Z 
Name  Schema Table  Database  Description  Type  Length  Unit  Default Value  Unified Content Descriptor 
Z 
spectra 
SIXDF 
raw measured redshift 
real 
4 



z 
allwise_sc 
WISE 
Unit sphere position z value 
float 
8 



Z_ABS 
spectra 
SIXDF 
crosscorrelation redshift 
real 
4 



Z_COMM 
spectra 
SIXDF 
observer's comment 
varchar 
29 



Z_EMI 
spectra 
SIXDF 
emission redshift 
real 
4 



Z_HELIO 
spectra 
SIXDF 
heliocentric redshift 
real 
4 



Z_ORIGIN 
spectra 
SIXDF 
redshift from C=combined V or R frame 
char 
1 



ZABSBESTERR 
spectra 
SIXDF 
error on the selected absorption line redshift, 0.0 if not measured 
real 
4 



zAperMag1 
vvvSource 
VVVDR1 
Extended source Z aperture corrected mag (0.7 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag1 
vvvSource 
VVVv20100531 
Extended source Z aperture corrected mag (0.7 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag1 
vvvSource 
VVVv20110718 
Extended source Z aperture corrected mag (0.7 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag1 
vvvSource, vvvSynopticSource 
VVVDR2 
Extended source Z aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zAperMag1Err 
vvvSource 
VVVDR1 
Error in extended source Z mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag1Err 
vvvSource 
VVVv20100531 
Error in extended source Z mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag1Err 
vvvSource 
VVVv20110718 
Error in extended source Z mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag1Err 
vvvSource, vvvSynopticSource 
VVVDR2 
Error in extended source Z mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag2 
vvvSynopticSource 
VVVDR1 
Extended source Z aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag2 
vvvSynopticSource 
VVVDR2 
Extended source Z aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zAperMag2Err 
vvvSynopticSource 
VVVDR1 
Error in extended source Z mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag2Err 
vvvSynopticSource 
VVVDR2 
Error in extended source Z mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag3 
svNgc253Source 
SVNGC253v20100429 
Default point/extended source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag3 
svOrionSource 
SVORIONv20100429 
Default point/extended source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag3 
ultravistaSource 
ULTRAVISTAv20100429 
Default point/extended source Z mag, no aperture correction applied If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag3 
videoSource 
VIDEODR2 
Default point source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag3 
videoSource 
VIDEODR3 
Default point source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag3 
videoSource 
VIDEODR4 
Default point source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zAperMag3 
videoSource 
VIDEOv20100513 
Default point/extended source Z mag, no aperture correction applied If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag3 
videoSource 
VIDEOv20111208 
Default point source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag3 
vikingSource 
VIKINGDR2 
Default point source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag3 
vikingSource 
VIKINGDR3 
Default point source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag3 
vikingSource 
VIKINGDR4 
Default point source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zAperMag3 
vikingSource 
VIKINGv20110714 
Default point source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag3 
vikingSource 
VIKINGv20111019 
Default point source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag3 
vikingSource 
VIKINGv20130417 
Default point source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag3 
vikingSource 
VIKINGv20140402 
Default point source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zAperMag3 
vikingSource 
VIKINGv20150421 
Default point source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zAperMag3 
vvvSource 
VVVDR1 
Default point/extended source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag3 
vvvSource 
VVVDR2 
Default point/extended source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zAperMag3 
vvvSource 
VVVv20100531 
Default point/extended source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag3 
vvvSource 
VVVv20110718 
Default point/extended source Z aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag3 
vvvSynopticSource 
VVVDR1 
Default point/extended source Z aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag3 
vvvSynopticSource 
VVVDR2 
Default point/extended source Z aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zAperMag3Err 
svNgc253Source 
SVNGC253v20100429 
Error in default point/extended source Z mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag3Err 
svOrionSource 
SVORIONv20100429 
Error in default point/extended source Z mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag3Err 
ultravistaSource 
ULTRAVISTAv20100429 
Error in default point/extended source Z mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag3Err 
videoSource 
VIDEODR2 
Error in default point/extended source Z mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag3Err 
videoSource 
VIDEODR3 
Error in default point/extended source Z mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag3Err 
videoSource 
VIDEODR4 
Error in default point/extended source Z mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.opt.I;phot.mag 
zAperMag3Err 
videoSource 
VIDEOv20100513 
Error in default point/extended source Z mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag3Err 
videoSource 
VIDEOv20111208 
Error in default point/extended source Z mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag3Err 
vikingSource 
VIKINGDR2 
Error in default point/extended source Z mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag3Err 
vikingSource 
VIKINGDR3 
Error in default point/extended source Z mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag3Err 
vikingSource 
VIKINGDR4 
Error in default point/extended source Z mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.opt.I 
zAperMag3Err 
vikingSource 
VIKINGv20110714 
Error in default point/extended source Z mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag3Err 
vikingSource 
VIKINGv20111019 
Error in default point/extended source Z mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag3Err 
vikingSource 
VIKINGv20130417 
Error in default point/extended source Z mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag3Err 
vikingSource 
VIKINGv20140402 
Error in default point/extended source Z mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag3Err 
vikingSource 
VIKINGv20150421 
Error in default point/extended source Z mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.opt.I;phot.mag 
zAperMag3Err 
vvvSource 
VVVDR2 
Error in default point/extended source Z mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag3Err 
vvvSource 
VVVv20100531 
Error in default point/extended source Z mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag3Err 
vvvSource 
VVVv20110718 
Error in default point/extended source Z mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag3Err 
vvvSource, vvvSynopticSource 
VVVDR1 
Error in default point/extended source Z mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag4 
svNgc253Source 
SVNGC253v20100429 
Extended source Z aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag4 
svOrionSource 
SVORIONv20100429 
Extended source Z aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag4 
ultravistaSource 
ULTRAVISTAv20100429 
Extended source Z mag, no aperture correction applied 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag4 
videoSource 
VIDEODR2 
Point source Z aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag4 
videoSource 
VIDEODR3 
Point source Z aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag4 
videoSource 
VIDEODR4 
Point source Z aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zAperMag4 
videoSource 
VIDEOv20100513 
Extended source Z mag, no aperture correction applied 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag4 
videoSource 
VIDEOv20111208 
Point source Z aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag4 
vikingSource 
VIKINGDR2 
Point source Z aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag4 
vikingSource 
VIKINGDR3 
Point source Z aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag4 
vikingSource 
VIKINGDR4 
Point source Z aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zAperMag4 
vikingSource 
VIKINGv20110714 
Point source Z aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag4 
vikingSource 
VIKINGv20111019 
Point source Z aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag4 
vikingSource 
VIKINGv20130417 
Point source Z aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag4 
vikingSource 
VIKINGv20140402 
Point source Z aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zAperMag4 
vikingSource 
VIKINGv20150421 
Point source Z aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zAperMag4 
vvvSource 
VVVDR2 
Extended source Z aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zAperMag4 
vvvSource 
VVVv20100531 
Extended source Z aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag4 
vvvSource 
VVVv20110718 
Extended source Z aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag4 
vvvSource, vvvSynopticSource 
VVVDR1 
Extended source Z aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag4Err 
svNgc253Source 
SVNGC253v20100429 
Error in extended source Z mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag4Err 
svOrionSource 
SVORIONv20100429 
Error in extended source Z mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag4Err 
ultravistaSource 
ULTRAVISTAv20100429 
Error in extended source Z mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag4Err 
videoSource 
VIDEODR2 
Error in point/extended source Z mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag4Err 
videoSource 
VIDEODR3 
Error in point/extended source Z mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag4Err 
videoSource 
VIDEODR4 
Error in point/extended source Z mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.opt.I;phot.mag 
zAperMag4Err 
videoSource 
VIDEOv20100513 
Error in extended source Z mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag4Err 
videoSource 
VIDEOv20111208 
Error in point/extended source Z mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag4Err 
vikingSource 
VIKINGDR2 
Error in point/extended source Z mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag4Err 
vikingSource 
VIKINGDR3 
Error in point/extended source Z mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag4Err 
vikingSource 
VIKINGDR4 
Error in point/extended source Z mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.opt.I 
zAperMag4Err 
vikingSource 
VIKINGv20110714 
Error in point/extended source Z mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag4Err 
vikingSource 
VIKINGv20111019 
Error in point/extended source Z mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag4Err 
vikingSource 
VIKINGv20130417 
Error in point/extended source Z mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag4Err 
vikingSource 
VIKINGv20140402 
Error in point/extended source Z mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag4Err 
vikingSource 
VIKINGv20150421 
Error in point/extended source Z mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.opt.I;phot.mag 
zAperMag4Err 
vvvSource 
VVVDR2 
Error in extended source Z mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag4Err 
vvvSource 
VVVv20100531 
Error in extended source Z mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag4Err 
vvvSource 
VVVv20110718 
Error in extended source Z mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag4Err 
vvvSource, vvvSynopticSource 
VVVDR1 
Error in extended source Z mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag5 
vvvSynopticSource 
VVVDR1 
Extended source Z aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag5 
vvvSynopticSource 
VVVDR2 
Extended source Z aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zAperMag5Err 
vvvSynopticSource 
VVVDR1 
Error in extended source Z mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag5Err 
vvvSynopticSource 
VVVDR2 
Error in extended source Z mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag6 
svNgc253Source 
SVNGC253v20100429 
Extended source Z aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag6 
svOrionSource 
SVORIONv20100429 
Extended source Z aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag6 
ultravistaSource 
ULTRAVISTAv20100429 
Extended source Z mag, no aperture correction applied 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag6 
videoSource 
VIDEODR2 
Point source Z aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag6 
videoSource 
VIDEODR3 
Point source Z aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag6 
videoSource 
VIDEODR4 
Point source Z aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zAperMag6 
videoSource 
VIDEOv20100513 
Extended source Z mag, no aperture correction applied 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag6 
videoSource 
VIDEOv20111208 
Point source Z aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag6 
vikingSource 
VIKINGDR2 
Point source Z aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag6 
vikingSource 
VIKINGDR3 
Point source Z aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag6 
vikingSource 
VIKINGDR4 
Point source Z aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zAperMag6 
vikingSource 
VIKINGv20110714 
Point source Z aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag6 
vikingSource 
VIKINGv20111019 
Point source Z aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag6 
vikingSource 
VIKINGv20130417 
Point source Z aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMag6 
vikingSource 
VIKINGv20140402 
Point source Z aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zAperMag6 
vikingSource 
VIKINGv20150421 
Point source Z aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zAperMag6Err 
svNgc253Source 
SVNGC253v20100429 
Error in extended source Z mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag6Err 
svOrionSource 
SVORIONv20100429 
Error in extended source Z mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag6Err 
ultravistaSource 
ULTRAVISTAv20100429 
Error in extended source Z mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag6Err 
videoSource 
VIDEODR2 
Error in point/extended source Z mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag6Err 
videoSource 
VIDEODR3 
Error in point/extended source Z mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag6Err 
videoSource 
VIDEODR4 
Error in point/extended source Z mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.opt.I;phot.mag 
zAperMag6Err 
videoSource 
VIDEOv20100513 
Error in extended source Z mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag6Err 
videoSource 
VIDEOv20111208 
Error in point/extended source Z mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag6Err 
vikingSource 
VIKINGDR2 
Error in point/extended source Z mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag6Err 
vikingSource 
VIKINGDR3 
Error in point/extended source Z mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag6Err 
vikingSource 
VIKINGDR4 
Error in point/extended source Z mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.opt.I 
zAperMag6Err 
vikingSource 
VIKINGv20110714 
Error in point/extended source Z mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag6Err 
vikingSource 
VIKINGv20111019 
Error in point/extended source Z mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag6Err 
vikingSource 
VIKINGv20130417 
Error in point/extended source Z mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag6Err 
vikingSource 
VIKINGv20140402 
Error in point/extended source Z mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
zAperMag6Err 
vikingSource 
VIKINGv20150421 
Error in point/extended source Z mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.opt.I;phot.mag 
zAperMagNoAperCorr3 
videoSource 
VIDEODR2 
Default extended source Z aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMagNoAperCorr3 
videoSource 
VIDEODR3 
Default extended source Z aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMagNoAperCorr3 
videoSource 
VIDEODR4 
Default extended source Z aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zAperMagNoAperCorr3 
videoSource 
VIDEOv20111208 
Default extended source Z aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMagNoAperCorr3 
vikingSource 
VIKINGDR2 
Default extended source Z aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMagNoAperCorr3 
vikingSource 
VIKINGDR3 
Default extended source Z aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMagNoAperCorr3 
vikingSource 
VIKINGDR4 
Default extended source Z aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zAperMagNoAperCorr3 
vikingSource 
VIKINGv20110714 
Default extended source Z aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMagNoAperCorr3 
vikingSource 
VIKINGv20111019 
Default extended source Z aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMagNoAperCorr3 
vikingSource 
VIKINGv20130417 
Default extended source Z aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMagNoAperCorr3 
vikingSource 
VIKINGv20140402 
Default extended source Z aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zAperMagNoAperCorr3 
vikingSource 
VIKINGv20150421 
Default extended source Z aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zAperMagNoAperCorr4 
videoSource 
VIDEODR2 
Extended source Z aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMagNoAperCorr4 
videoSource 
VIDEODR3 
Extended source Z aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMagNoAperCorr4 
videoSource 
VIDEODR4 
Extended source Z aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zAperMagNoAperCorr4 
videoSource 
VIDEOv20111208 
Extended source Z aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMagNoAperCorr4 
vikingSource 
VIKINGDR2 
Extended source Z aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMagNoAperCorr4 
vikingSource 
VIKINGDR3 
Extended source Z aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMagNoAperCorr4 
vikingSource 
VIKINGDR4 
Extended source Z aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zAperMagNoAperCorr4 
vikingSource 
VIKINGv20110714 
Extended source Z aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMagNoAperCorr4 
vikingSource 
VIKINGv20111019 
Extended source Z aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMagNoAperCorr4 
vikingSource 
VIKINGv20130417 
Extended source Z aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMagNoAperCorr4 
vikingSource 
VIKINGv20140402 
Extended source Z aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zAperMagNoAperCorr4 
vikingSource 
VIKINGv20150421 
Extended source Z aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zAperMagNoAperCorr6 
videoSource 
VIDEODR2 
Extended source Z aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMagNoAperCorr6 
videoSource 
VIDEODR3 
Extended source Z aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMagNoAperCorr6 
videoSource 
VIDEODR4 
Extended source Z aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zAperMagNoAperCorr6 
videoSource 
VIDEOv20111208 
Extended source Z aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMagNoAperCorr6 
vikingSource 
VIKINGDR2 
Extended source Z aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMagNoAperCorr6 
vikingSource 
VIKINGDR3 
Extended source Z aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMagNoAperCorr6 
vikingSource 
VIKINGDR4 
Extended source Z aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zAperMagNoAperCorr6 
vikingSource 
VIKINGv20110714 
Extended source Z aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMagNoAperCorr6 
vikingSource 
VIKINGv20111019 
Extended source Z aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMagNoAperCorr6 
vikingSource 
VIKINGv20130417 
Extended source Z aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zAperMagNoAperCorr6 
vikingSource 
VIKINGv20140402 
Extended source Z aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zAperMagNoAperCorr6 
vikingSource 
VIKINGv20150421 
Extended source Z aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zaStratAst 
videoVarFrameSetInfo 
VIDEODR2 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Z band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
zaStratAst 
videoVarFrameSetInfo 
VIDEODR3 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Z band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
zaStratAst 
videoVarFrameSetInfo 
VIDEODR4 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Z band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.opt.I 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
zaStratAst 
videoVarFrameSetInfo 
VIDEOv20111208 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Z band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
zaStratAst 
vikingVarFrameSetInfo 
VIKINGv20110714 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Z band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
zaStratPht 
videoVarFrameSetInfo 
VIDEODR2 
Strateva parameter, a, in fit to photometric rms vs magnitude in Z band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
zaStratPht 
videoVarFrameSetInfo 
VIDEODR3 
Strateva parameter, a, in fit to photometric rms vs magnitude in Z band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
zaStratPht 
videoVarFrameSetInfo 
VIDEODR4 
Strateva parameter, a, in fit to photometric rms vs magnitude in Z band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.opt.I 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
zaStratPht 
videoVarFrameSetInfo 
VIDEOv20111208 
Strateva parameter, a, in fit to photometric rms vs magnitude in Z band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
zaStratPht 
vikingVarFrameSetInfo 
VIKINGv20110714 
Strateva parameter, a, in fit to photometric rms vs magnitude in Z band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
zAverageConf 
svNgc253Source 
SVNGC253v20100429 
average confidence in 2 arcsec diameter default aperture (aper3) Z 
real 
4 

99999999 
meta.code 
zAverageConf 
svOrionSource 
SVORIONv20100429 
average confidence in 2 arcsec diameter default aperture (aper3) Z 
real 
4 

99999999 
meta.code 
zAverageConf 
vikingSource 
VIKINGDR2 
average confidence in 2 arcsec diameter default aperture (aper3) Z 
real 
4 

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

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

0.9999995e9 
stat.likelihood;em.opt.I 
zAverageConf 
vikingSource 
VIKINGv20110714 
average confidence in 2 arcsec diameter default aperture (aper3) Z 
real 
4 

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

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

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

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

0.9999995e9 
stat.likelihood;em.opt.I 
zAverageConf 
vvvSource 
VVVDR2 
average confidence in 2 arcsec diameter default aperture (aper3) Z 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.NIR 
zAverageConf 
vvvSource, vvvSynopticSource 
VVVDR1 
average confidence in 2 arcsec diameter default aperture (aper3) Z 
real 
4 

99999999 
stat.likelihood;em.IR.NIR 
zbestAper 
videoVariability 
VIDEODR2 
Best aperture (16) for photometric statistics in the Z band 
int 
4 

9999 

Aperture magnitude (16) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) 
zbestAper 
videoVariability 
VIDEODR3 
Best aperture (16) for photometric statistics in the Z band 
int 
4 

9999 
meta.code.class;em.IR.NIR 
Aperture magnitude (16) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) 
zbestAper 
videoVariability 
VIDEODR4 
Best aperture (16) for photometric statistics in the Z band 
int 
4 

9999 
meta.code.class;em.opt.I 
Aperture magnitude (16) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) 
zbestAper 
videoVariability 
VIDEOv20111208 
Best aperture (16) for photometric statistics in the Z band 
int 
4 

9999 

Aperture magnitude (16) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) 
zbestAper 
vikingVariability 
VIKINGv20110714 
Best aperture (16) for photometric statistics in the Z band 
int 
4 

9999 

Aperture magnitude (16) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) 
zbStratAst 
videoVarFrameSetInfo 
VIDEODR2 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Z band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
zbStratAst 
videoVarFrameSetInfo 
VIDEODR3 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Z band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
zbStratAst 
videoVarFrameSetInfo 
VIDEODR4 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Z band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.opt.I 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
zbStratAst 
videoVarFrameSetInfo 
VIDEOv20111208 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Z band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
zbStratAst 
vikingVarFrameSetInfo 
VIKINGv20110714 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Z band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
zbStratPht 
videoVarFrameSetInfo 
VIDEODR2 
Strateva parameter, b, in fit to photometric rms vs magnitude in Z band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
zbStratPht 
videoVarFrameSetInfo 
VIDEODR3 
Strateva parameter, b, in fit to photometric rms vs magnitude in Z band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
zbStratPht 
videoVarFrameSetInfo 
VIDEODR4 
Strateva parameter, b, in fit to photometric rms vs magnitude in Z band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.opt.I 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
zbStratPht 
videoVarFrameSetInfo 
VIDEOv20111208 
Strateva parameter, b, in fit to photometric rms vs magnitude in Z band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
zbStratPht 
vikingVarFrameSetInfo 
VIKINGv20110714 
Strateva parameter, b, in fit to photometric rms vs magnitude in Z band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
ZCATERR 
target 
SIXDF 
error on velocity in ZCAT 
int 
4 
km/s 


ZCATREF 
target 
SIXDF 
ZCAT reference 
smallint 
2 



ZCATVEL 
target 
SIXDF 
velocity in ZCAT 
int 
4 
km/s 


zchiSqAst 
videoVarFrameSetInfo 
VIDEODR2 
Goodness of fit of Strateva function to astrometric data in Z band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
zchiSqAst 
videoVarFrameSetInfo 
VIDEODR3 
Goodness of fit of Strateva function to astrometric data in Z band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
zchiSqAst 
videoVarFrameSetInfo 
VIDEODR4 
Goodness of fit of Strateva function to astrometric data in Z band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.opt.I 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
zchiSqAst 
videoVarFrameSetInfo 
VIDEOv20111208 
Goodness of fit of Strateva function to astrometric data in Z band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
zchiSqAst 
vikingVarFrameSetInfo 
VIKINGv20110714 
Goodness of fit of Strateva function to astrometric data in Z band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
zchiSqpd 
videoVariability 
VIDEODR2 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zchiSqpd 
videoVariability 
VIDEODR3 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zchiSqpd 
videoVariability 
VIDEODR4 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2;em.opt.I 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zchiSqpd 
videoVariability 
VIDEOv20111208 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zchiSqpd 
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. 
zchiSqPht 
videoVarFrameSetInfo 
VIDEODR2 
Goodness of fit of Strateva function to photometric data in Z band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
zchiSqPht 
videoVarFrameSetInfo 
VIDEODR3 
Goodness of fit of Strateva function to photometric data in Z band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
zchiSqPht 
videoVarFrameSetInfo 
VIDEODR4 
Goodness of fit of Strateva function to photometric data in Z band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.opt.I 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
zchiSqPht 
videoVarFrameSetInfo 
VIDEOv20111208 
Goodness of fit of Strateva function to photometric data in Z band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
zchiSqPht 
vikingVarFrameSetInfo 
VIKINGv20110714 
Goodness of fit of Strateva function to photometric data in Z band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
zClass 
svNgc253Source 
SVNGC253v20100429 
discrete image classification flag in Z 
smallint 
2 

9999 
src.class 
zClass 
svOrionSource 
SVORIONv20100429 
discrete image classification flag in Z 
smallint 
2 

9999 
src.class 
zClass 
ultravistaSource, ultravistaSourceRemeasurement 
ULTRAVISTAv20100429 
discrete image classification flag in Z 
smallint 
2 

9999 
src.class 
zClass 
videoSource 
VIDEODR2 
discrete image classification flag in Z 
smallint 
2 

9999 
src.class 
zClass 
videoSource 
VIDEODR3 
discrete image classification flag in Z 
smallint 
2 

9999 
src.class 
zClass 
videoSource 
VIDEODR4 
discrete image classification flag in Z 
smallint 
2 

9999 
src.class;em.opt.I 
zClass 
videoSource 
VIDEOv20111208 
discrete image classification flag in Z 
smallint 
2 

9999 
src.class 
zClass 
videoSource, videoSourceRemeasurement 
VIDEOv20100513 
discrete image classification flag in Z 
smallint 
2 

9999 
src.class 
zClass 
vikingSource 
VIKINGDR2 
discrete image classification flag in Z 
smallint 
2 

9999 
src.class 
zClass 
vikingSource 
VIKINGDR3 
discrete image classification flag in Z 
smallint 
2 

9999 
src.class 
zClass 
vikingSource 
VIKINGDR4 
discrete image classification flag in Z 
smallint 
2 

9999 
src.class;em.opt.I 
zClass 
vikingSource 
VIKINGv20111019 
discrete image classification flag in Z 
smallint 
2 

9999 
src.class 
zClass 
vikingSource 
VIKINGv20130417 
discrete image classification flag in Z 
smallint 
2 

9999 
src.class 
zClass 
vikingSource 
VIKINGv20140402 
discrete image classification flag in Z 
smallint 
2 

9999 
src.class 
zClass 
vikingSource 
VIKINGv20150421 
discrete image classification flag in Z 
smallint 
2 

9999 
src.class;em.opt.I 
zClass 
vikingSource, vikingSourceRemeasurement 
VIKINGv20110714 
discrete image classification flag in Z 
smallint 
2 

9999 
src.class 
zClass 
vvvSource 
VVVDR2 
discrete image classification flag in Z 
smallint 
2 

9999 
src.class 
zClass 
vvvSource 
VVVv20110718 
discrete image classification flag in Z 
smallint 
2 

9999 
src.class 
zClass 
vvvSource, vvvSourceRemeasurement 
VVVv20100531 
discrete image classification flag in Z 
smallint 
2 

9999 
src.class 
zClass 
vvvSource, vvvSynopticSource 
VVVDR1 
discrete image classification flag in Z 
smallint 
2 

9999 
src.class 
zClassStat 
svNgc253Source 
SVNGC253v20100429 
N(0,1) stellarnessofprofile statistic in Z 
real 
4 

0.9999995e9 
stat 
zClassStat 
svOrionSource 
SVORIONv20100429 
N(0,1) stellarnessofprofile statistic in Z 
real 
4 

0.9999995e9 
stat 
zClassStat 
ultravistaSource 
ULTRAVISTAv20100429 
SExtractor classification statistic in Z 
real 
4 

0.9999995e9 
stat 
zClassStat 
ultravistaSourceRemeasurement 
ULTRAVISTAv20100429 
N(0,1) stellarnessofprofile statistic in Z 
real 
4 

0.9999995e9 
stat 
zClassStat 
videoSource 
VIDEODR2 
SExtractor classification statistic in Z 
real 
4 

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

0.9999995e9 
stat 
zClassStat 
vvvSource 
VVVv20100531 
SExtractor classification statistic in Z 
real 
4 

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

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

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

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

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

0.9999995e9 
stat 
zcStratAst 
videoVarFrameSetInfo 
VIDEODR2 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Z band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
zcStratAst 
videoVarFrameSetInfo 
VIDEODR3 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Z band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
zcStratAst 
videoVarFrameSetInfo 
VIDEODR4 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Z band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.opt.I 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
zcStratAst 
videoVarFrameSetInfo 
VIDEOv20111208 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Z band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
zcStratAst 
vikingVarFrameSetInfo 
VIKINGv20110714 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Z band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
zcStratPht 
videoVarFrameSetInfo 
VIDEODR2 
Strateva parameter, c, in fit to photometric rms vs magnitude in Z band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
zcStratPht 
videoVarFrameSetInfo 
VIDEODR3 
Strateva parameter, c, in fit to photometric rms vs magnitude in Z band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
zcStratPht 
videoVarFrameSetInfo 
VIDEODR4 
Strateva parameter, c, in fit to photometric rms vs magnitude in Z band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.opt.I 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
zcStratPht 
videoVarFrameSetInfo 
VIDEOv20111208 
Strateva parameter, c, in fit to photometric rms vs magnitude in Z band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
zcStratPht 
vikingVarFrameSetInfo 
VIKINGv20110714 
Strateva parameter, c, in fit to photometric rms vs magnitude in Z band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
zd 
twomass_scn 
2MASS 
Scan's distance from the zenith at beginning of scan. 
real 
4 
degrees 

stat.fit.residual;pos.az.zd 
zd 
twomass_sixx2_scn 
2MASS 
beginning zenith distance of scan data 
real 
4 
deg 


zDeblend 
ultravistaSource, ultravistaSourceRemeasurement 
ULTRAVISTAv20100429 
placeholder flag indicating parent/child relation in Z 
int 
4 

99999999 
meta.code 
zDeblend 
videoSource, videoSourceRemeasurement 
VIDEOv20100513 
placeholder flag indicating parent/child relation in Z 
int 
4 

99999999 
meta.code 
zDeblend 
vikingSourceRemeasurement 
VIKINGv20110714 
placeholder flag indicating parent/child relation in Z 
int 
4 

99999999 
meta.code 
zDeblend 
vikingSourceRemeasurement 
VIKINGv20111019 
placeholder flag indicating parent/child relation in Z 
int 
4 

99999999 
meta.code 
zDeblend 
vvvSource 
VVVv20110718 
placeholder flag indicating parent/child relation in Z 
int 
4 

99999999 
meta.code 
zDeblend 
vvvSource, vvvSourceRemeasurement 
VVVv20100531 
placeholder flag indicating parent/child relation in Z 
int 
4 

99999999 
meta.code 
zEll 
svNgc253Source 
SVNGC253v20100429 
1b/a, where a/b=semimajor/minor axes in Z 
real 
4 

0.9999995e9 
src.ellipticity 
zEll 
svOrionSource 
SVORIONv20100429 
1b/a, where a/b=semimajor/minor axes in Z 
real 
4 

0.9999995e9 
src.ellipticity 
zEll 
ultravistaSource, ultravistaSourceRemeasurement 
ULTRAVISTAv20100429 
1b/a, where a/b=semimajor/minor axes in Z 
real 
4 

0.9999995e9 
src.ellipticity 
zEll 
videoSource 
VIDEODR2 
1b/a, where a/b=semimajor/minor axes in Z 
real 
4 

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

0.9999995e9 
src.ellipticity 
zEll 
vvvSource, vvvSynopticSource 
VVVDR1 
1b/a, where a/b=semimajor/minor axes in Z 
real 
4 

0.9999995e9 
src.ellipticity 
ZEMIBESTERR 
spectra 
SIXDF 
error on the selected emission line redshift, 0.0 if not measured 
real 
4 



zeNum 
svNgc253MergeLog 
SVNGC253v20100429 
the extension number of this Z frame 
tinyint 
1 


meta.number 
zeNum 
svOrionMergeLog 
SVORIONv20100429 
the extension number of this Z frame 
tinyint 
1 


meta.number 
zeNum 
ultravistaMergeLog 
ULTRAVISTAv20100429 
the extension number of this Z frame 
tinyint 
1 


meta.number 
zeNum 
videoMergeLog 
VIDEODR2 
the extension number of this Z frame 
tinyint 
1 


meta.number 
zeNum 
videoMergeLog 
VIDEODR3 
the extension number of this Z frame 
tinyint 
1 


meta.number 
zeNum 
videoMergeLog 
VIDEODR4 
the extension number of this Z frame 
tinyint 
1 


meta.number;em.opt.I 
zeNum 
videoMergeLog 
VIDEOv20100513 
the extension number of this Z frame 
tinyint 
1 


meta.number 
zeNum 
videoMergeLog 
VIDEOv20111208 
the extension number of this Z frame 
tinyint 
1 


meta.number 
zeNum 
vikingMergeLog 
VIKINGDR2 
the extension number of this Z frame 
tinyint 
1 


meta.number 
zeNum 
vikingMergeLog 
VIKINGDR3 
the extension number of this Z frame 
tinyint 
1 


meta.number 
zeNum 
vikingMergeLog 
VIKINGDR4 
the extension number of this Z frame 
tinyint 
1 


meta.number;em.opt.I 
zeNum 
vikingMergeLog 
VIKINGv20110714 
the extension number of this Z frame 
tinyint 
1 


meta.number 
zeNum 
vikingMergeLog 
VIKINGv20111019 
the extension number of this Z frame 
tinyint 
1 


meta.number 
zeNum 
vikingMergeLog 
VIKINGv20130417 
the extension number of this Z frame 
tinyint 
1 


meta.number 
zeNum 
vikingMergeLog 
VIKINGv20140402 
the extension number of this Z frame 
tinyint 
1 


meta.number 
zeNum 
vikingMergeLog 
VIKINGv20150421 
the extension number of this Z frame 
tinyint 
1 


meta.number;em.opt.I 
zeNum 
vvvMergeLog 
VVVDR2 
the extension number of this Z frame 
tinyint 
1 


meta.number 
zeNum 
vvvMergeLog 
VVVv20100531 
the extension number of this Z frame 
tinyint 
1 


meta.number 
zeNum 
vvvMergeLog 
VVVv20110718 
the extension number of this Z frame 
tinyint 
1 


meta.number 
zeNum 
vvvMergeLog, vvvSynopticMergeLog 
VVVDR1 
the extension number of this Z frame 
tinyint 
1 


meta.number 
zeroPoint 
ExternalProduct 
VHSDR3 
Zeropoint of each product 
real 
4 

0.9999995e9 

zeroPoint 
ExternalProduct 
VHSv20150108 
Zeropoint of each product 
real 
4 

0.9999995e9 

zeroPoint 
ExternalProduct 
VIDEODR4 
Zeropoint of each product 
real 
4 

0.9999995e9 

zeroPoint 
ExternalProduct 
VIDEOv20111208 
Zeropoint of each product 
real 
4 

0.9999995e9 

zeroPoint 
ExternalProduct 
VIKINGDR4 
Zeropoint of each product 
real 
4 

0.9999995e9 

zeroPoint 
ExternalProduct 
VIKINGv20150421 
Zeropoint of each product 
real 
4 

0.9999995e9 

zeroPoint 
ExternalProduct 
VMCDR3 
Zeropoint of each product 
real 
4 

0.9999995e9 

zeroPoint 
ExternalProduct 
VMCv20140428 
Zeropoint of each product 
real 
4 

0.9999995e9 

zeroPoint 
ExternalProduct 
VMCv20140903 
Zeropoint of each product 
real 
4 

0.9999995e9 

zeroPoint 
ExternalProduct 
VMCv20150309 
Zeropoint of each product 
real 
4 

0.9999995e9 

zeroPoint 
ExternalProduct 
VSAQC 
Zeropoint of each product 
real 
4 

0.9999995e9 

zErrBits 
svNgc253Source 
SVNGC253v20100429 
processing warning/error bitwise flags in Z 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
zErrBits 
svOrionSource 
SVORIONv20100429 
processing warning/error bitwise flags in Z 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
zErrBits 
ultravistaSource 
ULTRAVISTAv20100429 
processing warning/error bitwise flags in Z 
int 
4 

99999999 
meta.code 
This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows: Bit Flag  Meaning   1  The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected).   2  The object was originally blended with another   4  At least one pixel is saturated (or very close to)   8  The object is truncated (too close to an image boundary)   16  Object's aperture data are incomplete or corrupted   32  Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters.   64  Memory overflow occurred during deblending   128  Memory overflow occurred during extraction  

zErrBits 
ultravistaSourceRemeasurement 
ULTRAVISTAv20100429 
processing warning/error bitwise flags in Z 
int 
4 

99999999 
meta.code 
zErrBits 
videoSource 
VIDEODR2 
processing warning/error bitwise flags in Z 
int 
4 

99999999 
meta.code 
This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows: Bit Flag  Meaning   1  The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected).   2  The object was originally blended with another   4  At least one pixel is saturated (or very close to)   8  The object is truncated (too close to an image boundary)   16  Object's aperture data are incomplete or corrupted   32  Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters.   64  Memory overflow occurred during deblending   128  Memory overflow occurred during extraction  

zErrBits 
videoSource 
VIDEODR3 
processing warning/error bitwise flags in Z 
int 
4 

99999999 
meta.code 
This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows: Bit Flag  Meaning   1  The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected).   2  The object was originally blended with another   4  At least one pixel is saturated (or very close to)   8  The object is truncated (too close to an image boundary)   16  Object's aperture data are incomplete or corrupted   32  Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters.   64  Memory overflow occurred during deblending   128  Memory overflow occurred during extraction  

zErrBits 
videoSource 
VIDEODR4 
processing warning/error bitwise flags in Z 
int 
4 

99999999 
meta.code;em.opt.I 
This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows: Bit Flag  Meaning   1  The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected).   2  The object was originally blended with another   4  At least one pixel is saturated (or very close to)   8  The object is truncated (too close to an image boundary)   16  Object's aperture data are incomplete or corrupted   32  Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters.   64  Memory overflow occurred during deblending   128  Memory overflow occurred during extraction  

zErrBits 
videoSource 
VIDEOv20100513 
processing warning/error bitwise flags in Z 
int 
4 

99999999 
meta.code 
This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows: Bit Flag  Meaning   1  The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected).   2  The object was originally blended with another   4  At least one pixel is saturated (or very close to)   8  The object is truncated (too close to an image boundary)   16  Object's aperture data are incomplete or corrupted   32  Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters.   64  Memory overflow occurred during deblending   128  Memory overflow occurred during extraction  

zErrBits 
videoSource 
VIDEOv20111208 
processing warning/error bitwise flags in Z 
int 
4 

99999999 
meta.code 
This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows: Bit Flag  Meaning   1  The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected).   2  The object was originally blended with another   4  At least one pixel is saturated (or very close to)   8  The object is truncated (too close to an image boundary)   16  Object's aperture data are incomplete or corrupted   32  Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters.   64  Memory overflow occurred during deblending   128  Memory overflow occurred during extraction  

zErrBits 
videoSourceRemeasurement 
VIDEOv20100513 
processing warning/error bitwise flags in Z 
int 
4 

99999999 
meta.code 
zErrBits 
vikingSource 
VIKINGDR2 
processing warning/error bitwise flags in Z 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
zErrBits 
vikingSource 
VIKINGDR3 
processing warning/error bitwise flags in Z 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
zErrBits 
vikingSource 
VIKINGDR4 
processing warning/error bitwise flags in Z 
int 
4 

99999999 
meta.code;em.opt.I 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
zErrBits 
vikingSource 
VIKINGv20110714 
processing warning/error bitwise flags in Z 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
zErrBits 
vikingSource 
VIKINGv20111019 
processing warning/error bitwise flags in Z 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
zErrBits 
vikingSource 
VIKINGv20130417 
processing warning/error bitwise flags in Z 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
zErrBits 
vikingSource 
VIKINGv20140402 
processing warning/error bitwise flags in Z 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
zErrBits 
vikingSource 
VIKINGv20150421 
processing warning/error bitwise flags in Z 
int 
4 

99999999 
meta.code;em.opt.I 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
zErrBits 
vikingSourceRemeasurement 
VIKINGv20110714 
processing warning/error bitwise flags in Z 
int 
4 

99999999 
meta.code 
zErrBits 
vikingSourceRemeasurement 
VIKINGv20111019 
processing warning/error bitwise flags in Z 
int 
4 

99999999 
meta.code 
zErrBits 
vvvSource 
VVVDR2 
processing warning/error bitwise flags in Z 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
zErrBits 
vvvSource 
VVVv20100531 
processing warning/error bitwise flags in Z 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
zErrBits 
vvvSource 
VVVv20110718 
processing warning/error bitwise flags in Z 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
zErrBits 
vvvSource, vvvSynopticSource 
VVVDR1 
processing warning/error bitwise flags in Z 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
zErrBits 
vvvSourceRemeasurement 
VVVv20100531 
processing warning/error bitwise flags in Z 
int 
4 

99999999 
meta.code 
zErrBits 
vvvSourceRemeasurement 
VVVv20110718 
processing warning/error bitwise flags in Z 
int 
4 

99999999 
meta.code 
zEta 
svNgc253Source 
SVNGC253v20100429 
Offset of Z detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zEta 
svOrionSource 
SVORIONv20100429 
Offset of Z detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zEta 
ultravistaSource 
ULTRAVISTAv20100429 
Offset of Z detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zEta 
videoSource 
VIDEODR2 
Offset of Z detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zEta 
videoSource 
VIDEODR3 
Offset of Z detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zEta 
videoSource 
VIDEODR4 
Offset of Z detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.opt.I 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zEta 
videoSource 
VIDEOv20100513 
Offset of Z detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zEta 
videoSource 
VIDEOv20111208 
Offset of Z detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zEta 
vikingSource 
VIKINGDR2 
Offset of Z detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zEta 
vikingSource 
VIKINGDR3 
Offset of Z detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zEta 
vikingSource 
VIKINGDR4 
Offset of Z detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.opt.I 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zEta 
vikingSource 
VIKINGv20110714 
Offset of Z detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zEta 
vikingSource 
VIKINGv20111019 
Offset of Z detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zEta 
vikingSource 
VIKINGv20130417 
Offset of Z detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zEta 
vikingSource 
VIKINGv20140402 
Offset of Z detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zEta 
vikingSource 
VIKINGv20150421 
Offset of Z detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.opt.I 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zEta 
vvvSource 
VVVDR2 
Offset of Z detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zEta 
vvvSource 
VVVv20100531 
Offset of Z detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zEta 
vvvSource 
VVVv20110718 
Offset of Z detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zEta 
vvvSource, vvvSynopticSource 
VVVDR1 
Offset of Z detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zexpML 
videoVarFrameSetInfo 
VIDEODR2 
Expected magnitude limit of frameSet in this in Z band. 
real 
4 

0.9999995e9 

zexpML 
videoVarFrameSetInfo 
VIDEODR3 
Expected magnitude limit of frameSet in this in Z band. 
real 
4 

0.9999995e9 
phot.mag;stat.max;em.IR.NIR 
zexpML 
videoVarFrameSetInfo 
VIDEODR4 
Expected magnitude limit of frameSet in this in Z band. 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I;stat.max 
zexpML 
videoVarFrameSetInfo 
VIDEOv20111208 
Expected magnitude limit of frameSet in this in Z band. 
real 
4 

0.9999995e9 

zexpML 
vikingVarFrameSetInfo 
VIKINGv20110714 
Expected magnitude limit of frameSet in this in Z band. 
real 
4 

0.9999995e9 

zExpRms 
videoVariability 
VIDEODR2 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in Z band 
real 
4 
mag 
0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zExpRms 
videoVariability 
VIDEODR3 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in Z band 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.NIR 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zExpRms 
videoVariability 
VIDEODR4 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in Z band 
real 
4 
mag 
0.9999995e9 
stat.error;em.opt.I 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zExpRms 
videoVariability 
VIDEOv20111208 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in Z band 
real 
4 
mag 
0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zExpRms 
vikingVariability 
VIKINGv20110714 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in Z band 
real 
4 
mag 
0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
ZFINALERR 
spectra 
SIXDF 
error on final quoted redshift, 0.0 if not measured 
real 
4 



zGausig 
svNgc253Source 
SVNGC253v20100429 
RMS of axes of ellipse fit in Z 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
zGausig 
svOrionSource 
SVORIONv20100429 
RMS of axes of ellipse fit in Z 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
zGausig 
ultravistaSource, ultravistaSourceRemeasurement 
ULTRAVISTAv20100429 
RMS of axes of ellipse fit in Z 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
zGausig 
videoSource 
VIDEODR2 
RMS of axes of ellipse fit in Z 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
zGausig 
videoSource 
VIDEODR3 
RMS of axes of ellipse fit in Z 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
zGausig 
videoSource 
VIDEODR4 
RMS of axes of ellipse fit in Z 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.opt.I 
zGausig 
videoSource 
VIDEOv20111208 
RMS of axes of ellipse fit in Z 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
zGausig 
videoSource, videoSourceRemeasurement 
VIDEOv20100513 
RMS of axes of ellipse fit in Z 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
zGausig 
vikingSource 
VIKINGDR2 
RMS of axes of ellipse fit in Z 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
zGausig 
vikingSource 
VIKINGDR3 
RMS of axes of ellipse fit in Z 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
zGausig 
vikingSource 
VIKINGDR4 
RMS of axes of ellipse fit in Z 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.opt.I 
zGausig 
vikingSource 
VIKINGv20111019 
RMS of axes of ellipse fit in Z 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
zGausig 
vikingSource 
VIKINGv20130417 
RMS of axes of ellipse fit in Z 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
zGausig 
vikingSource 
VIKINGv20140402 
RMS of axes of ellipse fit in Z 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
zGausig 
vikingSource 
VIKINGv20150421 
RMS of axes of ellipse fit in Z 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.opt.I 
zGausig 
vikingSource, vikingSourceRemeasurement 
VIKINGv20110714 
RMS of axes of ellipse fit in Z 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
zGausig 
vvvSource 
VVVDR2 
RMS of axes of ellipse fit in Z 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
zGausig 
vvvSource 
VVVv20110718 
RMS of axes of ellipse fit in Z 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
zGausig 
vvvSource, vvvSourceRemeasurement 
VVVv20100531 
RMS of axes of ellipse fit in Z 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
zGausig 
vvvSource, vvvSynopticSource 
VVVDR1 
RMS of axes of ellipse fit in Z 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
zHalfRad 
videoSource 
VIDEODR4 
SExtractor halflight radius in Z band 
real 
4 
pixels 
0.9999995e9 
phys.angSize;em.opt.I 
zHlCorSMjRadAs 
svNgc253Source 
SVNGC253v20100429 
Seeing corrected halflight, semimajor axis in Z band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
zHlCorSMjRadAs 
ultravistaSource 
ULTRAVISTAv20100429 
Seeing corrected halflight, semimajor axis in Z band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
zHlCorSMjRadAs 
videoSource 
VIDEODR2 
Seeing corrected halflight, semimajor axis in Z band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
zHlCorSMjRadAs 
videoSource 
VIDEODR3 
Seeing corrected halflight, semimajor axis in Z band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
zHlCorSMjRadAs 
videoSource 
VIDEODR4 
Seeing corrected halflight, semimajor axis in Z band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.opt.I 
zHlCorSMjRadAs 
videoSource 
VIDEOv20100513 
Seeing corrected halflight, semimajor axis in Z band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
zHlCorSMjRadAs 
videoSource 
VIDEOv20111208 
Seeing corrected halflight, semimajor axis in Z band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
zHlCorSMjRadAs 
vikingSource 
VIKINGDR2 
Seeing corrected halflight, semimajor axis in Z band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
zHlCorSMjRadAs 
vikingSource 
VIKINGDR3 
Seeing corrected halflight, semimajor axis in Z band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
zHlCorSMjRadAs 
vikingSource 
VIKINGDR4 
Seeing corrected halflight, semimajor axis in Z band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.opt.I 
zHlCorSMjRadAs 
vikingSource 
VIKINGv20110714 
Seeing corrected halflight, semimajor axis in Z band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
zHlCorSMjRadAs 
vikingSource 
VIKINGv20111019 
Seeing corrected halflight, semimajor axis in Z band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
zHlCorSMjRadAs 
vikingSource 
VIKINGv20130417 
Seeing corrected halflight, semimajor axis in Z band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
zHlCorSMjRadAs 
vikingSource 
VIKINGv20140402 
Seeing corrected halflight, semimajor axis in Z band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
zHlCorSMjRadAs 
vikingSource 
VIKINGv20150421 
Seeing corrected halflight, semimajor axis in Z band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.opt.I 
zIntRms 
videoVariability 
VIDEODR2 
Intrinsic rms in Zband 
real 
4 
mag 
0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zIntRms 
videoVariability 
VIDEODR3 
Intrinsic rms in Zband 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.NIR 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zIntRms 
videoVariability 
VIDEODR4 
Intrinsic rms in Zband 
real 
4 
mag 
0.9999995e9 
stat.error;em.opt.I 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zIntRms 
videoVariability 
VIDEOv20111208 
Intrinsic rms in Zband 
real 
4 
mag 
0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zIntRms 
vikingVariability 
VIKINGv20110714 
Intrinsic rms in Zband 
real 
4 
mag 
0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zisDefAst 
videoVarFrameSetInfo 
VIDEODR2 
Use a default model for the astrometric noise in Z band. 
tinyint 
1 

0 

zisDefAst 
videoVarFrameSetInfo 
VIDEODR3 
Use a default model for the astrometric noise in Z band. 
tinyint 
1 

0 
meta.code;em.IR.NIR 
zisDefAst 
videoVarFrameSetInfo 
VIDEODR4 
Use a default model for the astrometric noise in Z band. 
tinyint 
1 

0 
meta.code;em.opt.I 
zisDefAst 
videoVarFrameSetInfo 
VIDEOv20111208 
Use a default model for the astrometric noise in Z band. 
tinyint 
1 

0 

zisDefPht 
videoVarFrameSetInfo 
VIDEODR2 
Use a default model for the photometric noise in Z band. 
tinyint 
1 

0 

zisDefPht 
videoVarFrameSetInfo 
VIDEODR3 
Use a default model for the photometric noise in Z band. 
tinyint 
1 

0 
meta.code;em.IR.NIR 
zisDefPht 
videoVarFrameSetInfo 
VIDEODR4 
Use a default model for the photometric noise in Z band. 
tinyint 
1 

0 
meta.code;em.opt.I 
zisDefPht 
videoVarFrameSetInfo 
VIDEOv20111208 
Use a default model for the photometric noise in Z band. 
tinyint 
1 

0 

zKronMag 
videoSource 
VIDEODR4 
Extended source Z mag (Kron  SExtractor MAG_AUTO) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zKronMagErr 
videoSource 
VIDEODR4 
Extended source Z mag error (Kron  SExtractor MAG_AUTO) 
real 
4 
mag 
0.9999995e9 
stat.error;em.opt.I;phot.mag 
zMag 
ultravistaSourceRemeasurement 
ULTRAVISTAv20100429 
Z mag (as appropriate for this merged source) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zMag 
videoSourceRemeasurement 
VIDEOv20100513 
Z mag (as appropriate for this merged source) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zMag 
vikingSourceRemeasurement 
VIKINGv20110714 
Z mag (as appropriate for this merged source) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zMag 
vikingSourceRemeasurement 
VIKINGv20111019 
Z mag (as appropriate for this merged source) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zMag 
vvvSourceRemeasurement 
VVVv20100531 
Z mag (as appropriate for this merged source) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zMag 
vvvSourceRemeasurement 
VVVv20110718 
Z mag (as appropriate for this merged source) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zMagErr 
ultravistaSourceRemeasurement 
ULTRAVISTAv20100429 
Error in Z mag 
real 
4 
mag 
0.9999995e9 
stat.error 
zMagErr 
videoSourceRemeasurement 
VIDEOv20100513 
Error in Z mag 
real 
4 
mag 
0.9999995e9 
stat.error 
zMagErr 
vikingSourceRemeasurement 
VIKINGv20110714 
Error in Z mag 
real 
4 
mag 
0.9999995e9 
stat.error 
zMagErr 
vikingSourceRemeasurement 
VIKINGv20111019 
Error in Z mag 
real 
4 
mag 
0.9999995e9 
stat.error 
zMagErr 
vvvSourceRemeasurement 
VVVv20100531 
Error in Z mag 
real 
4 
mag 
0.9999995e9 
stat.error 
zMagErr 
vvvSourceRemeasurement 
VVVv20110718 
Error in Z mag 
real 
4 
mag 
0.9999995e9 
stat.error 
zMagMAD 
videoVariability 
VIDEODR2 
Median Absolute Deviation of Z magnitude 
real 
4 
mag 
0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zMagMAD 
videoVariability 
VIDEODR3 
Median Absolute Deviation of Z magnitude 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.NIR 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zMagMAD 
videoVariability 
VIDEODR4 
Median Absolute Deviation of Z magnitude 
real 
4 
mag 
0.9999995e9 
stat.err;em.opt.I;phot.mag 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zMagMAD 
videoVariability 
VIDEOv20111208 
Median Absolute Deviation of Z magnitude 
real 
4 
mag 
0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zMagMAD 
vikingVariability 
VIKINGv20110714 
Median Absolute Deviation of Z magnitude 
real 
4 
mag 
0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zMagRms 
videoVariability 
VIDEODR2 
rms of Z magnitude 
real 
4 
mag 
0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zMagRms 
videoVariability 
VIDEODR3 
rms of Z magnitude 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.NIR 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zMagRms 
videoVariability 
VIDEODR4 
rms of Z magnitude 
real 
4 
mag 
0.9999995e9 
stat.error;em.opt.I;phot.mag 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zMagRms 
videoVariability 
VIDEOv20111208 
rms of Z magnitude 
real 
4 
mag 
0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zMagRms 
vikingVariability 
VIKINGv20110714 
rms of Z magnitude 
real 
4 
mag 
0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zmaxCadence 
videoVariability 
VIDEODR2 
maximum gap between observations 
real 
4 
days 
0.9999995e9 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
zmaxCadence 
videoVariability 
VIDEODR3 
maximum gap between observations 
real 
4 
days 
0.9999995e9 
time.interval;obs;stat.max 
The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
zmaxCadence 
videoVariability 
VIDEODR4 
maximum gap between observations 
real 
4 
days 
0.9999995e9 
time.interval;obs;stat.max 
The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
zmaxCadence 
videoVariability 
VIDEOv20111208 
maximum gap between observations 
real 
4 
days 
0.9999995e9 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
zmaxCadence 
vikingVariability 
VIKINGv20110714 
maximum gap between observations 
real 
4 
days 
0.9999995e9 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
zMaxMag 
videoVariability 
VIDEODR2 
Maximum magnitude in Z band, of good detections 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zMaxMag 
videoVariability 
VIDEODR3 
Maximum magnitude in Z band, of good detections 
real 
4 

0.9999995e9 
phot.mag;stat.max;em.IR.NIR 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zMaxMag 
videoVariability 
VIDEODR4 
Maximum magnitude in Z band, of good detections 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I;stat.max 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zMaxMag 
videoVariability 
VIDEOv20111208 
Maximum magnitude in Z band, of good detections 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zMaxMag 
vikingVariability 
VIKINGv20110714 
Maximum magnitude in Z band, of good detections 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zmeanMag 
videoVariability 
VIDEODR2 
Mean Z magnitude 
real 
4 
mag 
0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zmeanMag 
videoVariability 
VIDEODR3 
Mean Z magnitude 
real 
4 
mag 
0.9999995e9 
phot.mag;stat.mean;em.IR.NIR 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zmeanMag 
videoVariability 
VIDEODR4 
Mean Z magnitude 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I;stat.mean;em.opt.I 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zmeanMag 
videoVariability 
VIDEOv20111208 
Mean Z magnitude 
real 
4 
mag 
0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zmeanMag 
vikingVariability 
VIKINGv20110714 
Mean Z magnitude 
real 
4 
mag 
0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zmedCadence 
videoVariability 
VIDEODR2 
median gap between observations 
real 
4 
days 
0.9999995e9 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
zmedCadence 
videoVariability 
VIDEODR3 
median gap between observations 
real 
4 
days 
0.9999995e9 
time.interval;obs;stat.median 
The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
zmedCadence 
videoVariability 
VIDEODR4 
median gap between observations 
real 
4 
days 
0.9999995e9 
time.interval;obs;stat.median 
The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
zmedCadence 
videoVariability 
VIDEOv20111208 
median gap between observations 
real 
4 
days 
0.9999995e9 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
zmedCadence 
vikingVariability 
VIKINGv20110714 
median gap between observations 
real 
4 
days 
0.9999995e9 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
zmedianMag 
videoVariability 
VIDEODR2 
Median Z magnitude 
real 
4 
mag 
0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zmedianMag 
videoVariability 
VIDEODR3 
Median Z magnitude 
real 
4 
mag 
0.9999995e9 
phot.mag;stat.median;em.IR.NIR 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zmedianMag 
videoVariability 
VIDEODR4 
Median Z magnitude 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I;stat.median;em.opt.I 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zmedianMag 
videoVariability 
VIDEOv20111208 
Median Z magnitude 
real 
4 
mag 
0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zmedianMag 
vikingVariability 
VIKINGv20110714 
Median Z magnitude 
real 
4 
mag 
0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zmfID 
svNgc253MergeLog 
SVNGC253v20100429 
the UID of the relevant Z multiframe 
bigint 
8 


obs.field 
zmfID 
svOrionMergeLog 
SVORIONv20100429 
the UID of the relevant Z multiframe 
bigint 
8 


obs.field 
zmfID 
ultravistaMergeLog 
ULTRAVISTAv20100429 
the UID of the relevant Z multiframe 
bigint 
8 


obs.field 
zmfID 
videoMergeLog 
VIDEODR2 
the UID of the relevant Z multiframe 
bigint 
8 


obs.field 
zmfID 
videoMergeLog 
VIDEODR3 
the UID of the relevant Z multiframe 
bigint 
8 


meta.id;obs.field 
zmfID 
videoMergeLog 
VIDEODR4 
the UID of the relevant Z multiframe 
bigint 
8 


meta.id;obs.field;em.opt.I 
zmfID 
videoMergeLog 
VIDEOv20100513 
the UID of the relevant Z multiframe 
bigint 
8 


obs.field 
zmfID 
videoMergeLog 
VIDEOv20111208 
the UID of the relevant Z multiframe 
bigint 
8 


obs.field 
zmfID 
vikingMergeLog 
VIKINGDR2 
the UID of the relevant Z multiframe 
bigint 
8 


obs.field 
zmfID 
vikingMergeLog 
VIKINGDR3 
the UID of the relevant Z multiframe 
bigint 
8 


meta.id;obs.field 
zmfID 
vikingMergeLog 
VIKINGDR4 
the UID of the relevant Z multiframe 
bigint 
8 


meta.id;obs.field;em.opt.I 
zmfID 
vikingMergeLog 
VIKINGv20110714 
the UID of the relevant Z multiframe 
bigint 
8 


obs.field 
zmfID 
vikingMergeLog 
VIKINGv20111019 
the UID of the relevant Z multiframe 
bigint 
8 


obs.field 
zmfID 
vikingMergeLog 
VIKINGv20130417 
the UID of the relevant Z multiframe 
bigint 
8 


meta.id;obs.field 
zmfID 
vikingMergeLog 
VIKINGv20140402 
the UID of the relevant Z multiframe 
bigint 
8 


meta.id;obs.field 
zmfID 
vikingMergeLog 
VIKINGv20150421 
the UID of the relevant Z multiframe 
bigint 
8 


meta.id;obs.field;em.opt.I 
zmfID 
vvvMergeLog 
VVVDR2 
the UID of the relevant Z multiframe 
bigint 
8 


meta.id;obs.field 
zmfID 
vvvMergeLog 
VVVv20100531 
the UID of the relevant Z multiframe 
bigint 
8 


obs.field 
zmfID 
vvvMergeLog 
VVVv20110718 
the UID of the relevant Z multiframe 
bigint 
8 


obs.field 
zmfID 
vvvMergeLog, vvvSynopticMergeLog 
VVVDR1 
the UID of the relevant Z multiframe 
bigint 
8 


meta.id;obs.field 
zminCadence 
videoVariability 
VIDEODR2 
minimum gap between observations 
real 
4 
days 
0.9999995e9 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
zminCadence 
videoVariability 
VIDEODR3 
minimum gap between observations 
real 
4 
days 
0.9999995e9 
time.interval;obs;stat.min 
The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
zminCadence 
videoVariability 
VIDEODR4 
minimum gap between observations 
real 
4 
days 
0.9999995e9 
time.interval;obs;stat.min 
The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
zminCadence 
videoVariability 
VIDEOv20111208 
minimum gap between observations 
real 
4 
days 
0.9999995e9 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
zminCadence 
vikingVariability 
VIKINGv20110714 
minimum gap between observations 
real 
4 
days 
0.9999995e9 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
zMinMag 
videoVariability 
VIDEODR2 
Minimum magnitude in Z band, of good detections 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zMinMag 
videoVariability 
VIDEODR3 
Minimum magnitude in Z band, of good detections 
real 
4 

0.9999995e9 
phot.mag;stat.min;em.IR.NIR 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zMinMag 
videoVariability 
VIDEODR4 
Minimum magnitude in Z band, of good detections 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I;stat.min 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zMinMag 
videoVariability 
VIDEOv20111208 
Minimum magnitude in Z band, of good detections 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zMinMag 
vikingVariability 
VIKINGv20110714 
Minimum magnitude in Z band, of good detections 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zMjd 
vvvSynopticSource 
VVVDR1 
Modified Julian Day in Z band 
float 
8 
days 
0.9999995e9 
time.epoch 
zMjd 
vvvSynopticSource 
VVVDR2 
Modified Julian Day in Z band 
float 
8 
days 
0.9999995e9 
time.epoch 
zmy 
ultravistaSourceRemeasurement 
ULTRAVISTAv20100429 
Default colour ZY (using appropriate mags) 
real 
4 
mag 

PHOT_COLOR 
zmy 
videoSourceRemeasurement 
VIDEOv20100513 
Default colour ZY (using appropriate mags) 
real 
4 
mag 

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

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

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

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

PHOT_COLOR 
zmyErr 
ultravistaSourceRemeasurement 
ULTRAVISTAv20100429 
Error on colour ZY 
real 
4 
mag 

stat.error 
zmyErr 
videoSourceRemeasurement 
VIDEOv20100513 
Error on colour ZY 
real 
4 
mag 

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

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

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

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

stat.error 
zmyExt 
svNgc253Source 
SVNGC253v20100429 
Extended source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
svOrionSource 
SVORIONv20100429 
Extended source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
ultravistaSource 
ULTRAVISTAv20100429 
Extended source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
videoSource 
VIDEODR2 
Extended source colour ZY (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
videoSource 
VIDEODR3 
Extended source colour ZY (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
videoSource 
VIDEODR4 
Extended source colour ZY (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.opt.I;em.IR.NIR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
videoSource 
VIDEOv20100513 
Extended source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
videoSource 
VIDEOv20111208 
Extended source colour ZY (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
vikingSource 
VIKINGDR2 
Extended source colour ZY (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
vikingSource 
VIKINGDR3 
Extended source colour ZY (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
vikingSource 
VIKINGDR4 
Extended source colour ZY (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.opt.I;em.IR.NIR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
vikingSource 
VIKINGv20110714 
Extended source colour ZY (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
vikingSource 
VIKINGv20111019 
Extended source colour ZY (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
vikingSource 
VIKINGv20130417 
Extended source colour ZY (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
vikingSource 
VIKINGv20140402 
Extended source colour ZY (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.opt.I;em.IR.NIR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
vikingSource 
VIKINGv20150421 
Extended source colour ZY (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.opt.I;em.IR.NIR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExt 
vvvSource 
VVVv20100531 
Extended source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
svNgc253Source 
SVNGC253v20100429 
Error on extended source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
svOrionSource 
SVORIONv20100429 
Error on extended source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
ultravistaSource 
ULTRAVISTAv20100429 
Error on extended source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
videoSource 
VIDEODR2 
Error on extended source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
videoSource 
VIDEODR3 
Error on extended source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
videoSource 
VIDEODR4 
Error on extended source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error;em.opt.I;em.IR.NIR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
videoSource 
VIDEOv20100513 
Error on extended source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
videoSource 
VIDEOv20111208 
Error on extended source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
vikingSource 
VIKINGDR2 
Error on extended source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
vikingSource 
VIKINGDR3 
Error on extended source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
vikingSource 
VIKINGDR4 
Error on extended source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error;em.opt.I;em.IR.NIR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
vikingSource 
VIKINGv20110714 
Error on extended source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
vikingSource 
VIKINGv20111019 
Error on extended source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
vikingSource 
VIKINGv20130417 
Error on extended source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
vikingSource 
VIKINGv20140402 
Error on extended source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
vikingSource 
VIKINGv20150421 
Error on extended source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error;em.opt.I;em.IR.NIR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyExtErr 
vvvSource 
VVVv20100531 
Error on extended source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
svNgc253Source 
SVNGC253v20100429 
Point source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
svOrionSource 
SVORIONv20100429 
Point source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
ultravistaSource 
ULTRAVISTAv20100429 
Point source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
videoSource 
VIDEODR2 
Point source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
videoSource 
VIDEODR3 
Point source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
videoSource 
VIDEODR4 
Point source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.opt.I;em.IR.NIR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
videoSource 
VIDEOv20100513 
Point source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
videoSource 
VIDEOv20111208 
Point source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vikingSource 
VIKINGDR2 
Point source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vikingSource 
VIKINGDR3 
Point source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vikingSource 
VIKINGDR4 
Point source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.opt.I;em.IR.NIR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vikingSource 
VIKINGv20110714 
Point source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vikingSource 
VIKINGv20111019 
Point source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vikingSource 
VIKINGv20130417 
Point source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vikingSource 
VIKINGv20140402 
Point source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.opt.I;em.IR.NIR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vikingSource 
VIKINGv20150421 
Point source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.opt.I;em.IR.NIR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vvvSource 
VVVDR2 
Point source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.opt.I;em.IR.NIR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vvvSource 
VVVv20100531 
Point source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vvvSource 
VVVv20110718 
Point source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPnt 
vvvSource, vvvSynopticSource 
VVVDR1 
Point source colour ZY (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
svNgc253Source 
SVNGC253v20100429 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
svOrionSource 
SVORIONv20100429 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
ultravistaSource 
ULTRAVISTAv20100429 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
videoSource 
VIDEODR2 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
videoSource 
VIDEODR3 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
videoSource 
VIDEODR4 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error;em.opt.I;em.IR.NIR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
videoSource 
VIDEOv20100513 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
videoSource 
VIDEOv20111208 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vikingSource 
VIKINGDR2 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vikingSource 
VIKINGDR3 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vikingSource 
VIKINGDR4 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error;em.opt.I;em.IR.NIR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vikingSource 
VIKINGv20110714 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vikingSource 
VIKINGv20111019 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vikingSource 
VIKINGv20130417 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vikingSource 
VIKINGv20140402 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vikingSource 
VIKINGv20150421 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error;em.opt.I;em.IR.NIR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vvvSource 
VVVDR2 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vvvSource 
VVVv20100531 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vvvSource 
VVVv20110718 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zmyPntErr 
vvvSource, vvvSynopticSource 
VVVDR1 
Error on point source colour ZY 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
zndof 
videoVariability 
VIDEODR2 
Number of degrees of freedom for chisquare 
smallint 
2 

9999 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zndof 
videoVariability 
VIDEODR3 
Number of degrees of freedom for chisquare 
smallint 
2 

9999 
stat.fit.dof 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zndof 
videoVariability 
VIDEODR4 
Number of degrees of freedom for chisquare 
smallint 
2 

9999 
stat.fit.dof;em.opt.I 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zndof 
videoVariability 
VIDEOv20111208 
Number of degrees of freedom for chisquare 
smallint 
2 

9999 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zndof 
vikingVariability 
VIKINGv20110714 
Number of degrees of freedom for chisquare 
smallint 
2 

9999 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
znDofAst 
videoVarFrameSetInfo 
VIDEODR2 
Number of degrees of freedom of astrometric fit in Z band. 
smallint 
2 

9999 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
znDofAst 
videoVarFrameSetInfo 
VIDEODR3 
Number of degrees of freedom of astrometric fit in Z band. 
smallint 
2 

9999 
stat.fit.dof;stat.param;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
znDofAst 
videoVarFrameSetInfo 
VIDEODR4 
Number of degrees of freedom of astrometric fit in Z band. 
smallint 
2 

9999 
stat.fit.dof;stat.param;em.opt.I 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
znDofAst 
videoVarFrameSetInfo 
VIDEOv20111208 
Number of degrees of freedom of astrometric fit in Z band. 
smallint 
2 

9999 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
znDofAst 
vikingVarFrameSetInfo 
VIKINGv20110714 
Number of degrees of freedom of astrometric fit in Z band. 
smallint 
2 

9999 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
znDofPht 
videoVarFrameSetInfo 
VIDEODR2 
Number of degrees of freedom of photometric fit in Z band. 
smallint 
2 

9999 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
znDofPht 
videoVarFrameSetInfo 
VIDEODR3 
Number of degrees of freedom of photometric fit in Z band. 
smallint 
2 

9999 
stat.fit.dof;stat.param;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
znDofPht 
videoVarFrameSetInfo 
VIDEODR4 
Number of degrees of freedom of photometric fit in Z band. 
smallint 
2 

9999 
stat.fit.dof;stat.param;em.opt.I 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
znDofPht 
videoVarFrameSetInfo 
VIDEOv20111208 
Number of degrees of freedom of photometric fit in Z band. 
smallint 
2 

9999 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
znDofPht 
vikingVarFrameSetInfo 
VIKINGv20110714 
Number of degrees of freedom of photometric fit in Z band. 
smallint 
2 

9999 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
znFlaggedObs 
videoVariability 
VIDEODR2 
Number of detections in Z band flagged as potentially spurious by videoDetection.ppErrBits 
int 
4 

0 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
znFlaggedObs 
videoVariability 
VIDEODR3 
Number of detections in Z band flagged as potentially spurious by videoDetection.ppErrBits 
int 
4 

0 
meta.number 
The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
znFlaggedObs 
videoVariability 
VIDEODR4 
Number of detections in Z band flagged as potentially spurious by videoDetection.ppErrBits 
int 
4 

0 
meta.number;em.opt.I 
The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
znFlaggedObs 
videoVariability 
VIDEOv20111208 
Number of detections in Z band flagged as potentially spurious by videoDetection.ppErrBits 
int 
4 

0 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
znFlaggedObs 
vikingVariability 
VIKINGv20110714 
Number of detections in Z band flagged as potentially spurious by vikingDetection.ppErrBits 
int 
4 

0 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
znGoodObs 
videoVariability 
VIDEODR2 
Number of good detections in Z band 
int 
4 

0 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
znGoodObs 
videoVariability 
VIDEODR3 
Number of good detections in Z band 
int 
4 

0 
meta.number;em.IR.NIR 
The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
znGoodObs 
videoVariability 
VIDEODR4 
Number of good detections in Z band 
int 
4 

0 
meta.number;em.opt.I 
The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
znGoodObs 
videoVariability 
VIDEOv20111208 
Number of good detections in Z band 
int 
4 

0 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
znGoodObs 
vikingVariability 
VIKINGv20110714 
Number of good detections in Z band 
int 
4 

0 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
zNgt3sig 
videoVariability 
VIDEODR2 
Number of good detections in Zband that are more than 3 sigma deviations 
smallint 
2 

9999 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zNgt3sig 
videoVariability 
VIDEODR3 
Number of good detections in Zband that are more than 3 sigma deviations 
smallint 
2 

9999 
meta.number;em.IR.NIR 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zNgt3sig 
videoVariability 
VIDEODR4 
Number of good detections in Zband that are more than 3 sigma deviations 
smallint 
2 

9999 
meta.number;em.opt.I 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zNgt3sig 
videoVariability 
VIDEOv20111208 
Number of good detections in Zband that are more than 3 sigma deviations 
smallint 
2 

9999 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zNgt3sig 
vikingVariability 
VIKINGv20110714 
Number of good detections in Zband that are more than 3 sigma deviations 
smallint 
2 

9999 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
znMissingObs 
videoVariability 
VIDEODR2 
Number of Z band frames that this object should have been detected on and was not 
int 
4 

0 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
znMissingObs 
videoVariability 
VIDEODR3 
Number of Z band frames that this object should have been detected on and was not 
int 
4 

0 
meta.number;em.IR.NIR 
The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
znMissingObs 
videoVariability 
VIDEODR4 
Number of Z band frames that this object should have been detected on and was not 
int 
4 

0 
meta.number;em.opt.I 
The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
znMissingObs 
videoVariability 
VIDEOv20111208 
Number of Z band frames that this object should have been detected on and was not 
int 
4 

0 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
znMissingObs 
vikingVariability 
VIKINGv20110714 
Number of Z band frames that this object should have been detected on and was not 
int 
4 

0 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
zPA 
svNgc253Source 
SVNGC253v20100429 
ellipse fit celestial orientation in Z 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
zPA 
svOrionSource 
SVORIONv20100429 
ellipse fit celestial orientation in Z 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
zPA 
ultravistaSource, ultravistaSourceRemeasurement 
ULTRAVISTAv20100429 
ellipse fit celestial orientation in Z 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
zPA 
videoSource 
VIDEODR2 
ellipse fit celestial orientation in Z 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
zPA 
videoSource 
VIDEODR3 
ellipse fit celestial orientation in Z 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
zPA 
videoSource 
VIDEODR4 
ellipse fit celestial orientation in Z 
real 
4 
Degrees 
0.9999995e9 
pos.posAng;em.opt.I 
zPA 
videoSource 
VIDEOv20111208 
ellipse fit celestial orientation in Z 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
zPA 
videoSource, videoSourceRemeasurement 
VIDEOv20100513 
ellipse fit celestial orientation in Z 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
zPA 
vikingSource 
VIKINGDR2 
ellipse fit celestial orientation in Z 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
zPA 
vikingSource 
VIKINGDR3 
ellipse fit celestial orientation in Z 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
zPA 
vikingSource 
VIKINGDR4 
ellipse fit celestial orientation in Z 
real 
4 
Degrees 
0.9999995e9 
pos.posAng;em.opt.I 
zPA 
vikingSource 
VIKINGv20111019 
ellipse fit celestial orientation in Z 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
zPA 
vikingSource 
VIKINGv20130417 
ellipse fit celestial orientation in Z 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
zPA 
vikingSource 
VIKINGv20140402 
ellipse fit celestial orientation in Z 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
zPA 
vikingSource 
VIKINGv20150421 
ellipse fit celestial orientation in Z 
real 
4 
Degrees 
0.9999995e9 
pos.posAng;em.opt.I 
zPA 
vikingSource, vikingSourceRemeasurement 
VIKINGv20110714 
ellipse fit celestial orientation in Z 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
zPA 
vvvSource 
VVVDR2 
ellipse fit celestial orientation in Z 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
zPA 
vvvSource 
VVVv20110718 
ellipse fit celestial orientation in Z 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
zPA 
vvvSource, vvvSourceRemeasurement 
VVVv20100531 
ellipse fit celestial orientation in Z 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
zPA 
vvvSource, vvvSynopticSource 
VVVDR1 
ellipse fit celestial orientation in Z 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
zPetroMag 
svNgc253Source 
SVNGC253v20100429 
Extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zPetroMag 
svOrionSource 
SVORIONv20100429 
Extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zPetroMag 
ultravistaSource 
ULTRAVISTAv20100429 
Extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zPetroMag 
videoSource 
VIDEODR2 
Extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zPetroMag 
videoSource 
VIDEODR3 
Extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zPetroMag 
videoSource 
VIDEODR4 
Extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zPetroMag 
videoSource 
VIDEOv20100513 
Extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zPetroMag 
videoSource 
VIDEOv20111208 
Extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zPetroMag 
vikingSource 
VIKINGDR2 
Extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zPetroMag 
vikingSource 
VIKINGDR3 
Extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zPetroMag 
vikingSource 
VIKINGDR4 
Extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zPetroMag 
vikingSource 
VIKINGv20110714 
Extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zPetroMag 
vikingSource 
VIKINGv20111019 
Extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zPetroMag 
vikingSource 
VIKINGv20130417 
Extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zPetroMag 
vikingSource 
VIKINGv20140402 
Extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zPetroMag 
vikingSource 
VIKINGv20150421 
Extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zPetroMagErr 
svNgc253Source 
SVNGC253v20100429 
Error in extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
stat.error 
zPetroMagErr 
svOrionSource 
SVORIONv20100429 
Error in extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
stat.error 
zPetroMagErr 
ultravistaSource 
ULTRAVISTAv20100429 
Error in extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
stat.error 
zPetroMagErr 
videoSource 
VIDEODR2 
Error in extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
stat.error 
zPetroMagErr 
videoSource 
VIDEODR3 
Error in extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
stat.error 
zPetroMagErr 
videoSource 
VIDEODR4 
Error in extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
stat.error;em.opt.I;phot.mag 
zPetroMagErr 
videoSource 
VIDEOv20100513 
Error in extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
stat.error 
zPetroMagErr 
videoSource 
VIDEOv20111208 
Error in extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
stat.error 
zPetroMagErr 
vikingSource 
VIKINGDR2 
Error in extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
stat.error 
zPetroMagErr 
vikingSource 
VIKINGDR3 
Error in extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
stat.error 
zPetroMagErr 
vikingSource 
VIKINGDR4 
Error in extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
stat.error;em.opt.I 
zPetroMagErr 
vikingSource 
VIKINGv20110714 
Error in extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
stat.error 
zPetroMagErr 
vikingSource 
VIKINGv20111019 
Error in extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
stat.error 
zPetroMagErr 
vikingSource 
VIKINGv20130417 
Error in extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
stat.error 
zPetroMagErr 
vikingSource 
VIKINGv20140402 
Error in extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
stat.error 
zPetroMagErr 
vikingSource 
VIKINGv20150421 
Error in extended source Z mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
stat.error;em.opt.I;phot.mag 
zppErrBits 
svNgc253Source 
SVNGC253v20100429 
additional WFAU postprocessing error bits in Z 
int 
4 

0 
meta.code 
Postprocessing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings: Byte  Bit  Detection quality issue  Threshold or bit mask  Applies to     Decimal  Hexadecimal   0  4  Deblended  16  0x00000010  All VDFS catalogues  0  6  Bad pixel(s) in default aperture  64  0x00000040  All VDFS catalogues  0  7  Low confidence in default aperture  128  0x00000080  All VDFS catalogues  1  12  Lies within detector 16 region of a tile  4096  0x00001000  All catalogues from tiles  2  16  Close to saturated  65536  0x00010000  All VDFS catalogues  2  17  Photometric calibration probably subject to systematic error  131072  0x00020000  VVV only  2  22  Lies within a dither offset of the stacked frame boundary  4194304  0x00400000  All catalogues  2  23  Lies within the underexposed strip (or "ear") of a tile  8388608  0x00800000  All catalogues from tiles  3  24  Lies within an underexposed region of a tile due to missing detector  16777216  0x01000000  All catalogues from tiles  In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information. 
zppErrBits 
svOrionSource 
SVORIONv20100429 
additional WFAU postprocessing error bits in Z 
int 
4 

0 
meta.code 
Postprocessing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings: Byte  Bit  Detection quality issue  Threshold or bit mask  Applies to     Decimal  Hexadecimal   0  4  Deblended  16  0x00000010  All VDFS catalogues  0  6  Bad pixel(s) in default aperture  64  0x00000040  All VDFS catalogues  0  7  Low confidence in default aperture  128  0x00000080  All VDFS catalogues  1  12  Lies within detector 16 region of a tile  4096  0x00001000  All catalogues from tiles  2  16  Close to saturated  65536  0x00010000  All VDFS catalogues  2  17  Photometric calibration probably subject to systematic error  131072  0x00020000  VVV only  2  22  Lies within a dither offset of the stacked frame boundary  4194304  0x00400000  All catalogues  2  23  Lies within the underexposed strip (or "ear") of a tile  8388608  0x00800000  All catalogues from tiles  3  24  Lies within an underexposed region of a tile due to missing detector  16777216  0x01000000  All catalogues from tiles  In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information. 
zppErrBits 
ultravistaSource, ultravistaSourceRemeasurement 
ULTRAVISTAv20100429 
additional WFAU postprocessing error bits in Z 
int 
4 

0 
meta.code 
zppErrBits 
videoSource 
VIDEODR2 
additional WFAU postprocessing error bits in Z 
int 
4 

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

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

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

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

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

0 
meta.code 
Postprocessing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings: Byte  Bit  Detection quality issue  Threshold or bit mask  Applies to     Decimal  Hexadecimal   0  4  Deblended  16  0x00000010  All VDFS catalogues  0  6  Bad pixel(s) in default aperture  64  0x00000040  All VDFS catalogues  0  7  Low confidence in default aperture  128  0x00000080  All VDFS catalogues  1  12  Lies within detector 16 region of a tile  4096  0x00001000  All catalogues from tiles  2  16  Close to saturated  65536  0x00010000  All VDFS catalogues  2  17  Photometric calibration probably subject to systematic error  131072  0x00020000  VVV only  2  22  Lies within a dither offset of the stacked frame boundary  4194304  0x00400000  All catalogues  2  23  Lies within the underexposed strip (or "ear") of a tile  8388608  0x00800000  All catalogues from tiles  3  24  Lies within an underexposed region of a tile due to missing detector  16777216  0x01000000  All catalogues from tiles  In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information. 
zppErrBits 
vikingSource 
VIKINGDR3 
additional WFAU postprocessing error bits in Z 
int 
4 

0 
meta.code 
Postprocessing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings: Byte  Bit  Detection quality issue  Threshold or bit mask  Applies to     Decimal  Hexadecimal   0  4  Deblended  16  0x00000010  All VDFS catalogues  0  6  Bad pixel(s) in default aperture  64  0x00000040  All VDFS catalogues  0  7  Low confidence in default aperture  128  0x00000080  All VDFS catalogues  1  12  Lies within detector 16 region of a tile  4096  0x00001000  All catalogues from tiles  2  16  Close to saturated  65536  0x00010000  All VDFS catalogues  2  17  Photometric calibration probably subject to systematic error  131072  0x00020000  VVV only  2  22  Lies within a dither offset of the stacked frame boundary  4194304  0x00400000  All catalogues  2  23  Lies within the underexposed strip (or "ear") of a tile  8388608  0x00800000  All catalogues from tiles  3  24  Lies within an underexposed region of a tile due to missing detector  16777216  0x01000000  All catalogues from tiles  In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information. 
zppErrBits 
vikingSource 
VIKINGDR4 
additional WFAU postprocessing error bits in Z 
int 
4 

0 
meta.code;em.opt.I 
Postprocessing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings: Byte  Bit  Detection quality issue  Threshold or bit mask  Applies to     Decimal  Hexadecimal   0  4  Deblended  16  0x00000010  All VDFS catalogues  0  6  Bad pixel(s) in default aperture  64  0x00000040  All VDFS catalogues  0  7  Low confidence in default aperture  128  0x00000080  All VDFS catalogues  1  12  Lies within detector 16 region of a tile  4096  0x00001000  All catalogues from tiles  2  16  Close to saturated  65536  0x00010000  All VDFS catalogues  2  17  Photometric calibration probably subject to systematic error  131072  0x00020000  VVV only  2  22  Lies within a dither offset of the stacked frame boundary  4194304  0x00400000  All catalogues  2  23  Lies within the underexposed strip (or "ear") of a tile  8388608  0x00800000  All catalogues from tiles  3  24  Lies within an underexposed region of a tile due to missing detector  16777216  0x01000000  All catalogues from tiles  In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information. 
zppErrBits 
vikingSource 
VIKINGv20110714 
additional WFAU postprocessing error bits in Z 
int 
4 

0 
meta.code 
Postprocessing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings: Byte  Bit  Detection quality issue  Threshold or bit mask  Applies to     Decimal  Hexadecimal   0  4  Deblended  16  0x00000010  All VDFS catalogues  0  6  Bad pixel(s) in default aperture  64  0x00000040  All VDFS catalogues  0  7  Low confidence in default aperture  128  0x00000080  All VDFS catalogues  1  12  Lies within detector 16 region of a tile  4096  0x00001000  All catalogues from tiles  2  16  Close to saturated  65536  0x00010000  All VDFS catalogues  2  17  Photometric calibration probably subject to systematic error  131072  0x00020000  VVV only  2  22  Lies within a dither offset of the stacked frame boundary  4194304  0x00400000  All catalogues  2  23  Lies within the underexposed strip (or "ear") of a tile  8388608  0x00800000  All catalogues from tiles  3  24  Lies within an underexposed region of a tile due to missing detector  16777216  0x01000000  All catalogues from tiles  In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information. 
zppErrBits 
vikingSource 
VIKINGv20111019 
additional WFAU postprocessing error bits in Z 
int 
4 

0 
meta.code 
Postprocessing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings: Byte  Bit  Detection quality issue  Threshold or bit mask  Applies to     Decimal  Hexadecimal   0  4  Deblended  16  0x00000010  All VDFS catalogues  0  6  Bad pixel(s) in default aperture  64  0x00000040  All VDFS catalogues  0  7  Low confidence in default aperture  128  0x00000080  All VDFS catalogues  1  12  Lies within detector 16 region of a tile  4096  0x00001000  All catalogues from tiles  2  16  Close to saturated  65536  0x00010000  All VDFS catalogues  2  17  Photometric calibration probably subject to systematic error  131072  0x00020000  VVV only  2  22  Lies within a dither offset of the stacked frame boundary  4194304  0x00400000  All catalogues  2  23  Lies within the underexposed strip (or "ear") of a tile  8388608  0x00800000  All catalogues from tiles  3  24  Lies within an underexposed region of a tile due to missing detector  16777216  0x01000000  All catalogues from tiles  In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information. 
zppErrBits 
vikingSource 
VIKINGv20130417 
additional WFAU postprocessing error bits in Z 
int 
4 

0 
meta.code 
Postprocessing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings: Byte  Bit  Detection quality issue  Threshold or bit mask  Applies to     Decimal  Hexadecimal   0  4  Deblended  16  0x00000010  All VDFS catalogues  0  6  Bad pixel(s) in default aperture  64  0x00000040  All VDFS catalogues  0  7  Low confidence in default aperture  128  0x00000080  All VDFS catalogues  1  12  Lies within detector 16 region of a tile  4096  0x00001000  All catalogues from tiles  2  16  Close to saturated  65536  0x00010000  All VDFS catalogues  2  17  Photometric calibration probably subject to systematic error  131072  0x00020000  VVV only  2  22  Lies within a dither offset of the stacked frame boundary  4194304  0x00400000  All catalogues  2  23  Lies within the underexposed strip (or "ear") of a tile  8388608  0x00800000  All catalogues from tiles  3  24  Lies within an underexposed region of a tile due to missing detector  16777216  0x01000000  All catalogues from tiles  In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information. 
zppErrBits 
vikingSource 
VIKINGv20140402 
additional WFAU postprocessing error bits in Z 
int 
4 

0 
meta.code 
Postprocessing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings: Byte  Bit  Detection quality issue  Threshold or bit mask  Applies to     Decimal  Hexadecimal   0  4  Deblended  16  0x00000010  All VDFS catalogues  0  6  Bad pixel(s) in default aperture  64  0x00000040  All VDFS catalogues  0  7  Low confidence in default aperture  128  0x00000080  All VDFS catalogues  1  12  Lies within detector 16 region of a tile  4096  0x00001000  All catalogues from tiles  2  16  Close to saturated  65536  0x00010000  All VDFS catalogues  2  17  Photometric calibration probably subject to systematic error  131072  0x00020000  VVV only  2  22  Lies within a dither offset of the stacked frame boundary  4194304  0x00400000  All catalogues  2  23  Lies within the underexposed strip (or "ear") of a tile  8388608  0x00800000  All catalogues from tiles  3  24  Lies within an underexposed region of a tile due to missing detector  16777216  0x01000000  All catalogues from tiles  In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information. 
zppErrBits 
vikingSource 
VIKINGv20150421 
additional WFAU postprocessing error bits in Z 
int 
4 

0 
meta.code;em.opt.I 
Postprocessing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings: Byte  Bit  Detection quality issue  Threshold or bit mask  Applies to     Decimal  Hexadecimal   0  4  Deblended  16  0x00000010  All VDFS catalogues  0  6  Bad pixel(s) in default aperture  64  0x00000040  All VDFS catalogues  0  7  Low confidence in default aperture  128  0x00000080  All VDFS catalogues  1  12  Lies within detector 16 region of a tile  4096  0x00001000  All catalogues from tiles  2  16  Close to saturated  65536  0x00010000  All VDFS catalogues  2  17  Photometric calibration probably subject to systematic error  131072  0x00020000  VVV only  2  22  Lies within a dither offset of the stacked frame boundary  4194304  0x00400000  All catalogues  2  23  Lies within the underexposed strip (or "ear") of a tile  8388608  0x00800000  All catalogues from tiles  3  24  Lies within an underexposed region of a tile due to missing detector  16777216  0x01000000  All catalogues from tiles  In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information. 
zppErrBits 
vikingSourceRemeasurement 
VIKINGv20110714 
additional WFAU postprocessing error bits in Z 
int 
4 

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

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

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

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

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

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

0 
meta.code 
Postprocessing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings: Byte  Bit  Detection quality issue  Threshold or bit mask  Applies to     Decimal  Hexadecimal   0  4  Deblended  16  0x00000010  All VDFS catalogues  0  6  Bad pixel(s) in default aperture  64  0x00000040  All VDFS catalogues  0  7  Low confidence in default aperture  128  0x00000080  All VDFS catalogues  1  12  Lies within detector 16 region of a tile  4096  0x00001000  All catalogues from tiles  2  16  Close to saturated  65536  0x00010000  All VDFS catalogues  2  17  Photometric calibration probably subject to systematic error  131072  0x00020000  VVV only  2  22  Lies within a dither offset of the stacked frame boundary  4194304  0x00400000  All catalogues  2  23  Lies within the underexposed strip (or "ear") of a tile  8388608  0x00800000  All catalogues from tiles  3  24  Lies within an underexposed region of a tile due to missing detector  16777216  0x01000000  All catalogues from tiles  In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information. 
zppErrBits 
vvvSynopticSource 
VVVDR2 
additional WFAU postprocessing error bits in Z 
int 
4 

0 
meta.code 
Postprocessing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings: Byte  Bit  Detection quality issue  Threshold or bit mask  Applies to     Decimal  Hexadecimal   0  4  Deblended  16  0x00000010  All VDFS catalogues  0  6  Bad pixel(s) in default aperture  64  0x00000040  All VDFS catalogues  0  7  Low confidence in default aperture  128  0x00000080  All VDFS catalogues  1  12  Lies within detector 16 region of a tile  4096  0x00001000  All catalogues from tiles  2  16  Close to saturated  65536  0x00010000  All VDFS catalogues  2  17  Photometric calibration probably subject to systematic error  131072  0x00020000  VVV only  2  22  Lies within a dither offset of the stacked frame boundary  4194304  0x00400000  All catalogues  2  23  Lies within the underexposed strip (or "ear") of a tile  8388608  0x00800000  All catalogues from tiles  3  24  Lies within an underexposed region of a tile due to missing detector  16777216  0x01000000  All catalogues from tiles  In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information. 
zprobVar 
videoVariability 
VIDEODR2 
Probability of variable from chisquare (and other data) 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zprobVar 
videoVariability 
VIDEODR3 
Probability of variable from chisquare (and other data) 
real 
4 

0.9999995e9 
stat.probability 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zprobVar 
videoVariability 
VIDEODR4 
Probability of variable from chisquare (and other data) 
real 
4 

0.9999995e9 
stat.probability;em.opt.I 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zprobVar 
videoVariability 
VIDEOv20111208 
Probability of variable from chisquare (and other data) 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zprobVar 
vikingVariability 
VIKINGv20110714 
Probability of variable from chisquare (and other data) 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zPsfMag 
svNgc253Source 
SVNGC253v20100429 
Point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
phot.mag 
zPsfMag 
svOrionSource 
SVORIONv20100429 
Point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
phot.mag 
zPsfMag 
ultravistaSource 
ULTRAVISTAv20100429 
Not available in SE output 
real 
4 
mag 
0.9999995e9 
phot.mag 
zPsfMag 
videoSource 
VIDEOv20100513 
Not available in SE output 
real 
4 
mag 
0.9999995e9 
phot.mag 
zPsfMag 
vikingSource 
VIKINGDR2 
Point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
phot.mag 
zPsfMag 
vikingSource 
VIKINGDR3 
Point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
phot.mag 
zPsfMag 
vikingSource 
VIKINGDR4 
Point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zPsfMag 
vikingSource 
VIKINGv20110714 
Point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
phot.mag 
zPsfMag 
vikingSource 
VIKINGv20111019 
Point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
phot.mag 
zPsfMag 
vikingSource 
VIKINGv20130417 
Point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
phot.mag 
zPsfMag 
vikingSource 
VIKINGv20140402 
Point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zPsfMag 
vikingSource 
VIKINGv20150421 
Point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zPsfMagErr 
svNgc253Source 
SVNGC253v20100429 
Error in point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
stat.error 
zPsfMagErr 
svOrionSource 
SVORIONv20100429 
Error in point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
stat.error 
zPsfMagErr 
ultravistaSource 
ULTRAVISTAv20100429 
Not available in SE output 
real 
4 
mag 
0.9999995e9 
stat.error 
zPsfMagErr 
videoSource 
VIDEOv20100513 
Not available in SE output 
real 
4 
mag 
0.9999995e9 
stat.error 
zPsfMagErr 
vikingSource 
VIKINGDR2 
Error in point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
stat.error 
zPsfMagErr 
vikingSource 
VIKINGDR3 
Error in point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
stat.error 
zPsfMagErr 
vikingSource 
VIKINGDR4 
Error in point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
stat.error;em.opt.I 
zPsfMagErr 
vikingSource 
VIKINGv20110714 
Error in point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
stat.error 
zPsfMagErr 
vikingSource 
VIKINGv20111019 
Error in point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
stat.error 
zPsfMagErr 
vikingSource 
VIKINGv20130417 
Error in point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
stat.error 
zPsfMagErr 
vikingSource 
VIKINGv20140402 
Error in point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
stat.error 
zPsfMagErr 
vikingSource 
VIKINGv20150421 
Error in point source profilefitted Z mag 
real 
4 
mag 
0.9999995e9 
stat.error;em.opt.I;phot.mag 
zpSystem 
ExternalProduct 
VHSDR3 
System of zeropoint (Vega/AB) 
varchar 
16 

'NONE' 

zpSystem 
ExternalProduct 
VHSv20150108 
System of zeropoint (Vega/AB) 
varchar 
16 

'NONE' 

zpSystem 
ExternalProduct 
VIDEODR4 
System of zeropoint (Vega/AB) 
varchar 
16 

'NONE' 

zpSystem 
ExternalProduct 
VIDEOv20111208 
System of zeropoint (Vega/AB) 
varchar 
16 

'NONE' 

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

'NONE' 

zpSystem 
ExternalProduct 
VIKINGv20150421 
System of zeropoint (Vega/AB) 
varchar 
16 

'NONE' 

zpSystem 
ExternalProduct 
VMCDR3 
System of zeropoint (Vega/AB) 
varchar 
16 

'NONE' 

zpSystem 
ExternalProduct 
VMCv20140428 
System of zeropoint (Vega/AB) 
varchar 
16 

'NONE' 

zpSystem 
ExternalProduct 
VMCv20140903 
System of zeropoint (Vega/AB) 
varchar 
16 

'NONE' 

zpSystem 
ExternalProduct 
VMCv20150309 
System of zeropoint (Vega/AB) 
varchar 
16 

'NONE' 

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

'NONE' 

zSeqNum 
svNgc253Source 
SVNGC253v20100429 
the running number of the Z detection 
int 
4 

99999999 
meta.id 
zSeqNum 
svOrionSource 
SVORIONv20100429 
the running number of the Z detection 
int 
4 

99999999 
meta.id 
zSeqNum 
ultravistaSource 
ULTRAVISTAv20100429 
the running number of the Z detection 
int 
4 

99999999 
meta.id 
zSeqNum 
ultravistaSourceRemeasurement 
ULTRAVISTAv20100429 
the running number of the Z remeasurement 
int 
4 

99999999 
meta.id 
zSeqNum 
videoSource 
VIDEODR2 
the running number of the Z detection 
int 
4 

99999999 
meta.id 
zSeqNum 
videoSource 
VIDEODR3 
the running number of the Z detection 
int 
4 

99999999 
meta.number 
zSeqNum 
videoSource 
VIDEODR4 
the running number of the Z detection 
int 
4 

99999999 
meta.number;em.opt.I 
zSeqNum 
videoSource 
VIDEOv20100513 
the running number of the Z detection 
int 
4 

99999999 
meta.id 
zSeqNum 
videoSource 
VIDEOv20111208 
the running number of the Z detection 
int 
4 

99999999 
meta.id 
zSeqNum 
videoSourceRemeasurement 
VIDEOv20100513 
the running number of the Z remeasurement 
int 
4 

99999999 
meta.id 
zSeqNum 
vikingSource 
VIKINGDR2 
the running number of the Z detection 
int 
4 

99999999 
meta.id 
zSeqNum 
vikingSource 
VIKINGDR3 
the running number of the Z detection 
int 
4 

99999999 
meta.number 
zSeqNum 
vikingSource 
VIKINGDR4 
the running number of the Z detection 
int 
4 

99999999 
meta.number;em.opt.I 
zSeqNum 
vikingSource 
VIKINGv20110714 
the running number of the Z detection 
int 
4 

99999999 
meta.id 
zSeqNum 
vikingSource 
VIKINGv20111019 
the running number of the Z detection 
int 
4 

99999999 
meta.id 
zSeqNum 
vikingSource 
VIKINGv20130417 
the running number of the Z detection 
int 
4 

99999999 
meta.number 
zSeqNum 
vikingSource 
VIKINGv20140402 
the running number of the Z detection 
int 
4 

99999999 
meta.number 
zSeqNum 
vikingSource 
VIKINGv20150421 
the running number of the Z detection 
int 
4 

99999999 
meta.number;em.opt.I 
zSeqNum 
vikingSourceRemeasurement 
VIKINGv20110714 
the running number of the Z remeasurement 
int 
4 

99999999 
meta.id 
zSeqNum 
vikingSourceRemeasurement 
VIKINGv20111019 
the running number of the Z remeasurement 
int 
4 

99999999 
meta.id 
zSeqNum 
vvvSource 
VVVDR2 
the running number of the Z detection 
int 
4 

99999999 
meta.number 
zSeqNum 
vvvSource 
VVVv20100531 
the running number of the Z detection 
int 
4 

99999999 
meta.id 
zSeqNum 
vvvSource 
VVVv20110718 
the running number of the Z detection 
int 
4 

99999999 
meta.id 
zSeqNum 
vvvSource, vvvSynopticSource 
VVVDR1 
the running number of the Z detection 
int 
4 

99999999 
meta.number 
zSeqNum 
vvvSourceRemeasurement 
VVVv20100531 
the running number of the Z remeasurement 
int 
4 

99999999 
meta.id 
zSeqNum 
vvvSourceRemeasurement 
VVVv20110718 
the running number of the Z remeasurement 
int 
4 

99999999 
meta.id 
zSerMag2D 
svNgc253Source 
SVNGC253v20100429 
Extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zSerMag2D 
svOrionSource 
SVORIONv20100429 
Extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zSerMag2D 
ultravistaSource 
ULTRAVISTAv20100429 
Not available in SE output 
real 
4 
mag 
0.9999995e9 
phot.mag 
zSerMag2D 
videoSource 
VIDEOv20100513 
Not available in SE output 
real 
4 
mag 
0.9999995e9 
phot.mag 
zSerMag2D 
vikingSource 
VIKINGDR2 
Extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zSerMag2D 
vikingSource 
VIKINGDR3 
Extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zSerMag2D 
vikingSource 
VIKINGDR4 
Extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zSerMag2D 
vikingSource 
VIKINGv20110714 
Extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zSerMag2D 
vikingSource 
VIKINGv20111019 
Extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zSerMag2D 
vikingSource 
VIKINGv20130417 
Extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
phot.mag 
zSerMag2D 
vikingSource 
VIKINGv20140402 
Extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zSerMag2D 
vikingSource 
VIKINGv20150421 
Extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.I 
zSerMag2DErr 
svNgc253Source 
SVNGC253v20100429 
Error in extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
stat.error 
zSerMag2DErr 
svOrionSource 
SVORIONv20100429 
Error in extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
stat.error 
zSerMag2DErr 
ultravistaSource 
ULTRAVISTAv20100429 
Not available in SE output 
real 
4 
mag 
0.9999995e9 
stat.error 
zSerMag2DErr 
videoSource 
VIDEOv20100513 
Not available in SE output 
real 
4 
mag 
0.9999995e9 
stat.error 
zSerMag2DErr 
vikingSource 
VIKINGDR2 
Error in extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
stat.error 
zSerMag2DErr 
vikingSource 
VIKINGDR3 
Error in extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
stat.error 
zSerMag2DErr 
vikingSource 
VIKINGDR4 
Error in extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
stat.error;em.opt.I 
zSerMag2DErr 
vikingSource 
VIKINGv20110714 
Error in extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
stat.error 
zSerMag2DErr 
vikingSource 
VIKINGv20111019 
Error in extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
stat.error 
zSerMag2DErr 
vikingSource 
VIKINGv20130417 
Error in extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
stat.error 
zSerMag2DErr 
vikingSource 
VIKINGv20140402 
Error in extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
stat.error 
zSerMag2DErr 
vikingSource 
VIKINGv20150421 
Error in extended source Z mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
stat.error;em.opt.I;phot.mag 
zskewness 
videoVariability 
VIDEODR2 
Skewness in Z band (see Sesar et al. 2007) 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zskewness 
videoVariability 
VIDEODR3 
Skewness in Z band (see Sesar et al. 2007) 
real 
4 

0.9999995e9 
stat.param;em.IR.NIR 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zskewness 
videoVariability 
VIDEODR4 
Skewness in Z band (see Sesar et al. 2007) 
real 
4 
mag 
0.9999995e9 
stat.param;em.opt.I 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zskewness 
videoVariability 
VIDEOv20111208 
Skewness in Z band (see Sesar et al. 2007) 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zskewness 
vikingVariability 
VIKINGv20110714 
Skewness in Z band (see Sesar et al. 2007) 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
ZSOURCE 
mgcBrightSpec 
MGC 
Identifier for best redshift and quality 
varchar 
10 



ztotalPeriod 
videoVariability 
VIDEODR2 
total period of observations (last obsfirst obs) 
real 
4 
days 
0.9999995e9 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
ztotalPeriod 
videoVariability 
VIDEODR3 
total period of observations (last obsfirst obs) 
real 
4 
days 
0.9999995e9 
time.duration 
The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
ztotalPeriod 
videoVariability 
VIDEODR4 
total period of observations (last obsfirst obs) 
real 
4 
days 
0.9999995e9 
time.duration 
The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
ztotalPeriod 
videoVariability 
VIDEOv20111208 
total period of observations (last obsfirst obs) 
real 
4 
days 
0.9999995e9 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
ztotalPeriod 
vikingVariability 
VIKINGv20110714 
total period of observations (last obsfirst obs) 
real 
4 
days 
0.9999995e9 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
zVarClass 
videoVariability 
VIDEODR2 
Classification of variability in this band 
smallint 
2 

9999 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zVarClass 
videoVariability 
VIDEODR3 
Classification of variability in this band 
smallint 
2 

9999 
meta.code.class;src.var 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zVarClass 
videoVariability 
VIDEODR4 
Classification of variability in this band 
smallint 
2 

9999 
meta.code.class;src.var;em.opt.I 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zVarClass 
videoVariability 
VIDEOv20111208 
Classification of variability in this band 
smallint 
2 

9999 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zVarClass 
vikingVariability 
VIKINGv20110714 
Classification of variability in this band 
smallint 
2 

9999 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
zXi 
svNgc253Source 
SVNGC253v20100429 
Offset of Z detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zXi 
svOrionSource 
SVORIONv20100429 
Offset of Z detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zXi 
ultravistaSource 
ULTRAVISTAv20100429 
Offset of Z detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zXi 
videoSource 
VIDEODR2 
Offset of Z detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zXi 
videoSource 
VIDEODR3 
Offset of Z detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zXi 
videoSource 
VIDEODR4 
Offset of Z detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff;em.opt.I 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zXi 
videoSource 
VIDEOv20100513 
Offset of Z detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zXi 
videoSource 
VIDEOv20111208 
Offset of Z detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zXi 
vikingSource 
VIKINGDR2 
Offset of Z detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zXi 
vikingSource 
VIKINGDR3 
Offset of Z detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zXi 
vikingSource 
VIKINGDR4 
Offset of Z detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff;em.opt.I 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zXi 
vikingSource 
VIKINGv20110714 
Offset of Z detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zXi 
vikingSource 
VIKINGv20111019 
Offset of Z detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zXi 
vikingSource 
VIKINGv20130417 
Offset of Z detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zXi 
vikingSource 
VIKINGv20140402 
Offset of Z detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zXi 
vikingSource 
VIKINGv20150421 
Offset of Z detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff;em.opt.I 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zXi 
vvvSource 
VVVDR2 
Offset of Z detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zXi 
vvvSource 
VVVv20100531 
Offset of Z detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zXi 
vvvSource 
VVVv20110718 
Offset of Z detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
zXi 
vvvSource, vvvSynopticSource 
VVVDR1 
Offset of Z detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 