
mag 


j_msnr10 
twomass_scn 
TWOMASS 
The estimated Jband magnitude at which SNR=10 is achieved for this scan. 
real 
4 
mag 

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


j_n_snr10 
twomass_scn 
TWOMASS 
Number of point sources at Jband with SNR>10 (instrumental mag <=15.8) 
int 
4 


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



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


stat.fit.param 
j_peak 
twomass_xsc 
TWOMASS 
J peak pixel brightness. 
real 
4 
mag 

phot.mag.sb 
j_perc_darea 
twomass_xsc 
TWOMASS 
J 5sigma to 3sigma percent area change. 
smallint 
2 


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

pos.posAng 
j_psfchi 
twomass_psc 
TWOMASS 
Reduced chisquared goodnessoffit value for the Jband profilefit photometry made on the 1.3 s "Read_2" exposures. 
real 
4 


stat.fit.param 
j_psp 
twomass_scn 
TWOMASS 
Jband photometric sensitivity paramater (PSP). 
real 
4 


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



j_pts_noise 
twomass_scn 
TWOMASS 
Base10 logarithm of the mode of the noise distribution for all point source detections in the scan, where the noise is estimated from the measured Jband photometric errors and is expressed in units of mJy. 
real 
4 


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


j_r_c 
twomass_xsc 
TWOMASS 
J Kron circular aperture radius. 
real 
4 
arcsec 

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

phys.angSize;src 
j_r_eff 
twomass_xsc 
TWOMASS 
J halflight (integrated halfflux point) radius. 
real 
4 
arcsec 

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

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

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

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

phys.angSize;src 
j_resid_ann 
twomass_xsc 
TWOMASS 
J residual annulus background median. 
real 
4 
DN 

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


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


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


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


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


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


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


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


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


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


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


FIT_PARAM 
j_shape_avg 
twomass_scn 
TWOMASS 
Jband average seeing shape for scan. 
real 
4 


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



j_shape_rms 
twomass_scn 
TWOMASS 
RMSerror of Jband average seeing shape. 
real 
4 


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



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


FIT_PARAM 
j_snr 
twomass_psc 
TWOMASS 
Jband "scan" signaltonoise ratio. 
real 
4 
mag 

instr.det.noise 
j_snr 
twomass_sixx2_psc 
TWOMASS 
J band "scan" signaltonoise ratio 
real 
4 



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


meta.code 
j_zp_ap 
twomass_scn 
TWOMASS 
Photometric zeropoint for Jband aperture photometry. 
real 
4 
mag 

phot.mag;arith.zp 
j_zp_ap 
twomass_sixx2_scn 
TWOMASS 
J band ap. calibration photometric zeropoint for scan 
real 
4 
mag 


jAmpl 
vmcCepheidVariables 
VMCDR4 
PeaktoPeak amplitude in J band {catalogue TType keyword: A(J)} 
real 
4 
mag 
0.9999995e9 
src.var.amplitude;em.IR.J 
jAmpl 
vmcCepheidVariables 
VMCv20160311 
PeaktoPeak amplitude in J band {catalogue TType keyword: A(J)} 
real 
4 
mag 
0.9999995e9 
src.var.amplitude;em.IR.J 
jAmpl 
vmcCepheidVariables 
VMCv20160822 
PeaktoPeak amplitude in J band {catalogue TType keyword: A(J)} 
real 
4 
mag 
0.9999995e9 
src.var.amplitude;em.IR.J 
jAmpl 
vmcCepheidVariables 
VMCv20170109 
PeaktoPeak amplitude in J band {catalogue TType keyword: A(J)} 
real 
4 
mag 
0.9999995e9 
src.var.amplitude;em.IR.J 
jAmpl 
vmcCepheidVariables 
VMCv20170411 
PeaktoPeak amplitude in J band {catalogue TType keyword: A(J)} 
real 
4 
mag 
0.9999995e9 
src.var.amplitude;em.IR.J 
jAmpl 
vmcCepheidVariables 
VMCv20171101 
PeaktoPeak amplitude in J band {catalogue TType keyword: A(J)} 
real 
4 
mag 
0.9999995e9 
src.var.amplitude;em.IR.J 
jAmpl 
vmcCepheidVariables 
VMCv20180702 
PeaktoPeak amplitude in J band {catalogue TType keyword: A(J)} 
real 
4 
mag 
0.9999995e9 
src.var.amplitude;em.IR.J 
jAmpl 
vmcCepheidVariables 
VMCv20181120 
PeaktoPeak amplitude in J band {catalogue TType keyword: A(J)} 
real 
4 
mag 
0.9999995e9 
src.var.amplitude;em.IR.J 
jAmplErr 
vmcCepheidVariables 
VMCDR4 
Error in PeaktoPeak amplitude in J band {catalogue TType keyword: e_A(J)} 
real 
4 
mag 
0.9999995e9 
stat.error;src.var.amplitude;em.IR.J 
jAmplErr 
vmcCepheidVariables 
VMCv20160311 
Error in PeaktoPeak amplitude in J band {catalogue TType keyword: e_A(J)} 
real 
4 
mag 
0.9999995e9 
stat.error;src.var.amplitude;em.IR.J 
jAmplErr 
vmcCepheidVariables 
VMCv20160822 
Error in PeaktoPeak amplitude in J band {catalogue TType keyword: e_A(J)} 
real 
4 
mag 
0.9999995e9 
stat.error;src.var.amplitude;em.IR.J 
jAmplErr 
vmcCepheidVariables 
VMCv20170109 
Error in PeaktoPeak amplitude in J band {catalogue TType keyword: e_A(J)} 
real 
4 
mag 
0.9999995e9 
stat.error;src.var.amplitude;em.IR.J 
jAmplErr 
vmcCepheidVariables 
VMCv20170411 
Error in PeaktoPeak amplitude in J band {catalogue TType keyword: e_A(J)} 
real 
4 
mag 
0.9999995e9 
stat.error;src.var.amplitude;em.IR.J 
jAmplErr 
vmcCepheidVariables 
VMCv20171101 
Error in PeaktoPeak amplitude in J band {catalogue TType keyword: e_A(J)} 
real 
4 
mag 
0.9999995e9 
stat.error;src.var.amplitude;em.IR.J 
jAmplErr 
vmcCepheidVariables 
VMCv20180702 
Error in PeaktoPeak amplitude in J band {catalogue TType keyword: e_A(J)} 
real 
4 
mag 
0.9999995e9 
stat.error;src.var.amplitude;em.IR.J 
jAmplErr 
vmcCepheidVariables 
VMCv20181120 
Error in PeaktoPeak amplitude in J band {catalogue TType keyword: e_A(J)} 
real 
4 
mag 
0.9999995e9 
stat.error;src.var.amplitude;em.IR.J 
jAperJky3 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Default point source J aperture corrected (2.0 arcsec aperture diameter) calibrated flux If in doubt use this flux estimator 
real 
4 
jansky 
0.9999995e9 
phot.flux 
jAperJky3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Default point source J aperture corrected (2.0 arcsec aperture diameter) calibrated flux If in doubt use this flux estimator 
real 
4 
jansky 
0.9999995e9 
phot.flux 
jAperJky3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Default point source J aperture corrected (2.0 arcsec aperture diameter) calibrated flux If in doubt use this flux estimator 
real 
4 
jansky 
0.9999995e9 
phot.flux 
jAperJky3Err 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Error in default point/extended source J (2.0 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
stat.error 
jAperJky3Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Error in default point/extended source J (2.0 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
stat.error 
jAperJky3Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Error in default point/extended source J (2.0 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
stat.error 
jAperJky4 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Point source J aperture corrected (2.8 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
jAperJky4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Point source J aperture corrected (2.8 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
jAperJky4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Point source J aperture corrected (2.8 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
jAperJky4Err 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Error in point/extended source J (2.8 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
stat.error 
jAperJky4Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Error in point/extended source J (2.8 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
stat.error 
jAperJky4Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Error in point/extended source J (2.8 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
stat.error 
jAperJky6 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Point source J aperture corrected (5.7 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
jAperJky6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Point source J aperture corrected (5.7 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
jAperJky6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Point source J aperture corrected (5.7 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
jAperJky6Err 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Error in point/extended source J (5.7 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
stat.error 
jAperJky6Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Error in point/extended source J (5.7 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
stat.error 
jAperJky6Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Error in point/extended source J (5.7 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
stat.error 
jAperJkyNoAperCorr3 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Default extended source J (2.0 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux If in doubt use this flux estimator 
real 
4 
jansky 
0.9999995e9 
phot.flux 
jAperJkyNoAperCorr3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Default extended source J (2.0 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux If in doubt use this flux estimator 
real 
4 
jansky 
0.9999995e9 
phot.flux 
jAperJkyNoAperCorr3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Default extended source J (2.0 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux If in doubt use this flux estimator 
real 
4 
jansky 
0.9999995e9 
phot.flux 
jAperJkyNoAperCorr4 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Extended source J (2.8 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
jAperJkyNoAperCorr4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Extended source J (2.8 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
jAperJkyNoAperCorr4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Extended source J (2.8 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
jAperJkyNoAperCorr6 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Extended source J (5.7 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
jAperJkyNoAperCorr6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Extended source J (5.7 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
jAperJkyNoAperCorr6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Extended source J (5.7 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
jAperLup3 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Default point source J aperture corrected (2.0 arcsec aperture diameter) luptitude If in doubt use this flux estimator 
real 
4 
lup 
0.9999995e9 
phot.lup 
jAperLup3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Default point source J aperture corrected (2.0 arcsec aperture diameter) luptitude If in doubt use this flux estimator 
real 
4 
lup 
0.9999995e9 
phot.lup 
jAperLup3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Default point source J aperture corrected (2.0 arcsec aperture diameter) luptitude If in doubt use this flux estimator 
real 
4 
lup 
0.9999995e9 
phot.lup 
jAperLup3Err 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Error in default point/extended source J (2.0 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
stat.error 
jAperLup3Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Error in default point/extended source J (2.0 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
stat.error 
jAperLup3Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Error in default point/extended source J (2.0 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
stat.error 
jAperLup4 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Point source J aperture corrected (2.8 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
jAperLup4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Point source J aperture corrected (2.8 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
jAperLup4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Point source J aperture corrected (2.8 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
jAperLup4Err 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Error in point/extended source J (2.8 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
stat.error 
jAperLup4Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Error in point/extended source J (2.8 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
stat.error 
jAperLup4Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Error in point/extended source J (2.8 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
stat.error 
jAperLup6 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Point source J aperture corrected (5.7 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
jAperLup6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Point source J aperture corrected (5.7 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
jAperLup6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Point source J aperture corrected (5.7 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
jAperLup6Err 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Error in point/extended source J (5.7 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
stat.error 
jAperLup6Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Error in point/extended source J (5.7 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
stat.error 
jAperLup6Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Error in point/extended source J (5.7 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
stat.error 
jAperLupNoAperCorr3 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Default extended source J (2.0 arcsec aperture diameter, but no aperture correction applied) aperture luptitude If in doubt use this flux estimator 
real 
4 
lup 
0.9999995e9 
phot.lup 
jAperLupNoAperCorr3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Default extended source J (2.0 arcsec aperture diameter, but no aperture correction applied) aperture luptitude If in doubt use this flux estimator 
real 
4 
lup 
0.9999995e9 
phot.lup 
jAperLupNoAperCorr3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Default extended source J (2.0 arcsec aperture diameter, but no aperture correction applied) aperture luptitude If in doubt use this flux estimator 
real 
4 
lup 
0.9999995e9 
phot.lup 
jAperLupNoAperCorr4 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Extended source J (2.8 arcsec aperture diameter, but no aperture correction applied) aperture luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
jAperLupNoAperCorr4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Extended source J (2.8 arcsec aperture diameter, but no aperture correction applied) aperture luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
jAperLupNoAperCorr4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Extended source J (2.8 arcsec aperture diameter, but no aperture correction applied) aperture luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
jAperLupNoAperCorr6 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Extended source J (5.7 arcsec aperture diameter, but no aperture correction applied) aperture luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
jAperLupNoAperCorr6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Extended source J (5.7 arcsec aperture diameter, but no aperture correction applied) aperture luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
jAperLupNoAperCorr6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Extended source J (5.7 arcsec aperture diameter, but no aperture correction applied) aperture luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
jAperMag1 
vmcSynopticSource 
VMCDR1 
Extended source J aperture corrected mag (0.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag1 
vmcSynopticSource 
VMCDR2 
Extended source J aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag1 
vmcSynopticSource 
VMCDR3 
Extended source J aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag1 
vmcSynopticSource 
VMCDR4 
Extended source J aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag1 
vmcSynopticSource 
VMCDR5 
Extended source J aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag1 
vmcSynopticSource 
VMCv20110816 
Extended source J aperture corrected mag (0.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag1 
vmcSynopticSource 
VMCv20110909 
Extended source J aperture corrected mag (0.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag1 
vmcSynopticSource 
VMCv20120126 
Extended source J aperture corrected mag (0.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag1 
vmcSynopticSource 
VMCv20121128 
Extended source J aperture corrected mag (0.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag1 
vmcSynopticSource 
VMCv20130304 
Extended source J aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag1 
vmcSynopticSource 
VMCv20130805 
Extended source J aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag1 
vmcSynopticSource 
VMCv20140428 
Extended source J aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag1 
vmcSynopticSource 
VMCv20140903 
Extended source J aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag1 
vmcSynopticSource 
VMCv20150309 
Extended source J aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag1 
vmcSynopticSource 
VMCv20151218 
Extended source J aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag1 
vmcSynopticSource 
VMCv20160311 
Extended source J aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag1 
vmcSynopticSource 
VMCv20160822 
Extended source J aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag1 
vmcSynopticSource 
VMCv20170109 
Extended source J aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag1 
vmcSynopticSource 
VMCv20170411 
Extended source J aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag1 
vmcSynopticSource 
VMCv20171101 
Extended source J aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag1 
vmcSynopticSource 
VMCv20180702 
Extended source J aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag1 
vmcSynopticSource 
VMCv20181120 
Extended source J aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag1 
vvvSource 
VVVDR4 
Point source J aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag1 
vvvSource 
VVVDR5 
Point source J aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag1 
vvvSynopticSource 
VVVDR4 
Extended source J aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag1Err 
vmcSynopticSource 
VMCDR1 
Error in extended source J mag (0.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag1Err 
vmcSynopticSource 
VMCDR2 
Error in extended source J mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag1Err 
vmcSynopticSource 
VMCDR3 
Error in extended source J mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag1Err 
vmcSynopticSource 
VMCDR4 
Error in extended source J mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag1Err 
vmcSynopticSource 
VMCDR5 
Error in extended source J mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag1Err 
vmcSynopticSource 
VMCv20110816 
Error in extended source J mag (0.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag1Err 
vmcSynopticSource 
VMCv20110909 
Error in extended source J mag (0.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag1Err 
vmcSynopticSource 
VMCv20120126 
Error in extended source J mag (0.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag1Err 
vmcSynopticSource 
VMCv20121128 
Error in extended source J mag (0.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag1Err 
vmcSynopticSource 
VMCv20130304 
Error in extended source J mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag1Err 
vmcSynopticSource 
VMCv20130805 
Error in extended source J mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag1Err 
vmcSynopticSource 
VMCv20140428 
Error in extended source J mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J 
jAperMag1Err 
vmcSynopticSource 
VMCv20140903 
Error in extended source J mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag1Err 
vmcSynopticSource 
VMCv20150309 
Error in extended source J mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag1Err 
vmcSynopticSource 
VMCv20151218 
Error in extended source J mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag1Err 
vmcSynopticSource 
VMCv20160311 
Error in extended source J mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag1Err 
vmcSynopticSource 
VMCv20160822 
Error in extended source J mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag1Err 
vmcSynopticSource 
VMCv20170109 
Error in extended source J mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag1Err 
vmcSynopticSource 
VMCv20170411 
Error in extended source J mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag1Err 
vmcSynopticSource 
VMCv20171101 
Error in extended source J mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag1Err 
vmcSynopticSource 
VMCv20180702 
Error in extended source J mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag1Err 
vmcSynopticSource 
VMCv20181120 
Error in extended source J mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag1Err 
vvvSource 
VVVDR4 
Error in point source J mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag1Err 
vvvSource 
VVVDR5 
Error in point source J mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag1Err 
vvvSynopticSource 
VVVDR4 
Error in extended source J mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag2 
vmcSynopticSource 
VMCDR1 
Extended source J aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag2 
vmcSynopticSource 
VMCDR2 
Extended source J aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag2 
vmcSynopticSource 
VMCDR3 
Extended source J aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag2 
vmcSynopticSource 
VMCDR4 
Extended source J aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag2 
vmcSynopticSource 
VMCDR5 
Extended source J aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag2 
vmcSynopticSource 
VMCv20110816 
Extended source J aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag2 
vmcSynopticSource 
VMCv20110909 
Extended source J aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag2 
vmcSynopticSource 
VMCv20120126 
Extended source J aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag2 
vmcSynopticSource 
VMCv20121128 
Extended source J aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag2 
vmcSynopticSource 
VMCv20130304 
Extended source J aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag2 
vmcSynopticSource 
VMCv20130805 
Extended source J aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag2 
vmcSynopticSource 
VMCv20140428 
Extended source J aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag2 
vmcSynopticSource 
VMCv20140903 
Extended source J aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag2 
vmcSynopticSource 
VMCv20150309 
Extended source J aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag2 
vmcSynopticSource 
VMCv20151218 
Extended source J aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag2 
vmcSynopticSource 
VMCv20160311 
Extended source J aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag2 
vmcSynopticSource 
VMCv20160822 
Extended source J aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag2 
vmcSynopticSource 
VMCv20170109 
Extended source J aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag2 
vmcSynopticSource 
VMCv20170411 
Extended source J aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag2 
vmcSynopticSource 
VMCv20171101 
Extended source J aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag2 
vmcSynopticSource 
VMCv20180702 
Extended source J aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag2 
vmcSynopticSource 
VMCv20181120 
Extended source J aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag2 
vvvSynopticSource 
VVVDR4 
Extended source J aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag2Err 
vmcSynopticSource 
VMCDR1 
Error in extended source J mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag2Err 
vmcSynopticSource 
VMCDR2 
Error in extended source J mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag2Err 
vmcSynopticSource 
VMCDR3 
Error in extended source J mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag2Err 
vmcSynopticSource 
VMCDR4 
Error in extended source J mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag2Err 
vmcSynopticSource 
VMCDR5 
Error in extended source J mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag2Err 
vmcSynopticSource 
VMCv20110816 
Error in extended source J mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag2Err 
vmcSynopticSource 
VMCv20110909 
Error in extended source J mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag2Err 
vmcSynopticSource 
VMCv20120126 
Error in extended source J mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag2Err 
vmcSynopticSource 
VMCv20121128 
Error in extended source J mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag2Err 
vmcSynopticSource 
VMCv20130304 
Error in extended source J mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag2Err 
vmcSynopticSource 
VMCv20130805 
Error in extended source J mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag2Err 
vmcSynopticSource 
VMCv20140428 
Error in extended source J mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J 
jAperMag2Err 
vmcSynopticSource 
VMCv20140903 
Error in extended source J mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag2Err 
vmcSynopticSource 
VMCv20150309 
Error in extended source J mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag2Err 
vmcSynopticSource 
VMCv20151218 
Error in extended source J mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag2Err 
vmcSynopticSource 
VMCv20160311 
Error in extended source J mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag2Err 
vmcSynopticSource 
VMCv20160822 
Error in extended source J mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag2Err 
vmcSynopticSource 
VMCv20170109 
Error in extended source J mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag2Err 
vmcSynopticSource 
VMCv20170411 
Error in extended source J mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag2Err 
vmcSynopticSource 
VMCv20171101 
Error in extended source J mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag2Err 
vmcSynopticSource 
VMCv20180702 
Error in extended source J mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag2Err 
vmcSynopticSource 
VMCv20181120 
Error in extended source J mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag2Err 
vvvSynopticSource 
VVVDR4 
Error in extended source J mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag3 
ultravistaSource 
ULTRAVISTADR4 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Default point source J aperture corrected (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag3 
vhsSource 
VHSDR1 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag3 
vhsSource 
VHSDR2 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag3 
vhsSource 
VHSDR3 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vhsSource 
VHSDR4 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vhsSource 
VHSDR5 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vhsSource 
VHSDR6 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vhsSource 
VHSv20120926 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag3 
vhsSource 
VHSv20130417 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag3 
vhsSource 
VHSv20140409 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vhsSource 
VHSv20150108 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vhsSource 
VHSv20160114 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vhsSource 
VHSv20160507 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vhsSource 
VHSv20170630 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vhsSource 
VHSv20180419 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
videoSource 
VIDEODR2 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag3 
videoSource 
VIDEODR3 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag3 
videoSource 
VIDEODR4 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
videoSource 
VIDEODR5 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
videoSource 
VIDEOv20100513 
Default point/extended source J mag, no aperture correction applied If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag3 
videoSource 
VIDEOv20111208 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag3 
vikingSource 
VIKINGDR2 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag3 
vikingSource 
VIKINGDR3 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag3 
vikingSource 
VIKINGDR4 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vikingSource 
VIKINGv20110714 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag3 
vikingSource 
VIKINGv20111019 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag3 
vikingSource 
VIKINGv20130417 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag3 
vikingSource 
VIKINGv20140402 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vikingSource 
VIKINGv20150421 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vikingSource 
VIKINGv20151230 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vikingSource 
VIKINGv20160406 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vikingSource 
VIKINGv20161202 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vikingSource 
VIKINGv20170715 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Default point source J aperture corrected (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Default point source J aperture corrected (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag3 
vmcSource 
VMCDR1 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag3 
vmcSource 
VMCDR2 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vmcSource 
VMCDR3 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vmcSource 
VMCDR4 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vmcSource 
VMCDR5 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vmcSource 
VMCv20110816 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag3 
vmcSource 
VMCv20110909 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag3 
vmcSource 
VMCv20120126 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag3 
vmcSource 
VMCv20121128 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag3 
vmcSource 
VMCv20130304 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag3 
vmcSource 
VMCv20130805 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vmcSource 
VMCv20140428 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vmcSource 
VMCv20140903 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vmcSource 
VMCv20150309 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vmcSource 
VMCv20151218 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vmcSource 
VMCv20160311 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vmcSource 
VMCv20160822 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vmcSource 
VMCv20170109 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vmcSource 
VMCv20170411 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vmcSource 
VMCv20171101 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vmcSource 
VMCv20180702 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vmcSource 
VMCv20181120 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vmcSynopticSource 
VMCDR1 
Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag3 
vmcSynopticSource 
VMCDR2 
Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vmcSynopticSource 
VMCDR3 
Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vmcSynopticSource 
VMCDR4 
Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vmcSynopticSource 
VMCDR5 
Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vmcSynopticSource 
VMCv20110816 
Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag3 
vmcSynopticSource 
VMCv20110909 
Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag3 
vmcSynopticSource 
VMCv20120126 
Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag3 
vmcSynopticSource 
VMCv20121128 
Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag3 
vmcSynopticSource 
VMCv20130304 
Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag3 
vmcSynopticSource 
VMCv20130805 
Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vmcSynopticSource 
VMCv20140428 
Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vmcSynopticSource 
VMCv20140903 
Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vmcSynopticSource 
VMCv20150309 
Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vmcSynopticSource 
VMCv20151218 
Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vmcSynopticSource 
VMCv20160311 
Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vmcSynopticSource 
VMCv20160822 
Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vmcSynopticSource 
VMCv20170109 
Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vmcSynopticSource 
VMCv20170411 
Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vmcSynopticSource 
VMCv20171101 
Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vmcSynopticSource 
VMCv20180702 
Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vmcSynopticSource 
VMCv20181120 
Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vvvSource 
VVVDR4 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vvvSource 
VVVDR5 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vvvSynopticSource 
VVVDR4 
Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag3 
vvvVivaCatalogue 
VVVDR4 
J magnitude using aperture corrected mag (2.0 arcsec aperture diameter, from VVVDR4 1st epoch JHKs contemporaneous OB) {catalogue TType keyword: jAperMag3} 
real 
4 
mag 
9.999995e8 

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

jAperMag3Err 
ultravistaSource 
ULTRAVISTADR4 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag3Err 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Error in default point/extended source J (2.0 arcsec aperture diameter) magnitude 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag3Err 
vhsSource 
VHSDR1 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag3Err 
vhsSource 
VHSDR2 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag3Err 
vhsSource 
VHSDR3 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J 
jAperMag3Err 
vhsSource 
VHSDR4 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag3Err 
vhsSource 
VHSDR5 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag3Err 
vhsSource 
VHSDR6 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag3Err 
vhsSource 
VHSv20120926 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag3Err 
vhsSource 
VHSv20130417 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag3Err 
vhsSource 
VHSv20140409 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J 
jAperMag3Err 
vhsSource 
VHSv20150108 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag3Err 
vhsSource 
VHSv20160114 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag3Err 
vhsSource 
VHSv20160507 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag3Err 
vhsSource 
VHSv20170630 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag3Err 
vhsSource 
VHSv20180419 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag3Err 
videoSource 
VIDEODR2 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag3Err 
videoSource 
VIDEODR3 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag3Err 
videoSource 
VIDEODR4 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag3Err 
videoSource 
VIDEODR5 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag3Err 
videoSource 
VIDEOv20100513 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag3Err 
videoSource 
VIDEOv20111208 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag3Err 
vikingSource 
VIKINGDR2 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag3Err 
vikingSource 
VIKINGDR3 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag3Err 
vikingSource 
VIKINGDR4 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J 
jAperMag3Err 
vikingSource 
VIKINGv20110714 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag3Err 
vikingSource 
VIKINGv20111019 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag3Err 
vikingSource 
VIKINGv20130417 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag3Err 
vikingSource 
VIKINGv20140402 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag3Err 
vikingSource 
VIKINGv20150421 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag3Err 
vikingSource 
VIKINGv20151230 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag3Err 
vikingSource 
VIKINGv20160406 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag3Err 
vikingSource 
VIKINGv20161202 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag3Err 
vikingSource 
VIKINGv20170715 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag3Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Error in default point/extended source J (2.0 arcsec aperture diameter) magnitude 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag3Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Error in default point/extended source J (2.0 arcsec aperture diameter) magnitude 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag3Err 
vmcSource 
VMCDR2 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag3Err 
vmcSource 
VMCDR3 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag3Err 
vmcSource 
VMCDR4 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag3Err 
vmcSource 
VMCDR5 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag3Err 
vmcSource 
VMCv20110816 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag3Err 
vmcSource 
VMCv20110909 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag3Err 
vmcSource 
VMCv20120126 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag3Err 
vmcSource 
VMCv20121128 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag3Err 
vmcSource 
VMCv20130304 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag3Err 
vmcSource 
VMCv20130805 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag3Err 
vmcSource 
VMCv20140428 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J 
jAperMag3Err 
vmcSource 
VMCv20140903 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag3Err 
vmcSource 
VMCv20150309 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag3Err 
vmcSource 
VMCv20151218 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag3Err 
vmcSource 
VMCv20160311 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag3Err 
vmcSource 
VMCv20160822 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag3Err 
vmcSource 
VMCv20170109 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag3Err 
vmcSource 
VMCv20170411 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag3Err 
vmcSource 
VMCv20171101 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag3Err 
vmcSource 
VMCv20180702 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag3Err 
vmcSource 
VMCv20181120 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag3Err 
vmcSource, vmcSynopticSource 
VMCDR1 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag3Err 
vvvSource 
VVVDR4 
Error in default point source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag3Err 
vvvSource 
VVVDR5 
Error in default point source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag3Err 
vvvSynopticSource 
VVVDR4 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag3Err 
vvvVivaCatalogue 
VVVDR4 
Error in default point source J mag, from VVVDR4 {catalogue TType keyword: jAperMag3Err} 
real 
4 
mag 
9.999995e8 

jAperMag3Err 
vvvVivaCatalogue 
VVVDR5 
Error in default point source J mag, from VVVDR4 {catalogue TType keyword: jAperMag3Err} 
real 
4 
mag 
9.999995e8 

jAperMag4 
ultravistaSource 
ULTRAVISTADR4 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Point source J aperture corrected (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag4 
vhsSource 
VHSDR1 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag4 
vhsSource 
VHSDR2 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag4 
vhsSource 
VHSDR3 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vhsSource 
VHSDR4 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vhsSource 
VHSDR5 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vhsSource 
VHSDR6 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vhsSource 
VHSv20120926 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag4 
vhsSource 
VHSv20130417 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag4 
vhsSource 
VHSv20140409 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vhsSource 
VHSv20150108 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vhsSource 
VHSv20160114 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vhsSource 
VHSv20160507 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vhsSource 
VHSv20170630 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vhsSource 
VHSv20180419 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
videoSource 
VIDEODR2 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag4 
videoSource 
VIDEODR3 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag4 
videoSource 
VIDEODR4 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
videoSource 
VIDEODR5 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
videoSource 
VIDEOv20100513 
Extended source J mag, no aperture correction applied 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag4 
videoSource 
VIDEOv20111208 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag4 
vikingSource 
VIKINGDR2 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag4 
vikingSource 
VIKINGDR3 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag4 
vikingSource 
VIKINGDR4 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vikingSource 
VIKINGv20110714 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag4 
vikingSource 
VIKINGv20111019 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag4 
vikingSource 
VIKINGv20130417 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag4 
vikingSource 
VIKINGv20140402 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vikingSource 
VIKINGv20150421 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vikingSource 
VIKINGv20151230 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vikingSource 
VIKINGv20160406 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vikingSource 
VIKINGv20161202 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vikingSource 
VIKINGv20170715 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Point source J aperture corrected (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Point source J aperture corrected (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag4 
vmcSource 
VMCDR1 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag4 
vmcSource 
VMCDR2 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vmcSource 
VMCDR3 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vmcSource 
VMCDR4 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vmcSource 
VMCDR5 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vmcSource 
VMCv20110816 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag4 
vmcSource 
VMCv20110909 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag4 
vmcSource 
VMCv20120126 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag4 
vmcSource 
VMCv20121128 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag4 
vmcSource 
VMCv20130304 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag4 
vmcSource 
VMCv20130805 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vmcSource 
VMCv20140428 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vmcSource 
VMCv20140903 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vmcSource 
VMCv20150309 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vmcSource 
VMCv20151218 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vmcSource 
VMCv20160311 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vmcSource 
VMCv20160822 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vmcSource 
VMCv20170109 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vmcSource 
VMCv20170411 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vmcSource 
VMCv20171101 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vmcSource 
VMCv20180702 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vmcSource 
VMCv20181120 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vmcSynopticSource 
VMCDR1 
Extended source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag4 
vmcSynopticSource 
VMCDR2 
Extended source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vmcSynopticSource 
VMCDR3 
Extended source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vmcSynopticSource 
VMCDR4 
Extended source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vmcSynopticSource 
VMCDR5 
Extended source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vmcSynopticSource 
VMCv20110816 
Extended source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag4 
vmcSynopticSource 
VMCv20110909 
Extended source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag4 
vmcSynopticSource 
VMCv20120126 
Extended source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag4 
vmcSynopticSource 
VMCv20121128 
Extended source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag4 
vmcSynopticSource 
VMCv20130304 
Extended source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag4 
vmcSynopticSource 
VMCv20130805 
Extended source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vmcSynopticSource 
VMCv20140428 
Extended source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vmcSynopticSource 
VMCv20140903 
Extended source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vmcSynopticSource 
VMCv20150309 
Extended source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vmcSynopticSource 
VMCv20151218 
Extended source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vmcSynopticSource 
VMCv20160311 
Extended source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vmcSynopticSource 
VMCv20160822 
Extended source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vmcSynopticSource 
VMCv20170109 
Extended source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vmcSynopticSource 
VMCv20170411 
Extended source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vmcSynopticSource 
VMCv20171101 
Extended source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vmcSynopticSource 
VMCv20180702 
Extended source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vmcSynopticSource 
VMCv20181120 
Extended source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vvvSource 
VVVDR4 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vvvSource 
VVVDR5 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4 
vvvSynopticSource 
VVVDR4 
Extended source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag4Err 
ultravistaSource 
ULTRAVISTADR4 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag4Err 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Error in point/extended source J (2.8 arcsec aperture diameter) magnitude 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag4Err 
vhsSource 
VHSDR1 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag4Err 
vhsSource 
VHSDR2 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag4Err 
vhsSource 
VHSDR3 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J 
jAperMag4Err 
vhsSource 
VHSDR4 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag4Err 
vhsSource 
VHSDR5 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag4Err 
vhsSource 
VHSDR6 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag4Err 
vhsSource 
VHSv20120926 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag4Err 
vhsSource 
VHSv20130417 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag4Err 
vhsSource 
VHSv20140409 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J 
jAperMag4Err 
vhsSource 
VHSv20150108 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag4Err 
vhsSource 
VHSv20160114 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag4Err 
vhsSource 
VHSv20160507 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag4Err 
vhsSource 
VHSv20170630 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag4Err 
vhsSource 
VHSv20180419 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag4Err 
videoSource 
VIDEODR2 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag4Err 
videoSource 
VIDEODR3 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag4Err 
videoSource 
VIDEODR4 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag4Err 
videoSource 
VIDEODR5 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag4Err 
videoSource 
VIDEOv20100513 
Error in extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag4Err 
videoSource 
VIDEOv20111208 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag4Err 
vikingSource 
VIKINGDR2 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag4Err 
vikingSource 
VIKINGDR3 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag4Err 
vikingSource 
VIKINGDR4 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J 
jAperMag4Err 
vikingSource 
VIKINGv20110714 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag4Err 
vikingSource 
VIKINGv20111019 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag4Err 
vikingSource 
VIKINGv20130417 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag4Err 
vikingSource 
VIKINGv20140402 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag4Err 
vikingSource 
VIKINGv20150421 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag4Err 
vikingSource 
VIKINGv20151230 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag4Err 
vikingSource 
VIKINGv20160406 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag4Err 
vikingSource 
VIKINGv20161202 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag4Err 
vikingSource 
VIKINGv20170715 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag4Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Error in point/extended source J (2.8 arcsec aperture diameter) magnitude 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag4Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Error in point/extended source J (2.8 arcsec aperture diameter) magnitude 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag4Err 
vmcSource 
VMCDR1 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag4Err 
vmcSource 
VMCDR2 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag4Err 
vmcSource 
VMCDR3 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag4Err 
vmcSource 
VMCDR4 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag4Err 
vmcSource 
VMCDR5 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag4Err 
vmcSource 
VMCv20110816 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag4Err 
vmcSource 
VMCv20110909 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag4Err 
vmcSource 
VMCv20120126 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag4Err 
vmcSource 
VMCv20121128 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag4Err 
vmcSource 
VMCv20130304 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag4Err 
vmcSource 
VMCv20130805 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag4Err 
vmcSource 
VMCv20140428 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J 
jAperMag4Err 
vmcSource 
VMCv20140903 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag4Err 
vmcSource 
VMCv20150309 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag4Err 
vmcSource 
VMCv20151218 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag4Err 
vmcSource 
VMCv20160311 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag4Err 
vmcSource 
VMCv20160822 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag4Err 
vmcSource 
VMCv20170109 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag4Err 
vmcSource 
VMCv20170411 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag4Err 
vmcSource 
VMCv20171101 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag4Err 
vmcSource 
VMCv20180702 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag4Err 
vmcSource 
VMCv20181120 
Error in point/extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag4Err 
vmcSynopticSource 
VMCDR1 
Error in extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag4Err 
vmcSynopticSource 
VMCDR2 
Error in extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag4Err 
vmcSynopticSource 
VMCDR3 
Error in extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag4Err 
vmcSynopticSource 
VMCDR4 
Error in extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag4Err 
vmcSynopticSource 
VMCDR5 
Error in extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag4Err 
vmcSynopticSource 
VMCv20110816 
Error in extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag4Err 
vmcSynopticSource 
VMCv20110909 
Error in extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag4Err 
vmcSynopticSource 
VMCv20120126 
Error in extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag4Err 
vmcSynopticSource 
VMCv20121128 
Error in extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag4Err 
vmcSynopticSource 
VMCv20130304 
Error in extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag4Err 
vmcSynopticSource 
VMCv20130805 
Error in extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag4Err 
vmcSynopticSource 
VMCv20140428 
Error in extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J 
jAperMag4Err 
vmcSynopticSource 
VMCv20140903 
Error in extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag4Err 
vmcSynopticSource 
VMCv20150309 
Error in extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag4Err 
vmcSynopticSource 
VMCv20151218 
Error in extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag4Err 
vmcSynopticSource 
VMCv20160311 
Error in extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag4Err 
vmcSynopticSource 
VMCv20160822 
Error in extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag4Err 
vmcSynopticSource 
VMCv20170109 
Error in extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag4Err 
vmcSynopticSource 
VMCv20170411 
Error in extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag4Err 
vmcSynopticSource 
VMCv20171101 
Error in extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag4Err 
vmcSynopticSource 
VMCv20180702 
Error in extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag4Err 
vmcSynopticSource 
VMCv20181120 
Error in extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag4Err 
vvvSource 
VVVDR4 
Error in point source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag4Err 
vvvSource 
VVVDR5 
Error in point source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag4Err 
vvvSynopticSource 
VVVDR4 
Error in extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag5 
vmcSynopticSource 
VMCDR1 
Extended source J aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag5 
vmcSynopticSource 
VMCDR2 
Extended source J aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag5 
vmcSynopticSource 
VMCDR3 
Extended source J aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag5 
vmcSynopticSource 
VMCDR4 
Extended source J aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag5 
vmcSynopticSource 
VMCDR5 
Extended source J aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag5 
vmcSynopticSource 
VMCv20110816 
Extended source J aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag5 
vmcSynopticSource 
VMCv20110909 
Extended source J aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag5 
vmcSynopticSource 
VMCv20120126 
Extended source J aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag5 
vmcSynopticSource 
VMCv20121128 
Extended source J aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag5 
vmcSynopticSource 
VMCv20130304 
Extended source J aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag5 
vmcSynopticSource 
VMCv20130805 
Extended source J aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag5 
vmcSynopticSource 
VMCv20140428 
Extended source J aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag5 
vmcSynopticSource 
VMCv20140903 
Extended source J aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag5 
vmcSynopticSource 
VMCv20150309 
Extended source J aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag5 
vmcSynopticSource 
VMCv20151218 
Extended source J aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag5 
vmcSynopticSource 
VMCv20160311 
Extended source J aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag5 
vmcSynopticSource 
VMCv20160822 
Extended source J aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag5 
vmcSynopticSource 
VMCv20170109 
Extended source J aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag5 
vmcSynopticSource 
VMCv20170411 
Extended source J aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag5 
vmcSynopticSource 
VMCv20171101 
Extended source J aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag5 
vmcSynopticSource 
VMCv20180702 
Extended source J aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag5 
vmcSynopticSource 
VMCv20181120 
Extended source J aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag5 
vvvSynopticSource 
VVVDR4 
Extended source J aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag5Err 
vmcSynopticSource 
VMCDR1 
Error in extended source J mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag5Err 
vmcSynopticSource 
VMCDR2 
Error in extended source J mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag5Err 
vmcSynopticSource 
VMCDR3 
Error in extended source J mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag5Err 
vmcSynopticSource 
VMCDR4 
Error in extended source J mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag5Err 
vmcSynopticSource 
VMCDR5 
Error in extended source J mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag5Err 
vmcSynopticSource 
VMCv20110816 
Error in extended source J mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag5Err 
vmcSynopticSource 
VMCv20110909 
Error in extended source J mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag5Err 
vmcSynopticSource 
VMCv20120126 
Error in extended source J mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag5Err 
vmcSynopticSource 
VMCv20121128 
Error in extended source J mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag5Err 
vmcSynopticSource 
VMCv20130304 
Error in extended source J mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag5Err 
vmcSynopticSource 
VMCv20130805 
Error in extended source J mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag5Err 
vmcSynopticSource 
VMCv20140428 
Error in extended source J mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J 
jAperMag5Err 
vmcSynopticSource 
VMCv20140903 
Error in extended source J mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag5Err 
vmcSynopticSource 
VMCv20150309 
Error in extended source J mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag5Err 
vmcSynopticSource 
VMCv20151218 
Error in extended source J mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag5Err 
vmcSynopticSource 
VMCv20160311 
Error in extended source J mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag5Err 
vmcSynopticSource 
VMCv20160822 
Error in extended source J mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag5Err 
vmcSynopticSource 
VMCv20170109 
Error in extended source J mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag5Err 
vmcSynopticSource 
VMCv20170411 
Error in extended source J mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag5Err 
vmcSynopticSource 
VMCv20171101 
Error in extended source J mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag5Err 
vmcSynopticSource 
VMCv20180702 
Error in extended source J mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag5Err 
vmcSynopticSource 
VMCv20181120 
Error in extended source J mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag5Err 
vvvSynopticSource 
VVVDR4 
Error in extended source J mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag6 
ultravistaSource 
ULTRAVISTADR4 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Point source J aperture corrected (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag6 
vhsSource 
VHSDR1 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag6 
vhsSource 
VHSDR2 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag6 
vhsSource 
VHSDR3 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
vhsSource 
VHSDR4 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
vhsSource 
VHSDR5 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
vhsSource 
VHSDR6 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
vhsSource 
VHSv20120926 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag6 
vhsSource 
VHSv20130417 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag6 
vhsSource 
VHSv20140409 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
vhsSource 
VHSv20150108 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
vhsSource 
VHSv20160114 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
vhsSource 
VHSv20160507 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
vhsSource 
VHSv20170630 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
vhsSource 
VHSv20180419 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
videoSource 
VIDEODR2 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag6 
videoSource 
VIDEODR3 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag6 
videoSource 
VIDEODR4 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
videoSource 
VIDEODR5 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
videoSource 
VIDEOv20100513 
Extended source J mag, no aperture correction applied 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag6 
videoSource 
VIDEOv20111208 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag6 
vikingSource 
VIKINGDR2 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag6 
vikingSource 
VIKINGDR3 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag6 
vikingSource 
VIKINGDR4 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
vikingSource 
VIKINGv20110714 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag6 
vikingSource 
VIKINGv20111019 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag6 
vikingSource 
VIKINGv20130417 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag6 
vikingSource 
VIKINGv20140402 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
vikingSource 
VIKINGv20150421 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
vikingSource 
VIKINGv20151230 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
vikingSource 
VIKINGv20160406 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
vikingSource 
VIKINGv20161202 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
vikingSource 
VIKINGv20170715 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Point source J aperture corrected (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Point source J aperture corrected (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag6 
vmcSource 
VMCDR1 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag6 
vmcSource 
VMCDR2 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
vmcSource 
VMCDR3 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
vmcSource 
VMCDR4 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
vmcSource 
VMCDR5 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
vmcSource 
VMCv20110816 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag6 
vmcSource 
VMCv20110909 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag6 
vmcSource 
VMCv20120126 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag6 
vmcSource 
VMCv20121128 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag6 
vmcSource 
VMCv20130304 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag6 
vmcSource 
VMCv20130805 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
vmcSource 
VMCv20140428 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
vmcSource 
VMCv20140903 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
vmcSource 
VMCv20150309 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
vmcSource 
VMCv20151218 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
vmcSource 
VMCv20160311 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
vmcSource 
VMCv20160822 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
vmcSource 
VMCv20170109 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
vmcSource 
VMCv20170411 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
vmcSource 
VMCv20171101 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
vmcSource 
VMCv20180702 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6 
vmcSource 
VMCv20181120 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMag6Err 
ultravistaSource 
ULTRAVISTADR4 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag6Err 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Error in point/extended source J (5.7 arcsec aperture diameter) magnitude 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag6Err 
vhsSource 
VHSDR1 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag6Err 
vhsSource 
VHSDR2 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag6Err 
vhsSource 
VHSDR3 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J 
jAperMag6Err 
vhsSource 
VHSDR4 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag6Err 
vhsSource 
VHSDR5 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag6Err 
vhsSource 
VHSDR6 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag6Err 
vhsSource 
VHSv20120926 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag6Err 
vhsSource 
VHSv20130417 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag6Err 
vhsSource 
VHSv20140409 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J 
jAperMag6Err 
vhsSource 
VHSv20150108 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag6Err 
vhsSource 
VHSv20160114 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag6Err 
vhsSource 
VHSv20160507 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag6Err 
vhsSource 
VHSv20170630 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag6Err 
vhsSource 
VHSv20180419 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag6Err 
videoSource 
VIDEODR2 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag6Err 
videoSource 
VIDEODR3 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag6Err 
videoSource 
VIDEODR4 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag6Err 
videoSource 
VIDEODR5 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag6Err 
videoSource 
VIDEOv20100513 
Error in extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag6Err 
videoSource 
VIDEOv20111208 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag6Err 
vikingSource 
VIKINGDR2 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag6Err 
vikingSource 
VIKINGDR3 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag6Err 
vikingSource 
VIKINGDR4 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J 
jAperMag6Err 
vikingSource 
VIKINGv20110714 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag6Err 
vikingSource 
VIKINGv20111019 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag6Err 
vikingSource 
VIKINGv20130417 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag6Err 
vikingSource 
VIKINGv20140402 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag6Err 
vikingSource 
VIKINGv20150421 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag6Err 
vikingSource 
VIKINGv20151230 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag6Err 
vikingSource 
VIKINGv20160406 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag6Err 
vikingSource 
VIKINGv20161202 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag6Err 
vikingSource 
VIKINGv20170715 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag6Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Error in point/extended source J (5.7 arcsec aperture diameter) magnitude 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag6Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Error in point/extended source J (5.7 arcsec aperture diameter) magnitude 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag6Err 
vmcSource 
VMCDR1 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag6Err 
vmcSource 
VMCDR2 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag6Err 
vmcSource 
VMCDR3 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag6Err 
vmcSource 
VMCDR4 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag6Err 
vmcSource 
VMCDR5 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag6Err 
vmcSource 
VMCv20110816 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag6Err 
vmcSource 
VMCv20110909 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag6Err 
vmcSource 
VMCv20120126 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag6Err 
vmcSource 
VMCv20121128 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag6Err 
vmcSource 
VMCv20130304 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag6Err 
vmcSource 
VMCv20130805 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag6Err 
vmcSource 
VMCv20140428 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J 
jAperMag6Err 
vmcSource 
VMCv20140903 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag6Err 
vmcSource 
VMCv20150309 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.J;phot.mag 
jAperMag6Err 
vmcSource 
VMCv20151218 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag6Err 
vmcSource 
VMCv20160311 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag6Err 
vmcSource 
VMCv20160822 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag6Err 
vmcSource 
VMCv20170109 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag6Err 
vmcSource 
VMCv20170411 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag6Err 
vmcSource 
VMCv20171101 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag6Err 
vmcSource 
VMCv20180702 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMag6Err 
vmcSource 
VMCv20181120 
Error in point/extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.J 
jAperMagNoAperCorr3 
ultravistaSource 
ULTRAVISTADR4 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Default extended source J (2.0 arcsec aperture diameter, but no aperture correction applied) aperture magnitude If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr3 
vhsSource 
VHSDR1 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr3 
vhsSource 
VHSDR2 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr3 
vhsSource 
VHSDR3 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
vhsSource 
VHSDR4 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
vhsSource 
VHSDR5 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
vhsSource 
VHSDR6 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
vhsSource 
VHSv20120926 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr3 
vhsSource 
VHSv20130417 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr3 
vhsSource 
VHSv20140409 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
vhsSource 
VHSv20150108 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
vhsSource 
VHSv20160114 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
vhsSource 
VHSv20160507 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
vhsSource 
VHSv20170630 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
vhsSource 
VHSv20180419 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
videoSource 
VIDEODR2 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr3 
videoSource 
VIDEODR3 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr3 
videoSource 
VIDEODR4 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
videoSource 
VIDEODR5 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
videoSource 
VIDEOv20111208 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr3 
vikingSource 
VIKINGDR2 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr3 
vikingSource 
VIKINGDR3 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr3 
vikingSource 
VIKINGDR4 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
vikingSource 
VIKINGv20110714 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr3 
vikingSource 
VIKINGv20111019 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr3 
vikingSource 
VIKINGv20130417 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr3 
vikingSource 
VIKINGv20140402 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
vikingSource 
VIKINGv20150421 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
vikingSource 
VIKINGv20151230 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
vikingSource 
VIKINGv20160406 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
vikingSource 
VIKINGv20161202 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
vikingSource 
VIKINGv20170715 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Default extended source J (2.0 arcsec aperture diameter, but no aperture correction applied) aperture magnitude If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Default extended source J (2.0 arcsec aperture diameter, but no aperture correction applied) aperture magnitude If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr3 
vmcSource 
VMCDR1 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr3 
vmcSource 
VMCDR2 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
vmcSource 
VMCDR3 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
vmcSource 
VMCDR4 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
vmcSource 
VMCDR5 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
vmcSource 
VMCv20110816 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr3 
vmcSource 
VMCv20110909 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr3 
vmcSource 
VMCv20120126 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr3 
vmcSource 
VMCv20121128 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr3 
vmcSource 
VMCv20130304 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr3 
vmcSource 
VMCv20130805 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
vmcSource 
VMCv20140428 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
vmcSource 
VMCv20140903 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
vmcSource 
VMCv20150309 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
vmcSource 
VMCv20151218 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
vmcSource 
VMCv20160311 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
vmcSource 
VMCv20160822 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
vmcSource 
VMCv20170109 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
vmcSource 
VMCv20170411 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
vmcSource 
VMCv20171101 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
vmcSource 
VMCv20180702 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr3 
vmcSource 
VMCv20181120 
Default extended source J aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
ultravistaSource 
ULTRAVISTADR4 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Extended source J (2.8 arcsec aperture diameter, but no aperture correction applied) aperture magnitude 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr4 
vhsSource 
VHSDR1 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr4 
vhsSource 
VHSDR2 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr4 
vhsSource 
VHSDR3 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
vhsSource 
VHSDR4 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
vhsSource 
VHSDR5 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
vhsSource 
VHSDR6 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
vhsSource 
VHSv20120926 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr4 
vhsSource 
VHSv20130417 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr4 
vhsSource 
VHSv20140409 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
vhsSource 
VHSv20150108 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
vhsSource 
VHSv20160114 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
vhsSource 
VHSv20160507 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
vhsSource 
VHSv20170630 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
vhsSource 
VHSv20180419 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
videoSource 
VIDEODR2 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr4 
videoSource 
VIDEODR3 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr4 
videoSource 
VIDEODR4 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
videoSource 
VIDEODR5 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
videoSource 
VIDEOv20111208 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr4 
vikingSource 
VIKINGDR2 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr4 
vikingSource 
VIKINGDR3 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr4 
vikingSource 
VIKINGDR4 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
vikingSource 
VIKINGv20110714 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr4 
vikingSource 
VIKINGv20111019 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr4 
vikingSource 
VIKINGv20130417 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr4 
vikingSource 
VIKINGv20140402 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
vikingSource 
VIKINGv20150421 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
vikingSource 
VIKINGv20151230 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
vikingSource 
VIKINGv20160406 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
vikingSource 
VIKINGv20161202 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
vikingSource 
VIKINGv20170715 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Extended source J (2.8 arcsec aperture diameter, but no aperture correction applied) aperture magnitude 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Extended source J (2.8 arcsec aperture diameter, but no aperture correction applied) aperture magnitude 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr4 
vmcSource 
VMCDR1 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr4 
vmcSource 
VMCDR2 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
vmcSource 
VMCDR3 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
vmcSource 
VMCDR4 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
vmcSource 
VMCDR5 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
vmcSource 
VMCv20110816 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr4 
vmcSource 
VMCv20110909 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr4 
vmcSource 
VMCv20120126 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr4 
vmcSource 
VMCv20121128 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr4 
vmcSource 
VMCv20130304 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr4 
vmcSource 
VMCv20130805 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
vmcSource 
VMCv20140428 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
vmcSource 
VMCv20140903 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
vmcSource 
VMCv20150309 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
vmcSource 
VMCv20151218 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
vmcSource 
VMCv20160311 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
vmcSource 
VMCv20160822 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
vmcSource 
VMCv20170109 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
vmcSource 
VMCv20170411 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
vmcSource 
VMCv20171101 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
vmcSource 
VMCv20180702 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr4 
vmcSource 
VMCv20181120 
Extended source J aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
ultravistaSource 
ULTRAVISTADR4 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Extended source J (5.7 arcsec aperture diameter, but no aperture correction applied) aperture magnitude 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr6 
vhsSource 
VHSDR1 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr6 
vhsSource 
VHSDR2 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr6 
vhsSource 
VHSDR3 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
vhsSource 
VHSDR4 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
vhsSource 
VHSDR5 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
vhsSource 
VHSDR6 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
vhsSource 
VHSv20120926 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr6 
vhsSource 
VHSv20130417 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr6 
vhsSource 
VHSv20140409 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
vhsSource 
VHSv20150108 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
vhsSource 
VHSv20160114 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
vhsSource 
VHSv20160507 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
vhsSource 
VHSv20170630 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
vhsSource 
VHSv20180419 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
videoSource 
VIDEODR2 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr6 
videoSource 
VIDEODR3 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr6 
videoSource 
VIDEODR4 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
videoSource 
VIDEODR5 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
videoSource 
VIDEOv20111208 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr6 
vikingSource 
VIKINGDR2 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr6 
vikingSource 
VIKINGDR3 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr6 
vikingSource 
VIKINGDR4 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
vikingSource 
VIKINGv20110714 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr6 
vikingSource 
VIKINGv20111019 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr6 
vikingSource 
VIKINGv20130417 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr6 
vikingSource 
VIKINGv20140402 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
vikingSource 
VIKINGv20150421 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
vikingSource 
VIKINGv20151230 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
vikingSource 
VIKINGv20160406 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
vikingSource 
VIKINGv20161202 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
vikingSource 
VIKINGv20170715 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Extended source J (5.7 arcsec aperture diameter, but no aperture correction applied) aperture magnitude 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Extended source J (5.7 arcsec aperture diameter, but no aperture correction applied) aperture magnitude 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr6 
vmcSource 
VMCDR1 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr6 
vmcSource 
VMCDR2 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
vmcSource 
VMCDR3 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
vmcSource 
VMCDR4 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
vmcSource 
VMCDR5 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
vmcSource 
VMCv20110816 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr6 
vmcSource 
VMCv20110909 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr6 
vmcSource 
VMCv20120126 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr6 
vmcSource 
VMCv20121128 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr6 
vmcSource 
VMCv20130304 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr6 
vmcSource 
VMCv20130805 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
vmcSource 
VMCv20140428 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
vmcSource 
VMCv20140903 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
vmcSource 
VMCv20150309 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
vmcSource 
VMCv20151218 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
vmcSource 
VMCv20160311 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
vmcSource 
VMCv20160822 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
vmcSource 
VMCv20170109 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
vmcSource 
VMCv20170411 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
vmcSource 
VMCv20171101 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
vmcSource 
VMCv20180702 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jAperMagNoAperCorr6 
vmcSource 
VMCv20181120 
Extended source J aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jaStratAst 
ultravistaVarFrameSetInfo 
ULTRAVISTADR4 
Parameter, c0 from FerreiraLopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
videoVarFrameSetInfo 
VIDEODR2 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
videoVarFrameSetInfo 
VIDEODR3 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
videoVarFrameSetInfo 
VIDEODR4 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
videoVarFrameSetInfo 
VIDEODR5 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
videoVarFrameSetInfo 
VIDEOv20100513 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
videoVarFrameSetInfo 
VIDEOv20111208 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vikingVarFrameSetInfo 
VIKINGDR2 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vikingVarFrameSetInfo 
VIKINGDR3 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vikingVarFrameSetInfo 
VIKINGDR4 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vikingVarFrameSetInfo 
VIKINGv20110714 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vikingVarFrameSetInfo 
VIKINGv20111019 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vikingVarFrameSetInfo 
VIKINGv20130417 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vikingVarFrameSetInfo 
VIKINGv20140402 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vikingVarFrameSetInfo 
VIKINGv20150421 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vikingVarFrameSetInfo 
VIKINGv20151230 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vikingVarFrameSetInfo 
VIKINGv20160406 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vikingVarFrameSetInfo 
VIKINGv20161202 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vikingVarFrameSetInfo 
VIKINGv20170715 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vmcVarFrameSetInfo 
VMCDR1 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vmcVarFrameSetInfo 
VMCDR2 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vmcVarFrameSetInfo 
VMCDR3 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vmcVarFrameSetInfo 
VMCDR4 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vmcVarFrameSetInfo 
VMCDR5 
Parameter, c0 from FerreiraLopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vmcVarFrameSetInfo 
VMCv20110816 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vmcVarFrameSetInfo 
VMCv20110909 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vmcVarFrameSetInfo 
VMCv20120126 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vmcVarFrameSetInfo 
VMCv20121128 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vmcVarFrameSetInfo 
VMCv20130304 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vmcVarFrameSetInfo 
VMCv20130805 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vmcVarFrameSetInfo 
VMCv20140428 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vmcVarFrameSetInfo 
VMCv20140903 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vmcVarFrameSetInfo 
VMCv20150309 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vmcVarFrameSetInfo 
VMCv20151218 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vmcVarFrameSetInfo 
VMCv20160311 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vmcVarFrameSetInfo 
VMCv20160822 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vmcVarFrameSetInfo 
VMCv20170109 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vmcVarFrameSetInfo 
VMCv20170411 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vmcVarFrameSetInfo 
VMCv20171101 
Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vmcVarFrameSetInfo 
VMCv20180702 
Parameter, c0 from FerreiraLopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vmcVarFrameSetInfo 
VMCv20181120 
Parameter, c0 from FerreiraLopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratAst 
vvvVarFrameSetInfo 
VVVDR5 
Parameter, c0 from FerreiraLopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
ultravistaMapLcVarFrameSetInfo 
ULTRAVISTADR4 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
ultravistaVarFrameSetInfo 
ULTRAVISTADR4 
Parameter, c0 from FerreiraLopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
videoVarFrameSetInfo 
VIDEODR2 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
videoVarFrameSetInfo 
VIDEODR3 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
videoVarFrameSetInfo 
VIDEODR4 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
videoVarFrameSetInfo 
VIDEODR5 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
videoVarFrameSetInfo 
VIDEOv20100513 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
videoVarFrameSetInfo 
VIDEOv20111208 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vikingVarFrameSetInfo 
VIKINGDR2 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vikingVarFrameSetInfo 
VIKINGDR3 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vikingVarFrameSetInfo 
VIKINGDR4 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vikingVarFrameSetInfo 
VIKINGv20110714 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vikingVarFrameSetInfo 
VIKINGv20111019 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vikingVarFrameSetInfo 
VIKINGv20130417 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vikingVarFrameSetInfo 
VIKINGv20140402 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vikingVarFrameSetInfo 
VIKINGv20150421 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vikingVarFrameSetInfo 
VIKINGv20151230 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vikingVarFrameSetInfo 
VIKINGv20160406 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vikingVarFrameSetInfo 
VIKINGv20161202 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vikingVarFrameSetInfo 
VIKINGv20170715 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vmcVarFrameSetInfo 
VMCDR1 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vmcVarFrameSetInfo 
VMCDR2 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vmcVarFrameSetInfo 
VMCDR3 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vmcVarFrameSetInfo 
VMCDR4 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vmcVarFrameSetInfo 
VMCDR5 
Parameter, c0 from FerreiraLopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vmcVarFrameSetInfo 
VMCv20110816 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vmcVarFrameSetInfo 
VMCv20110909 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vmcVarFrameSetInfo 
VMCv20120126 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vmcVarFrameSetInfo 
VMCv20121128 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vmcVarFrameSetInfo 
VMCv20130304 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vmcVarFrameSetInfo 
VMCv20130805 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vmcVarFrameSetInfo 
VMCv20140428 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vmcVarFrameSetInfo 
VMCv20140903 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vmcVarFrameSetInfo 
VMCv20150309 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vmcVarFrameSetInfo 
VMCv20151218 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vmcVarFrameSetInfo 
VMCv20160311 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vmcVarFrameSetInfo 
VMCv20160822 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vmcVarFrameSetInfo 
VMCv20170109 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vmcVarFrameSetInfo 
VMCv20170411 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vmcVarFrameSetInfo 
VMCv20171101 
Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vmcVarFrameSetInfo 
VMCv20180702 
Parameter, c0 from FerreiraLopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vmcVarFrameSetInfo 
VMCv20181120 
Parameter, c0 from FerreiraLopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jaStratPht 
vvvVarFrameSetInfo 
VVVDR5 
Parameter, c0 from FerreiraLopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jAverageConf 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.NIR 
jAverageConf 
vhsSource 
VHSDR1 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

99999999 
meta.code 
jAverageConf 
vhsSource 
VHSDR2 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

99999999 
meta.code 
jAverageConf 
vhsSource 
VHSDR3 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.J 
jAverageConf 
vhsSource 
VHSDR4 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.J 
jAverageConf 
vhsSource 
VHSDR5 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.J 
jAverageConf 
vhsSource 
VHSDR6 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.J 
jAverageConf 
vhsSource 
VHSv20120926 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

99999999 
stat.likelihood;em.IR.NIR 
jAverageConf 
vhsSource 
VHSv20130417 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.NIR 
jAverageConf 
vhsSource 
VHSv20140409 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.J 
jAverageConf 
vhsSource 
VHSv20150108 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.J 
jAverageConf 
vhsSource 
VHSv20160114 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.J 
jAverageConf 
vhsSource 
VHSv20160507 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.J 
jAverageConf 
vhsSource 
VHSv20170630 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.J 
jAverageConf 
vhsSource 
VHSv20180419 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.J 
jAverageConf 
vikingSource 
VIKINGDR2 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

99999999 
meta.code 
jAverageConf 
vikingSource 
VIKINGDR3 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

99999999 
stat.likelihood;em.IR.NIR 
jAverageConf 
vikingSource 
VIKINGDR4 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.J 
jAverageConf 
vikingSource 
VIKINGv20110714 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

99999999 
meta.code 
jAverageConf 
vikingSource 
VIKINGv20111019 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

99999999 
meta.code 
jAverageConf 
vikingSource 
VIKINGv20130417 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.NIR 
jAverageConf 
vikingSource 
VIKINGv20140402 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.NIR 
jAverageConf 
vikingSource 
VIKINGv20150421 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.J 
jAverageConf 
vikingSource 
VIKINGv20151230 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.J 
jAverageConf 
vikingSource 
VIKINGv20160406 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.J 
jAverageConf 
vikingSource 
VIKINGv20161202 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.J 
jAverageConf 
vikingSource 
VIKINGv20170715 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.J 
jAverageConf 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.NIR 
jAverageConf 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.NIR 
jAverageConf 
vmcSource 
VMCDR2 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.NIR 
jAverageConf 
vmcSource 
VMCDR3 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.J 
jAverageConf 
vmcSource 
VMCDR4 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.J 
jAverageConf 
vmcSource 
VMCDR5 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.J 
jAverageConf 
vmcSource 
VMCv20110816 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

99999999 
meta.code 
jAverageConf 
vmcSource 
VMCv20110909 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

99999999 
meta.code 
jAverageConf 
vmcSource 
VMCv20120126 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

99999999 
meta.code 
jAverageConf 
vmcSource 
VMCv20121128 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

99999999 
stat.likelihood;em.IR.NIR 
jAverageConf 
vmcSource 
VMCv20130304 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.NIR 
jAverageConf 
vmcSource 
VMCv20130805 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.NIR 
jAverageConf 
vmcSource 
VMCv20140428 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.J 
jAverageConf 
vmcSource 
VMCv20140903 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.J 
jAverageConf 
vmcSource 
VMCv20150309 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.J 
jAverageConf 
vmcSource 
VMCv20151218 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.J 
jAverageConf 
vmcSource 
VMCv20160311 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.J 
jAverageConf 
vmcSource 
VMCv20160822 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.J 
jAverageConf 
vmcSource 
VMCv20170109 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.J 
jAverageConf 
vmcSource 
VMCv20170411 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.J 
jAverageConf 
vmcSource 
VMCv20171101 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.J 
jAverageConf 
vmcSource 
VMCv20180702 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.J 
jAverageConf 
vmcSource 
VMCv20181120 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.J 
jAverageConf 
vmcSource, vmcSynopticSource 
VMCDR1 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

99999999 
meta.code 
jAverageConf 
vvvSource 
VVVDR5 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.J 
jAverageConf 
vvvSource, vvvSynopticSource 
VVVDR4 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.J 
jbestAper 
ultravistaMapLcVariability 
ULTRAVISTADR4 
Best aperture (13) for photometric statistics in the J 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) 
jbestAper 
ultravistaVariability 
ULTRAVISTADR4 
Best aperture (16) for photometric statistics in the J band 
int 
4 

9999 
meta.code.class;em.IR.J 
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) 
jbestAper 
videoVariability 
VIDEODR2 
Best aperture (16) for photometric statistics in the J 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) 
jbestAper 
videoVariability 
VIDEODR3 
Best aperture (16) for photometric statistics in the J 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) 
jbestAper 
videoVariability 
VIDEODR4 
Best aperture (16) for photometric statistics in the J band 
int 
4 

9999 
meta.code.class;em.IR.J 
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) 
jbestAper 
videoVariability 
VIDEODR5 
Best aperture (16) for photometric statistics in the J band 
int 
4 

9999 
meta.code.class;em.IR.J 
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) 
jbestAper 
videoVariability 
VIDEOv20100513 
Best aperture (16) for photometric statistics in the J 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) 
jbestAper 
videoVariability 
VIDEOv20111208 
Best aperture (16) for photometric statistics in the J 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) 
jbestAper 
vikingVariability 
VIKINGDR2 
Best aperture (16) for photometric statistics in the J 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) 
jbestAper 
vikingVariability 
VIKINGDR3 
Best aperture (16) for photometric statistics in the J 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) 
jbestAper 
vikingVariability 
VIKINGDR4 
Best aperture (16) for photometric statistics in the J band 
int 
4 

9999 
meta.code.class;em.IR.J 
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) 
jbestAper 
vikingVariability 
VIKINGv20110714 
Best aperture (16) for photometric statistics in the J 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) 
jbestAper 
vikingVariability 
VIKINGv20111019 
Best aperture (16) for photometric statistics in the J 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) 
jbestAper 
vikingVariability 
VIKINGv20130417 
Best aperture (16) for photometric statistics in the J 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) 
jbestAper 
vikingVariability 
VIKINGv20140402 
Best aperture (16) for photometric statistics in the J 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) 
jbestAper 
vikingVariability 
VIKINGv20150421 
Best aperture (16) for photometric statistics in the J band 
int 
4 

9999 
meta.code.class;em.IR.J 
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) 
jbestAper 
vikingVariability 
VIKINGv20151230 
Best aperture (16) for photometric statistics in the J band 
int 
4 

9999 
meta.code.class;em.IR.J 
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) 
jbestAper 
vikingVariability 
VIKINGv20160406 
Best aperture (16) for photometric statistics in the J band 
int 
4 

9999 
meta.code.class;em.IR.J 
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) 
jbestAper 
vikingVariability 
VIKINGv20161202 
Best aperture (16) for photometric statistics in the J band 
int 
4 

9999 
meta.code.class;em.IR.J 
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) 
jbestAper 
vikingVariability 
VIKINGv20170715 
Best aperture (16) for photometric statistics in the J band 
int 
4 

9999 
meta.code.class;em.IR.J 
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) 
jbestAper 
vmcVariability 
VMCDR1 
Best aperture (16) for photometric statistics in the J 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) 
jbestAper 
vmcVariability 
VMCDR2 
Best aperture (16) for photometric statistics in the J 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) 
jbestAper 
vmcVariability 
VMCDR3 
Best aperture (16) for photometric statistics in the J band 
int 
4 

9999 
meta.code.class;em.IR.J 
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) 
jbestAper 
vmcVariability 
VMCDR4 
Best aperture (16) for photometric statistics in the J band 
int 
4 

9999 
meta.code.class;em.IR.J 
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) 
jbestAper 
vmcVariability 
VMCDR5 
Best aperture (16) for photometric statistics in the J band 
int 
4 

9999 
meta.code.class;em.IR.J 
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) 
jbestAper 
vmcVariability 
VMCv20110816 
Best aperture (16) for photometric statistics in the J 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) 
jbestAper 
vmcVariability 
VMCv20110909 
Best aperture (16) for photometric statistics in the J 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) 
jbestAper 
vmcVariability 
VMCv20120126 
Best aperture (16) for photometric statistics in the J 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) 
jbestAper 
vmcVariability 
VMCv20121128 
Best aperture (16) for photometric statistics in the J 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) 
jbestAper 
vmcVariability 
VMCv20130304 
Best aperture (16) for photometric statistics in the J 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) 
jbestAper 
vmcVariability 
VMCv20130805 
Best aperture (16) for photometric statistics in the J 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) 
jbestAper 
vmcVariability 
VMCv20140428 
Best aperture (16) for photometric statistics in the J band 
int 
4 

9999 
meta.code.class;em.IR.J 
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) 
jbestAper 
vmcVariability 
VMCv20140903 
Best aperture (16) for photometric statistics in the J band 
int 
4 

9999 
meta.code.class;em.IR.J 
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) 
jbestAper 
vmcVariability 
VMCv20150309 
Best aperture (16) for photometric statistics in the J band 
int 
4 

9999 
meta.code.class;em.IR.J 
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) 
jbestAper 
vmcVariability 
VMCv20151218 
Best aperture (16) for photometric statistics in the J band 
int 
4 

9999 
meta.code.class;em.IR.J 
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) 
jbestAper 
vmcVariability 
VMCv20160311 
Best aperture (16) for photometric statistics in the J band 
int 
4 

9999 
meta.code.class;em.IR.J 
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) 
jbestAper 
vmcVariability 
VMCv20160822 
Best aperture (16) for photometric statistics in the J band 
int 
4 

9999 
meta.code.class;em.IR.J 
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) 
jbestAper 
vmcVariability 
VMCv20170109 
Best aperture (16) for photometric statistics in the J band 
int 
4 

9999 
meta.code.class;em.IR.J 
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) 
jbestAper 
vmcVariability 
VMCv20170411 
Best aperture (16) for photometric statistics in the J band 
int 
4 

9999 
meta.code.class;em.IR.J 
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) 
jbestAper 
vmcVariability 
VMCv20171101 
Best aperture (16) for photometric statistics in the J band 
int 
4 

9999 
meta.code.class;em.IR.J 
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) 
jbestAper 
vmcVariability 
VMCv20180702 
Best aperture (16) for photometric statistics in the J band 
int 
4 

9999 
meta.code.class;em.IR.J 
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) 
jbestAper 
vmcVariability 
VMCv20181120 
Best aperture (16) for photometric statistics in the J band 
int 
4 

9999 
meta.code.class;em.IR.J 
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) 
jbestAper 
vvvVariability 
VVVDR5 
Best aperture (16) for photometric statistics in the J band 
int 
4 

9999 
meta.code.class;em.IR.J 
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) 
jbStratAst 
ultravistaVarFrameSetInfo 
ULTRAVISTADR4 
Parameter, c1 from FerreiraLopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
videoVarFrameSetInfo 
VIDEODR2 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
videoVarFrameSetInfo 
VIDEODR3 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
videoVarFrameSetInfo 
VIDEODR4 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
videoVarFrameSetInfo 
VIDEODR5 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
videoVarFrameSetInfo 
VIDEOv20100513 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
videoVarFrameSetInfo 
VIDEOv20111208 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vikingVarFrameSetInfo 
VIKINGDR2 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vikingVarFrameSetInfo 
VIKINGDR3 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vikingVarFrameSetInfo 
VIKINGDR4 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vikingVarFrameSetInfo 
VIKINGv20110714 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vikingVarFrameSetInfo 
VIKINGv20111019 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vikingVarFrameSetInfo 
VIKINGv20130417 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vikingVarFrameSetInfo 
VIKINGv20140402 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vikingVarFrameSetInfo 
VIKINGv20150421 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vikingVarFrameSetInfo 
VIKINGv20151230 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vikingVarFrameSetInfo 
VIKINGv20160406 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vikingVarFrameSetInfo 
VIKINGv20161202 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vikingVarFrameSetInfo 
VIKINGv20170715 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vmcVarFrameSetInfo 
VMCDR1 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vmcVarFrameSetInfo 
VMCDR2 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vmcVarFrameSetInfo 
VMCDR3 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vmcVarFrameSetInfo 
VMCDR4 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vmcVarFrameSetInfo 
VMCDR5 
Parameter, c1 from FerreiraLopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vmcVarFrameSetInfo 
VMCv20110816 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vmcVarFrameSetInfo 
VMCv20110909 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vmcVarFrameSetInfo 
VMCv20120126 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vmcVarFrameSetInfo 
VMCv20121128 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vmcVarFrameSetInfo 
VMCv20130304 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vmcVarFrameSetInfo 
VMCv20130805 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vmcVarFrameSetInfo 
VMCv20140428 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vmcVarFrameSetInfo 
VMCv20140903 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vmcVarFrameSetInfo 
VMCv20150309 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vmcVarFrameSetInfo 
VMCv20151218 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vmcVarFrameSetInfo 
VMCv20160311 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vmcVarFrameSetInfo 
VMCv20160822 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vmcVarFrameSetInfo 
VMCv20170109 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vmcVarFrameSetInfo 
VMCv20170411 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vmcVarFrameSetInfo 
VMCv20171101 
Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vmcVarFrameSetInfo 
VMCv20180702 
Parameter, c1 from FerreiraLopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vmcVarFrameSetInfo 
VMCv20181120 
Parameter, c1 from FerreiraLopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratAst 
vvvVarFrameSetInfo 
VVVDR5 
Parameter, c1 from FerreiraLopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
ultravistaMapLcVarFrameSetInfo 
ULTRAVISTADR4 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
ultravistaVarFrameSetInfo 
ULTRAVISTADR4 
Parameter, c1 from FerreiraLopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
videoVarFrameSetInfo 
VIDEODR2 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
videoVarFrameSetInfo 
VIDEODR3 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
videoVarFrameSetInfo 
VIDEODR4 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
videoVarFrameSetInfo 
VIDEODR5 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
videoVarFrameSetInfo 
VIDEOv20100513 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
videoVarFrameSetInfo 
VIDEOv20111208 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vikingVarFrameSetInfo 
VIKINGDR2 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vikingVarFrameSetInfo 
VIKINGDR3 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vikingVarFrameSetInfo 
VIKINGDR4 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vikingVarFrameSetInfo 
VIKINGv20110714 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vikingVarFrameSetInfo 
VIKINGv20111019 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vikingVarFrameSetInfo 
VIKINGv20130417 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vikingVarFrameSetInfo 
VIKINGv20140402 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vikingVarFrameSetInfo 
VIKINGv20150421 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vikingVarFrameSetInfo 
VIKINGv20151230 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vikingVarFrameSetInfo 
VIKINGv20160406 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vikingVarFrameSetInfo 
VIKINGv20161202 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vikingVarFrameSetInfo 
VIKINGv20170715 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vmcVarFrameSetInfo 
VMCDR1 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vmcVarFrameSetInfo 
VMCDR2 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vmcVarFrameSetInfo 
VMCDR3 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vmcVarFrameSetInfo 
VMCDR4 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vmcVarFrameSetInfo 
VMCDR5 
Parameter, c1 from FerreiraLopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vmcVarFrameSetInfo 
VMCv20110816 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vmcVarFrameSetInfo 
VMCv20110909 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vmcVarFrameSetInfo 
VMCv20120126 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vmcVarFrameSetInfo 
VMCv20121128 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vmcVarFrameSetInfo 
VMCv20130304 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vmcVarFrameSetInfo 
VMCv20130805 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vmcVarFrameSetInfo 
VMCv20140428 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vmcVarFrameSetInfo 
VMCv20140903 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vmcVarFrameSetInfo 
VMCv20150309 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vmcVarFrameSetInfo 
VMCv20151218 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vmcVarFrameSetInfo 
VMCv20160311 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vmcVarFrameSetInfo 
VMCv20160822 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vmcVarFrameSetInfo 
VMCv20170109 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vmcVarFrameSetInfo 
VMCv20170411 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vmcVarFrameSetInfo 
VMCv20171101 
Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vmcVarFrameSetInfo 
VMCv20180702 
Parameter, c1 from FerreiraLopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vmcVarFrameSetInfo 
VMCv20181120 
Parameter, c1 from FerreiraLopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jbStratPht 
vvvVarFrameSetInfo 
VVVDR5 
Parameter, c1 from FerreiraLopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
ultravistaVarFrameSetInfo 
ULTRAVISTADR4 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
videoVarFrameSetInfo 
VIDEODR2 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
videoVarFrameSetInfo 
VIDEODR3 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
videoVarFrameSetInfo 
VIDEODR4 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
videoVarFrameSetInfo 
VIDEODR5 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
videoVarFrameSetInfo 
VIDEOv20100513 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
videoVarFrameSetInfo 
VIDEOv20111208 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vikingVarFrameSetInfo 
VIKINGDR2 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vikingVarFrameSetInfo 
VIKINGDR3 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vikingVarFrameSetInfo 
VIKINGDR4 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vikingVarFrameSetInfo 
VIKINGv20110714 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vikingVarFrameSetInfo 
VIKINGv20111019 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vikingVarFrameSetInfo 
VIKINGv20130417 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vikingVarFrameSetInfo 
VIKINGv20140402 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vikingVarFrameSetInfo 
VIKINGv20150421 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vikingVarFrameSetInfo 
VIKINGv20151230 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vikingVarFrameSetInfo 
VIKINGv20160406 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vikingVarFrameSetInfo 
VIKINGv20161202 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vikingVarFrameSetInfo 
VIKINGv20170715 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vmcVarFrameSetInfo 
VMCDR1 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vmcVarFrameSetInfo 
VMCDR2 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vmcVarFrameSetInfo 
VMCDR3 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vmcVarFrameSetInfo 
VMCDR4 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vmcVarFrameSetInfo 
VMCDR5 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vmcVarFrameSetInfo 
VMCv20110816 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vmcVarFrameSetInfo 
VMCv20110909 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vmcVarFrameSetInfo 
VMCv20120126 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vmcVarFrameSetInfo 
VMCv20121128 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vmcVarFrameSetInfo 
VMCv20130304 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vmcVarFrameSetInfo 
VMCv20130805 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vmcVarFrameSetInfo 
VMCv20140428 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vmcVarFrameSetInfo 
VMCv20140903 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vmcVarFrameSetInfo 
VMCv20150309 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vmcVarFrameSetInfo 
VMCv20151218 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vmcVarFrameSetInfo 
VMCv20160311 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vmcVarFrameSetInfo 
VMCv20160822 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vmcVarFrameSetInfo 
VMCv20170109 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vmcVarFrameSetInfo 
VMCv20170411 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vmcVarFrameSetInfo 
VMCv20171101 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vmcVarFrameSetInfo 
VMCv20180702 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vmcVarFrameSetInfo 
VMCv20181120 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqAst 
vvvVarFrameSetInfo 
VVVDR5 
Goodness of fit of Strateva function to astrometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqpd 
ultravistaMapLcVariability 
ULTRAVISTADR4 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
ultravistaVariability 
ULTRAVISTADR4 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2;em.IR.J 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
videoVariability 
VIDEODR2 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
videoVariability 
VIDEODR3 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
videoVariability 
VIDEODR4 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2;em.IR.J 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
videoVariability 
VIDEODR5 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2;em.IR.J 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
videoVariability 
VIDEOv20100513 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
videoVariability 
VIDEOv20111208 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vikingVariability 
VIKINGDR2 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vikingVariability 
VIKINGDR3 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vikingVariability 
VIKINGDR4 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2;em.IR.J 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vikingVariability 
VIKINGv20110714 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vikingVariability 
VIKINGv20111019 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vikingVariability 
VIKINGv20130417 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vikingVariability 
VIKINGv20140402 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vikingVariability 
VIKINGv20150421 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2;em.IR.J 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vikingVariability 
VIKINGv20151230 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2;em.IR.J 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vikingVariability 
VIKINGv20160406 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2;em.IR.J 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vikingVariability 
VIKINGv20161202 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2;em.IR.J 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vikingVariability 
VIKINGv20170715 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2;em.IR.J 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vmcVariability 
VMCDR1 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vmcVariability 
VMCDR2 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vmcVariability 
VMCDR3 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2;em.IR.J 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vmcVariability 
VMCDR4 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2;em.IR.J 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vmcVariability 
VMCDR5 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2;em.IR.J 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vmcVariability 
VMCv20110816 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vmcVariability 
VMCv20110909 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vmcVariability 
VMCv20120126 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vmcVariability 
VMCv20121128 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vmcVariability 
VMCv20130304 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vmcVariability 
VMCv20130805 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vmcVariability 
VMCv20140428 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2;em.IR.J 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vmcVariability 
VMCv20140903 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2;em.IR.J 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vmcVariability 
VMCv20150309 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2;em.IR.J 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vmcVariability 
VMCv20151218 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2;em.IR.J 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vmcVariability 
VMCv20160311 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2;em.IR.J 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vmcVariability 
VMCv20160822 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2;em.IR.J 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vmcVariability 
VMCv20170109 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2;em.IR.J 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vmcVariability 
VMCv20170411 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2;em.IR.J 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vmcVariability 
VMCv20171101 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2;em.IR.J 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vmcVariability 
VMCv20180702 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2;em.IR.J 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vmcVariability 
VMCv20181120 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2;em.IR.J 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqpd 
vvvVariability 
VVVDR5 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2;em.IR.J 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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. 
jchiSqPht 
ultravistaMapLcVarFrameSetInfo, ultravistaVarFrameSetInfo 
ULTRAVISTADR4 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
videoVarFrameSetInfo 
VIDEODR2 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
videoVarFrameSetInfo 
VIDEODR3 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
videoVarFrameSetInfo 
VIDEODR4 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
videoVarFrameSetInfo 
VIDEODR5 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
videoVarFrameSetInfo 
VIDEOv20100513 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
videoVarFrameSetInfo 
VIDEOv20111208 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vikingVarFrameSetInfo 
VIKINGDR2 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vikingVarFrameSetInfo 
VIKINGDR3 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vikingVarFrameSetInfo 
VIKINGDR4 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vikingVarFrameSetInfo 
VIKINGv20110714 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vikingVarFrameSetInfo 
VIKINGv20111019 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vikingVarFrameSetInfo 
VIKINGv20130417 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vikingVarFrameSetInfo 
VIKINGv20140402 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vikingVarFrameSetInfo 
VIKINGv20150421 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vikingVarFrameSetInfo 
VIKINGv20151230 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vikingVarFrameSetInfo 
VIKINGv20160406 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vikingVarFrameSetInfo 
VIKINGv20161202 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vikingVarFrameSetInfo 
VIKINGv20170715 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vmcVarFrameSetInfo 
VMCDR1 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vmcVarFrameSetInfo 
VMCDR2 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vmcVarFrameSetInfo 
VMCDR3 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vmcVarFrameSetInfo 
VMCDR4 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vmcVarFrameSetInfo 
VMCDR5 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vmcVarFrameSetInfo 
VMCv20110816 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vmcVarFrameSetInfo 
VMCv20110909 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vmcVarFrameSetInfo 
VMCv20120126 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vmcVarFrameSetInfo 
VMCv20121128 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vmcVarFrameSetInfo 
VMCv20130304 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vmcVarFrameSetInfo 
VMCv20130805 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vmcVarFrameSetInfo 
VMCv20140428 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vmcVarFrameSetInfo 
VMCv20140903 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vmcVarFrameSetInfo 
VMCv20150309 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vmcVarFrameSetInfo 
VMCv20151218 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vmcVarFrameSetInfo 
VMCv20160311 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vmcVarFrameSetInfo 
VMCv20160822 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vmcVarFrameSetInfo 
VMCv20170109 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vmcVarFrameSetInfo 
VMCv20170411 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vmcVarFrameSetInfo 
VMCv20171101 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vmcVarFrameSetInfo 
VMCv20180702 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vmcVarFrameSetInfo 
VMCv20181120 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jchiSqPht 
vvvVarFrameSetInfo 
VVVDR5 
Goodness of fit of Strateva function to photometric data in J band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
Jclass 
vvvParallaxCatalogue 
VVVDR5 
VVV DR4 J morphological classification. 1 = galaxy,0 = noise,1 = stellar,2 = probably stellar,3 = probable galaxy,7 = bad pixel within 2" aperture,9 = saturated {catalogue TType keyword: Jclass} 
int 
4 

99999999 

Jclass 
vvvParallaxCatalogue, vvvProperMotionCatalogue 
VVVDR4 
VVV DR4 J morphological classification. 1 = galaxy,0 = noise,1 = stellar,2 = probably stellar,3 = probable galaxy,7 = bad pixel within 2" aperture,9 = saturated {catalogue TType keyword: Jclass} 
int 
4 

99999999 

jClass 
ultravistaSource 
ULTRAVISTADR4 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClass 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
discrete image classification flag in J 
smallint 
2 

9999 
src.class 
jClass 
vhsSource 
VHSDR2 
discrete image classification flag in J 
smallint 
2 

9999 
src.class 
jClass 
vhsSource 
VHSDR3 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClass 
vhsSource 
VHSDR4 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClass 
vhsSource 
VHSDR5 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClass 
vhsSource 
VHSDR6 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClass 
vhsSource 
VHSv20120926 
discrete image classification flag in J 
smallint 
2 

9999 
src.class 
jClass 
vhsSource 
VHSv20130417 
discrete image classification flag in J 
smallint 
2 

9999 
src.class 
jClass 
vhsSource 
VHSv20140409 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClass 
vhsSource 
VHSv20150108 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClass 
vhsSource 
VHSv20160114 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClass 
vhsSource 
VHSv20160507 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClass 
vhsSource 
VHSv20170630 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClass 
vhsSource 
VHSv20180419 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClass 
vhsSource, vhsSourceRemeasurement 
VHSDR1 
discrete image classification flag in J 
smallint 
2 

9999 
src.class 
jClass 
videoSource 
VIDEODR2 
discrete image classification flag in J 
smallint 
2 

9999 
src.class 
jClass 
videoSource 
VIDEODR3 
discrete image classification flag in J 
smallint 
2 

9999 
src.class 
jClass 
videoSource 
VIDEODR4 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClass 
videoSource 
VIDEODR5 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClass 
videoSource 
VIDEOv20111208 
discrete image classification flag in J 
smallint 
2 

9999 
src.class 
jClass 
videoSource, videoSourceRemeasurement 
VIDEOv20100513 
discrete image classification flag in J 
smallint 
2 

9999 
src.class 
jClass 
vikingSource 
VIKINGDR2 
discrete image classification flag in J 
smallint 
2 

9999 
src.class 
jClass 
vikingSource 
VIKINGDR3 
discrete image classification flag in J 
smallint 
2 

9999 
src.class 
jClass 
vikingSource 
VIKINGDR4 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClass 
vikingSource 
VIKINGv20111019 
discrete image classification flag in J 
smallint 
2 

9999 
src.class 
jClass 
vikingSource 
VIKINGv20130417 
discrete image classification flag in J 
smallint 
2 

9999 
src.class 
jClass 
vikingSource 
VIKINGv20140402 
discrete image classification flag in J 
smallint 
2 

9999 
src.class 
jClass 
vikingSource 
VIKINGv20150421 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClass 
vikingSource 
VIKINGv20151230 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClass 
vikingSource 
VIKINGv20160406 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClass 
vikingSource 
VIKINGv20161202 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClass 
vikingSource 
VIKINGv20170715 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClass 
vikingSource, vikingSourceRemeasurement 
VIKINGv20110714 
discrete image classification flag in J 
smallint 
2 

9999 
src.class 
jClass 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
discrete image classification flag in J 
smallint 
2 

9999 
src.class 
jClass 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
discrete image classification flag in J 
smallint 
2 

9999 
src.class 
jClass 
vmcSource 
VMCDR2 
discrete image classification flag in J 
smallint 
2 

9999 
src.class 
jClass 
vmcSource 
VMCDR3 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClass 
vmcSource 
VMCDR4 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClass 
vmcSource 
VMCDR5 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClass 
vmcSource 
VMCv20110909 
discrete image classification flag in J 
smallint 
2 

9999 
src.class 
jClass 
vmcSource 
VMCv20120126 
discrete image classification flag in J 
smallint 
2 

9999 
src.class 
jClass 
vmcSource 
VMCv20121128 
discrete image classification flag in J 
smallint 
2 

9999 
src.class 
jClass 
vmcSource 
VMCv20130304 
discrete image classification flag in J 
smallint 
2 

9999 
src.class 
jClass 
vmcSource 
VMCv20130805 
discrete image classification flag in J 
smallint 
2 

9999 
src.class 
jClass 
vmcSource 
VMCv20140428 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClass 
vmcSource 
VMCv20140903 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClass 
vmcSource 
VMCv20150309 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClass 
vmcSource 
VMCv20151218 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClass 
vmcSource 
VMCv20160311 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClass 
vmcSource 
VMCv20160822 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClass 
vmcSource 
VMCv20170109 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClass 
vmcSource 
VMCv20170411 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClass 
vmcSource 
VMCv20171101 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClass 
vmcSource 
VMCv20180702 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClass 
vmcSource 
VMCv20181120 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClass 
vmcSource, vmcSourceRemeasurement 
VMCv20110816 
discrete image classification flag in J 
smallint 
2 

9999 
src.class 
jClass 
vmcSource, vmcSynopticSource 
VMCDR1 
discrete image classification flag in J 
smallint 
2 

9999 
src.class 
jClass 
vvvSource 
VVVDR5 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClass 
vvvSource, vvvSynopticSource 
VVVDR4 
discrete image classification flag in J 
smallint 
2 

9999 
src.class;em.IR.J 
jClassStat 
ultravistaSource 
ULTRAVISTADR4 
SExtractor classification statistic in J 
real 
4 

0.9999995e9 
stat;em.IR.J 
jClassStat 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat 
jClassStat 
vhsSource 
VHSDR2 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat 
jClassStat 
vhsSource 
VHSDR3 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat;em.IR.J 
jClassStat 
vhsSource 
VHSDR4 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat;em.IR.J 
jClassStat 
vhsSource 
VHSDR5 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat;em.IR.J 
jClassStat 
vhsSource 
VHSDR6 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat;em.IR.J 
jClassStat 
vhsSource 
VHSv20120926 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat 
jClassStat 
vhsSource 
VHSv20130417 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat 
jClassStat 
vhsSource 
VHSv20140409 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat;em.IR.J 
jClassStat 
vhsSource 
VHSv20150108 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat;em.IR.J 
jClassStat 
vhsSource 
VHSv20160114 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat;em.IR.J 
jClassStat 
vhsSource 
VHSv20160507 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat;em.IR.J 
jClassStat 
vhsSource 
VHSv20170630 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat;em.IR.J 
jClassStat 
vhsSource 
VHSv20180419 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat;em.IR.J 
jClassStat 
vhsSource, vhsSourceRemeasurement 
VHSDR1 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat 
jClassStat 
videoSource 
VIDEODR2 
SExtractor classification statistic in J 
real 
4 

0.9999995e9 
stat 
jClassStat 
videoSource 
VIDEODR3 
SExtractor classification statistic in J 
real 
4 

0.9999995e9 
stat 
jClassStat 
videoSource 
VIDEODR4 
SExtractor classification statistic in J 
real 
4 

0.9999995e9 
stat;em.IR.J 
jClassStat 
videoSource 
VIDEODR5 
SExtractor classification statistic in J 
real 
4 

0.9999995e9 
stat;em.IR.J 
jClassStat 
videoSource 
VIDEOv20100513 
SExtractor classification statistic in J 
real 
4 

0.9999995e9 
stat 
jClassStat 
videoSource 
VIDEOv20111208 
SExtractor classification statistic in J 
real 
4 

0.9999995e9 
stat 
jClassStat 
videoSourceRemeasurement 
VIDEOv20100513 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

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

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

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

0.9999995e9 
stat;em.IR.J 
jClassStat 
vikingSource 
VIKINGv20111019 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

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

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

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

0.9999995e9 
stat;em.IR.J 
jClassStat 
vikingSource 
VIKINGv20151230 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat;em.IR.J 
jClassStat 
vikingSource 
VIKINGv20160406 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat;em.IR.J 
jClassStat 
vikingSource 
VIKINGv20161202 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat;em.IR.J 
jClassStat 
vikingSource 
VIKINGv20170715 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat;em.IR.J 
jClassStat 
vikingSource, vikingSourceRemeasurement 
VIKINGv20110714 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

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

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

0.9999995e9 
stat 
jClassStat 
vmcSource 
VMCDR2 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat 
jClassStat 
vmcSource 
VMCDR3 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat;em.IR.J 
jClassStat 
vmcSource 
VMCDR4 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat;em.IR.J 
jClassStat 
vmcSource 
VMCDR5 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat;em.IR.J 
jClassStat 
vmcSource 
VMCv20110909 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat 
jClassStat 
vmcSource 
VMCv20120126 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat 
jClassStat 
vmcSource 
VMCv20121128 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat 
jClassStat 
vmcSource 
VMCv20130304 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat 
jClassStat 
vmcSource 
VMCv20130805 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat 
jClassStat 
vmcSource 
VMCv20140428 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat;em.IR.J 
jClassStat 
vmcSource 
VMCv20140903 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat;em.IR.J 
jClassStat 
vmcSource 
VMCv20150309 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat;em.IR.J 
jClassStat 
vmcSource 
VMCv20151218 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat;em.IR.J 
jClassStat 
vmcSource 
VMCv20160311 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat;em.IR.J 
jClassStat 
vmcSource 
VMCv20160822 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat;em.IR.J 
jClassStat 
vmcSource 
VMCv20170109 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat;em.IR.J 
jClassStat 
vmcSource 
VMCv20170411 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat;em.IR.J 
jClassStat 
vmcSource 
VMCv20171101 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat;em.IR.J 
jClassStat 
vmcSource 
VMCv20180702 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat;em.IR.J 
jClassStat 
vmcSource 
VMCv20181120 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat;em.IR.J 
jClassStat 
vmcSource, vmcSourceRemeasurement 
VMCv20110816 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat 
jClassStat 
vmcSource, vmcSynopticSource 
VMCDR1 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat 
jClassStat 
vvvSource 
VVVDR4 
SExtractor classification statistic in J 
real 
4 

0.9999995e9 
stat;em.IR.J 
jClassStat 
vvvSource 
VVVDR5 
SExtractor classification statistic in J 
real 
4 

0.9999995e9 
stat;em.IR.J 
jClassStat 
vvvSynopticSource 
VVVDR4 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat;em.IR.J 
jCorr 
twompzPhotoz 
TWOMPZ 
J 20mag/sq." isophotal fiducial ell. ap. magnitude with Galactic dust correction {image primary HDU keyword: Jcorr} 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.J 
jCorrErr 
twompzPhotoz 
TWOMPZ 
J 1sigma uncertainty in 20mag/sq." aperture {image primary HDU keyword: j_msig_k20fe} 
real 
4 
mag 
0.9999995e9 

jcStratAst 
ultravistaVarFrameSetInfo 
ULTRAVISTADR4 
Parameter, c2 from FerreiraLopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
videoVarFrameSetInfo 
VIDEODR2 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
videoVarFrameSetInfo 
VIDEODR3 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
videoVarFrameSetInfo 
VIDEODR4 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
videoVarFrameSetInfo 
VIDEODR5 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
videoVarFrameSetInfo 
VIDEOv20100513 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
videoVarFrameSetInfo 
VIDEOv20111208 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vikingVarFrameSetInfo 
VIKINGDR2 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vikingVarFrameSetInfo 
VIKINGDR3 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vikingVarFrameSetInfo 
VIKINGDR4 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vikingVarFrameSetInfo 
VIKINGv20110714 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vikingVarFrameSetInfo 
VIKINGv20111019 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vikingVarFrameSetInfo 
VIKINGv20130417 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vikingVarFrameSetInfo 
VIKINGv20140402 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vikingVarFrameSetInfo 
VIKINGv20150421 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vikingVarFrameSetInfo 
VIKINGv20151230 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vikingVarFrameSetInfo 
VIKINGv20160406 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vikingVarFrameSetInfo 
VIKINGv20161202 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vikingVarFrameSetInfo 
VIKINGv20170715 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vmcVarFrameSetInfo 
VMCDR1 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vmcVarFrameSetInfo 
VMCDR2 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vmcVarFrameSetInfo 
VMCDR3 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vmcVarFrameSetInfo 
VMCDR4 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vmcVarFrameSetInfo 
VMCDR5 
Parameter, c2 from FerreiraLopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vmcVarFrameSetInfo 
VMCv20110816 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vmcVarFrameSetInfo 
VMCv20110909 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vmcVarFrameSetInfo 
VMCv20120126 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vmcVarFrameSetInfo 
VMCv20121128 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vmcVarFrameSetInfo 
VMCv20130304 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vmcVarFrameSetInfo 
VMCv20130805 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vmcVarFrameSetInfo 
VMCv20140428 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vmcVarFrameSetInfo 
VMCv20140903 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vmcVarFrameSetInfo 
VMCv20150309 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vmcVarFrameSetInfo 
VMCv20151218 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vmcVarFrameSetInfo 
VMCv20160311 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vmcVarFrameSetInfo 
VMCv20160822 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vmcVarFrameSetInfo 
VMCv20170109 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vmcVarFrameSetInfo 
VMCv20170411 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vmcVarFrameSetInfo 
VMCv20171101 
Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vmcVarFrameSetInfo 
VMCv20180702 
Parameter, c2 from FerreiraLopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vmcVarFrameSetInfo 
VMCv20181120 
Parameter, c2 from FerreiraLopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratAst 
vvvVarFrameSetInfo 
VVVDR5 
Parameter, c2 from FerreiraLopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
ultravistaMapLcVarFrameSetInfo 
ULTRAVISTADR4 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
ultravistaVarFrameSetInfo 
ULTRAVISTADR4 
Parameter, c2 from FerreiraLopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
videoVarFrameSetInfo 
VIDEODR2 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
videoVarFrameSetInfo 
VIDEODR3 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
videoVarFrameSetInfo 
VIDEODR4 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
videoVarFrameSetInfo 
VIDEODR5 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
videoVarFrameSetInfo 
VIDEOv20100513 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
videoVarFrameSetInfo 
VIDEOv20111208 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vikingVarFrameSetInfo 
VIKINGDR2 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vikingVarFrameSetInfo 
VIKINGDR3 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vikingVarFrameSetInfo 
VIKINGDR4 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vikingVarFrameSetInfo 
VIKINGv20110714 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vikingVarFrameSetInfo 
VIKINGv20111019 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vikingVarFrameSetInfo 
VIKINGv20130417 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vikingVarFrameSetInfo 
VIKINGv20140402 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vikingVarFrameSetInfo 
VIKINGv20150421 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vikingVarFrameSetInfo 
VIKINGv20151230 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vikingVarFrameSetInfo 
VIKINGv20160406 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vikingVarFrameSetInfo 
VIKINGv20161202 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vikingVarFrameSetInfo 
VIKINGv20170715 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vmcVarFrameSetInfo 
VMCDR1 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vmcVarFrameSetInfo 
VMCDR2 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vmcVarFrameSetInfo 
VMCDR3 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vmcVarFrameSetInfo 
VMCDR4 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vmcVarFrameSetInfo 
VMCDR5 
Parameter, c2 from FerreiraLopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vmcVarFrameSetInfo 
VMCv20110816 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vmcVarFrameSetInfo 
VMCv20110909 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vmcVarFrameSetInfo 
VMCv20120126 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vmcVarFrameSetInfo 
VMCv20121128 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vmcVarFrameSetInfo 
VMCv20130304 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vmcVarFrameSetInfo 
VMCv20130805 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vmcVarFrameSetInfo 
VMCv20140428 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vmcVarFrameSetInfo 
VMCv20140903 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vmcVarFrameSetInfo 
VMCv20150309 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vmcVarFrameSetInfo 
VMCv20151218 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vmcVarFrameSetInfo 
VMCv20160311 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vmcVarFrameSetInfo 
VMCv20160822 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vmcVarFrameSetInfo 
VMCv20170109 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vmcVarFrameSetInfo 
VMCv20170411 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vmcVarFrameSetInfo 
VMCv20171101 
Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vmcVarFrameSetInfo 
VMCv20180702 
Parameter, c2 from FerreiraLopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vmcVarFrameSetInfo 
VMCv20181120 
Parameter, c2 from FerreiraLopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jcStratPht 
vvvVarFrameSetInfo 
VVVDR5 
Parameter, c2 from FerreiraLopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.J 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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. 
jdate 
twomass_psc 
TWOMASS 
The Julian Date of the source measurement accurate to +30 seconds. 
float 
8 
Julian days 

time.epoch 
jdate 
twomass_scn 
TWOMASS 
Julian Date at beginning of scan. 
float 
8 
Julian days 

time.epoch 
jdate 
twomass_sixx2_psc 
TWOMASS 
julian date of source measurement to +/ 30 sec 
float 
8 
jdate 


jdate 
twomass_sixx2_scn 
TWOMASS 
Julian date beginning UT of scan data 
float 
8 
jdate 


jdate 
twomass_xsc 
TWOMASS 
Julian date of the source measurement accurate to +3 minutes. 
float 
8 
Julian days 

time.epoch 
jDeblend 
vhsSourceRemeasurement 
VHSDR1 
placeholder flag indicating parent/child relation in J 
int 
4 

99999999 
meta.code 
jDeblend 
videoSource, videoSourceRemeasurement 
VIDEOv20100513 
placeholder flag indicating parent/child relation in J 
int 
4 

99999999 
meta.code 
jDeblend 
vikingSourceRemeasurement 
VIKINGv20110714 
placeholder flag indicating parent/child relation in J 
int 
4 

99999999 
meta.code 
jDeblend 
vikingSourceRemeasurement 
VIKINGv20111019 
placeholder flag indicating parent/child relation in J 
int 
4 

99999999 
meta.code 
jDeblend 
vmcSourceRemeasurement 
VMCv20110816 
placeholder flag indicating parent/child relation in J 
int 
4 

99999999 
meta.code 
jDeblend 
vmcSourceRemeasurement 
VMCv20110909 
placeholder flag indicating parent/child relation in J 
int 
4 

99999999 
meta.code 
Jell 
vvvParallaxCatalogue 
VVVDR5 
Ellipticity of the DR4 J detection. {catalogue TType keyword: Jell} 
real 
4 

999999500.0 

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

999999500.0 

jEll 
ultravistaSource 
ULTRAVISTADR4 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.J 
jEll 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticty 
jEll 
vhsSource 
VHSDR2 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity 
jEll 
vhsSource 
VHSDR3 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.J 
jEll 
vhsSource 
VHSDR4 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.J 
jEll 
vhsSource 
VHSDR5 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.J 
jEll 
vhsSource 
VHSDR6 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.J 
jEll 
vhsSource 
VHSv20120926 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity 
jEll 
vhsSource 
VHSv20130417 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity 
jEll 
vhsSource 
VHSv20140409 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.J 
jEll 
vhsSource 
VHSv20150108 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.J 
jEll 
vhsSource 
VHSv20160114 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.J 
jEll 
vhsSource 
VHSv20160507 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.J 
jEll 
vhsSource 
VHSv20170630 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.J 
jEll 
vhsSource 
VHSv20180419 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.J 
jEll 
vhsSource, vhsSourceRemeasurement 
VHSDR1 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity 
jEll 
videoSource 
VIDEODR2 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

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

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

0.9999995e9 
src.ellipticity;em.IR.J 
jEll 
videoSource 
VIDEODR5 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.J 
jEll 
videoSource 
VIDEOv20111208 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity 
jEll 
videoSource, videoSourceRemeasurement 
VIDEOv20100513 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

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

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

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

0.9999995e9 
src.ellipticity;em.IR.J 
jEll 
vikingSource 
VIKINGv20111019 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

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

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

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

0.9999995e9 
src.ellipticity;em.IR.J 
jEll 
vikingSource 
VIKINGv20151230 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.J 
jEll 
vikingSource 
VIKINGv20160406 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.J 
jEll 
vikingSource 
VIKINGv20161202 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.J 
jEll 
vikingSource 
VIKINGv20170715 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.J 
jEll 
vikingSource, vikingSourceRemeasurement 
VIKINGv20110714 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

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

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

0.9999995e9 
src.ellipticity 
jEll 
vmcSource 
VMCDR2 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity 
jEll 
vmcSource 
VMCDR3 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.J 
jEll 
vmcSource 
VMCDR4 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.J 
jEll 
vmcSource 
VMCDR5 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.J 
jEll 
vmcSource 
VMCv20110909 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity 
jEll 
vmcSource 
VMCv20120126 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity 
jEll 
vmcSource 
VMCv20121128 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity 
jEll 
vmcSource 
VMCv20130304 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity 
jEll 
vmcSource 
VMCv20130805 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity 
jEll 
vmcSource 
VMCv20140428 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.J 
jEll 
vmcSource 
VMCv20140903 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.J 
jEll 
vmcSource 
VMCv20150309 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.J 
jEll 
vmcSource 
VMCv20151218 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.J 
jEll 
vmcSource 
VMCv20160311 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.J 
jEll 
vmcSource 
VMCv20160822 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.J 
jEll 
vmcSource 
VMCv20170109 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.J 
jEll 
vmcSource 
VMCv20170411 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.J 
jEll 
vmcSource 
VMCv20171101 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.J 
jEll 
vmcSource 
VMCv20180702 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.J 
jEll 
vmcSource 
VMCv20181120 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.J 
jEll 
vmcSource, vmcSourceRemeasurement 
VMCv20110816 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity 
jEll 
vmcSource, vmcSynopticSource 
VMCDR1 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity 
jEll 
vvvSource 
VVVDR5 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.J 
jEll 
vvvSource, vvvSynopticSource 
VVVDR4 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.J 
jeNum 
ultravistaMergeLog, ultravistaRemeasMergeLog 
ULTRAVISTADR4 
the extension number of this J frame 
tinyint 
1 


meta.number;em.IR.J 
jeNum 
vhsMergeLog 
VHSDR1 
the extension number of this J frame 
tinyint 
1 


meta.number 
jeNum 
vhsMergeLog 
VHSDR2 
the extension number of this J frame 
tinyint 
1 


meta.number 
jeNum 
vhsMergeLog 
VHSDR3 
the extension number of this J frame 
tinyint 
1 