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


k_2mrat 
twomass_scn 
TWOMASS 
Ksband average 2nd image moment ratio. 
real 
4 


stat.fit.param 
k_2mrat 
twomass_sixx2_scn 
TWOMASS 
K band average 2nd image moment ratio for scan 
real 
4 



k_5sig_ba 
twomass_xsc 
TWOMASS 
K minor/major axis ratio fit to the 5sigma isophote. 
real 
4 


phys.size.axisRatio 
k_5sig_phi 
twomass_xsc 
TWOMASS 
K angle to 5sigma major axis (E of N). 
smallint 
2 
degrees 

stat.error 
k_5surf 
twomass_xsc 
TWOMASS 
K central surface brightness (r<=5). 
real 
4 
mag 

phot.mag.sb 
k_ba 
twomass_sixx2_xsc 
TWOMASS 
K minor/major axis ratio fit to the 3sigma isophote 
real 
4 



k_ba 
twomass_xsc 
TWOMASS 
K minor/major axis ratio fit to the 3sigma isophote. 
real 
4 


phys.size.axisRatio 
k_back 
twomass_xsc 
TWOMASS 
K coadd median background. 
real 
4 


meta.code 
k_bisym_chi 
twomass_xsc 
TWOMASS 
K bisymmetric crosscorrelation chi. 
real 
4 


stat.fit.param 
k_bisym_rat 
twomass_xsc 
TWOMASS 
K bisymmetric flux ratio. 
real 
4 


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

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

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


stat.fit.param 
k_cmsig 
twomass_psc 
TWOMASS 
Corrected photometric uncertainty for the default Ksband magnitude. 
real 
4 
mag 
Ksband 
phot.flux 
k_con_indx 
twomass_xsc 
TWOMASS 
K concentration index r_75%/r_25%. 
real 
4 


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


stat.fit.residual 
k_flg_10 
twomass_xsc 
TWOMASS 
K confusion flag for 10 arcsec circular ap. mag. 
smallint 
2 


meta.code 
k_flg_15 
twomass_xsc 
TWOMASS 
K confusion flag for 15 arcsec circular ap. mag. 
smallint 
2 


meta.code 
k_flg_20 
twomass_xsc 
TWOMASS 
K confusion flag for 20 arcsec circular ap. mag. 
smallint 
2 


meta.code 
k_flg_25 
twomass_xsc 
TWOMASS 
K confusion flag for 25 arcsec circular ap. mag. 
smallint 
2 


meta.code 
k_flg_30 
twomass_xsc 
TWOMASS 
K confusion flag for 30 arcsec circular ap. mag. 
smallint 
2 


meta.code 
k_flg_40 
twomass_xsc 
TWOMASS 
K confusion flag for 40 arcsec circular ap. mag. 
smallint 
2 


meta.code 
k_flg_5 
twomass_xsc 
TWOMASS 
K confusion flag for 5 arcsec circular ap. mag. 
smallint 
2 


meta.code 
k_flg_50 
twomass_xsc 
TWOMASS 
K confusion flag for 50 arcsec circular ap. mag. 
smallint 
2 


meta.code 
k_flg_60 
twomass_xsc 
TWOMASS 
K confusion flag for 60 arcsec circular ap. mag. 
smallint 
2 


meta.code 
k_flg_7 
twomass_sixx2_xsc 
TWOMASS 
K confusion flag for 7 arcsec circular ap. mag 
smallint 
2 



k_flg_7 
twomass_xsc 
TWOMASS 
K confusion flag for 7 arcsec circular ap. mag. 
smallint 
2 


meta.code 
k_flg_70 
twomass_xsc 
TWOMASS 
K confusion flag for 70 arcsec circular ap. mag. 
smallint 
2 


meta.code 
k_flg_c 
twomass_xsc 
TWOMASS 
K confusion flag for Kron circular mag. 
smallint 
2 


meta.code 
k_flg_e 
twomass_xsc 
TWOMASS 
K confusion flag for Kron elliptical mag. 
smallint 
2 


meta.code 
k_flg_fc 
twomass_xsc 
TWOMASS 
K confusion flag for fiducial Kron circ. mag. 
smallint 
2 


meta.code 
k_flg_fe 
twomass_xsc 
TWOMASS 
K confusion flag for fiducial Kron ell. mag. 
smallint 
2 


meta.code 
k_flg_i20c 
twomass_xsc 
TWOMASS 
K confusion flag for 20mag/sq." iso. circ. mag. 
smallint 
2 


meta.code 
k_flg_i20e 
twomass_xsc 
TWOMASS 
K confusion flag for 20mag/sq." iso. ell. mag. 
smallint 
2 


meta.code 
k_flg_i21c 
twomass_xsc 
TWOMASS 
K confusion flag for 21mag/sq." iso. circ. mag. 
smallint 
2 


meta.code 
k_flg_i21e 
twomass_xsc 
TWOMASS 
K confusion flag for 21mag/sq." iso. ell. mag. 
smallint 
2 


meta.code 
k_flg_j21fc 
twomass_xsc 
TWOMASS 
K confusion flag for 21mag/sq." iso. fid. circ. mag. 
smallint 
2 


meta.code 
k_flg_j21fe 
twomass_xsc 
TWOMASS 
K confusion flag for 21mag/sq." iso. fid. ell. mag. 
smallint 
2 


meta.code 
k_flg_k20fc 
twomass_xsc 
TWOMASS 
K confusion flag for 20mag/sq." iso. fid. circ. mag. 
smallint 
2 


meta.code 
k_flg_k20fe 
twomass_sixx2_xsc 
TWOMASS 
K confusion flag for 20mag/sq.″ iso. fid. ell. mag 
smallint 
2 



k_flg_k20fe 
twomass_xsc 
TWOMASS 
K confusion flag for 20mag/sq." iso. fid. ell. mag. 
smallint 
2 


meta.code 
k_m 
twomass_psc 
TWOMASS 
Default Ksband magnitude 
real 
4 
mag 

phot.flux 
k_m 
twomass_sixx2_psc 
TWOMASS 
K selected "default" magnitude 
real 
4 
mag 


k_m_10 
twomass_xsc 
TWOMASS 
K 10 arcsec radius circular aperture magnitude. 
real 
4 
mag 

phot.flux 
k_m_15 
twomass_xsc 
TWOMASS 
K 15 arcsec radius circular aperture magnitude. 
real 
4 
mag 

phot.flux 
k_m_20 
twomass_xsc 
TWOMASS 
K 20 arcsec radius circular aperture magnitude. 
real 
4 
mag 

phot.flux 
k_m_25 
twomass_xsc 
TWOMASS 
K 25 arcsec radius circular aperture magnitude. 
real 
4 
mag 

phot.flux 
k_m_2mass 
allwise_sc2 
WISE 
2MASS K_{s}band magnitude of the associated 2MASS PSC source. This column is "null" if there is no associated 2MASS PSC source or if the 2MASS PSC K_{s}band magnitude entry is "null". 
float 
8 
mag 


k_m_30 
twomass_xsc 
TWOMASS 
K 30 arcsec radius circular aperture magnitude. 
real 
4 
mag 

phot.flux 
k_m_40 
twomass_xsc 
TWOMASS 
K 40 arcsec radius circular aperture magnitude. 
real 
4 
mag 

phot.flux 
k_m_5 
twomass_xsc 
TWOMASS 
K 5 arcsec radius circular aperture magnitude. 
real 
4 
mag 

phot.flux 
k_m_50 
twomass_xsc 
TWOMASS 
K 50 arcsec radius circular aperture magnitude. 
real 
4 
mag 

phot.flux 
k_m_60 
twomass_xsc 
TWOMASS 
K 60 arcsec radius circular aperture magnitude. 
real 
4 
mag 

phot.flux 
k_m_7 
twomass_sixx2_xsc 
TWOMASS 
K 7 arcsec radius circular aperture magnitude 
real 
4 
mag 


k_m_7 
twomass_xsc 
TWOMASS 
K 7 arcsec radius circular aperture magnitude. 
real 
4 
mag 

phot.flux 
k_m_70 
twomass_xsc 
TWOMASS 
K 70 arcsec radius circular aperture magnitude. 
real 
4 
mag 

phot.flux 
k_m_c 
twomass_xsc 
TWOMASS 
K Kron circular aperture magnitude. 
real 
4 
mag 

phot.flux 
k_m_e 
twomass_xsc 
TWOMASS 
K Kron elliptical aperture magnitude. 
real 
4 
mag 

phot.flux 
k_m_ext 
twomass_sixx2_xsc 
TWOMASS 
K mag from fit extrapolation 
real 
4 
mag 


k_m_ext 
twomass_xsc 
TWOMASS 
K mag from fit extrapolation. 
real 
4 
mag 

phot.flux 
k_m_fc 
twomass_xsc 
TWOMASS 
K fiducial Kron circular magnitude. 
real 
4 
mag 

phot.flux 
k_m_fe 
twomass_xsc 
TWOMASS 
K fiducial Kron ell. mag aperture magnitude. 
real 
4 
mag 

phot.flux 
k_m_i20c 
twomass_xsc 
TWOMASS 
K 20mag/sq." isophotal circular ap. magnitude. 
real 
4 
mag 

phot.flux 
k_m_i20e 
twomass_xsc 
TWOMASS 
K 20mag/sq." isophotal elliptical ap. magnitude. 
real 
4 
mag 

phot.flux 
k_m_i21c 
twomass_xsc 
TWOMASS 
K 21mag/sq." isophotal circular ap. magnitude. 
real 
4 
mag 

phot.flux 
k_m_i21e 
twomass_xsc 
TWOMASS 
K 21mag/sq." isophotal elliptical ap. magnitude. 
real 
4 
mag 

phot.flux 
k_m_j21fc 
twomass_xsc 
TWOMASS 
K 21mag/sq." isophotal fiducial circ. ap. mag. 
real 
4 
mag 

phot.flux 
k_m_j21fe 
twomass_xsc 
TWOMASS 
K 21mag/sq." isophotal fiducial ell. ap. magnitude. 
real 
4 
mag 

phot.flux 
k_m_k20fc 
twomass_xsc 
TWOMASS 
K 20mag/sq." isophotal fiducial circ. ap. mag. 
real 
4 
mag 

phot.flux 
K_M_K20FE 
twomass 
SIXDF 
K 20mag/sq." isophotal fiducial ell. ap. magnitude 
real 
4 
mag 


k_m_k20fe 
twomass_sixx2_xsc 
TWOMASS 
K 20mag/sq.″ isophotal fiducial ell. ap. magnitude 
real 
4 
mag 


k_m_k20fe 
twomass_xsc 
TWOMASS 
K 20mag/sq." isophotal fiducial ell. ap. magnitude. 
real 
4 
mag 

phot.flux 
k_m_stdap 
twomass_psc 
TWOMASS 
Ksband "standard" aperture magnitude. 
real 
4 
mag 

phot.flux 
k_m_sys 
twomass_xsc 
TWOMASS 
K system photometry magnitude. 
real 
4 
mag 

phot.flux 
k_mnsurfb_eff 
twomass_xsc 
TWOMASS 
K mean surface brightness at the halflight radius. 
real 
4 
mag 

phot.mag.sb 
k_msig 
twomass_sixx2_psc 
TWOMASS 
K "default" mag uncertainty 
real 
4 
mag 


k_msig_10 
twomass_xsc 
TWOMASS 
K 1sigma uncertainty in 10 arcsec circular ap. mag. 
real 
4 
mag 

stat.error 
k_msig_15 
twomass_xsc 
TWOMASS 
K 1sigma uncertainty in 15 arcsec circular ap. mag. 
real 
4 
mag 

stat.error 
k_msig_20 
twomass_xsc 
TWOMASS 
K 1sigma uncertainty in 20 arcsec circular ap. mag. 
real 
4 
mag 

stat.error 
k_msig_25 
twomass_xsc 
TWOMASS 
K 1sigma uncertainty in 25 arcsec circular ap. mag. 
real 
4 
mag 

stat.error 
k_msig_2mass 
allwise_sc2 
WISE 
2MASS K_{s}band corrected photometric uncertainty of the associated 2MASS PSC source. This column is "null" if there is no associated 2MASS PSC source or if the 2MASS PSC K_{s}band uncertainty entry is "null". 
float 
8 
mag 


k_msig_30 
twomass_xsc 
TWOMASS 
K 1sigma uncertainty in 30 arcsec circular ap. mag. 
real 
4 
mag 

stat.error 
k_msig_40 
twomass_xsc 
TWOMASS 
K 1sigma uncertainty in 40 arcsec circular ap. mag. 
real 
4 
mag 

stat.error 
k_msig_5 
twomass_xsc 
TWOMASS 
K 1sigma uncertainty in 5 arcsec circular ap. mag. 
real 
4 
mag 

stat.error 
k_msig_50 
twomass_xsc 
TWOMASS 
K 1sigma uncertainty in 50 arcsec circular ap. mag. 
real 
4 
mag 

stat.error 
k_msig_60 
twomass_xsc 
TWOMASS 
K 1sigma uncertainty in 60 arcsec circular ap. mag. 
real 
4 
mag 

stat.error 
k_msig_7 
twomass_sixx2_xsc 
TWOMASS 
K 1sigma uncertainty in 7 arcsec circular ap. mag 
real 
4 
mag 


k_msig_7 
twomass_xsc 
TWOMASS 
K 1sigma uncertainty in 7 arcsec circular ap. mag. 
real 
4 
mag 

stat.error 
k_msig_70 
twomass_xsc 
TWOMASS 
K 1sigma uncertainty in 70 arcsec circular ap. mag. 
real 
4 
mag 

stat.error 
k_msig_c 
twomass_xsc 
TWOMASS 
K 1sigma uncertainty in Kron circular mag. 
real 
4 
mag 

stat.error 
k_msig_e 
twomass_xsc 
TWOMASS 
K 1sigma uncertainty in Kron elliptical mag. 
real 
4 
mag 

stat.error 
k_msig_ext 
twomass_sixx2_xsc 
TWOMASS 
K 1sigma uncertainty in mag from fit extrapolation 
real 
4 
mag 


k_msig_ext 
twomass_xsc 
TWOMASS 
K 1sigma uncertainty in mag from fit extrapolation. 
real 
4 
mag 

stat.error 
k_msig_fc 
twomass_xsc 
TWOMASS 
K 1sigma uncertainty in fiducial Kron circ. mag. 
real 
4 
mag 

stat.error 
k_msig_fe 
twomass_xsc 
TWOMASS 
K 1sigma uncertainty in fiducial Kron ell. mag. 
real 
4 
mag 

stat.error 
k_msig_i20c 
twomass_xsc 
TWOMASS 
K 1sigma uncertainty in 20mag/sq." iso. circ. mag. 
real 
4 
mag 

stat.error 
k_msig_i20e 
twomass_xsc 
TWOMASS 
K 1sigma uncertainty in 20mag/sq." iso. ell. mag. 
real 
4 
mag 

stat.error 
k_msig_i21c 
twomass_xsc 
TWOMASS 
K 1sigma uncertainty in 21mag/sq." iso. circ. mag. 
real 
4 
mag 

stat.error 
k_msig_i21e 
twomass_xsc 
TWOMASS 
K 1sigma uncertainty in 21mag/sq." iso. ell. mag. 
real 
4 
mag 

stat.error 
k_msig_j21fc 
twomass_xsc 
TWOMASS 
K 1sigma uncertainty in 21mag/sq." iso.fid.circ.mag. 
real 
4 
mag 

stat.error 
k_msig_j21fe 
twomass_xsc 
TWOMASS 
K 1sigma uncertainty in 21mag/sq." iso.fid.ell.mag. 
real 
4 
mag 

stat.error 
k_msig_k20fc 
twomass_xsc 
TWOMASS 
K 1sigma uncertainty in 20mag/sq." iso.fid.circ. mag. 
real 
4 
mag 

stat.error 
k_msig_k20fe 
twomass_sixx2_xsc 
TWOMASS 
K 1sigma uncertainty in 20mag/sq.″ iso.fid.ell.mag 
real 
4 
mag 


k_msig_k20fe 
twomass_xsc 
TWOMASS 
K 1sigma uncertainty in 20mag/sq." iso.fid.ell.mag. 
real 
4 
mag 

stat.error 
k_msig_stdap 
twomass_psc 
TWOMASS 
Uncertainty in the Ksband standard aperture magnitude. 
real 
4 
mag 

phot.flux 
k_msig_sys 
twomass_xsc 
TWOMASS 
K 1sigma uncertainty in system photometry mag. 
real 
4 
mag 

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


k_msnr10 
twomass_scn 
TWOMASS 
The estimated Ksband magnitude at which SNR=10 is achieved for this scan. 
real 
4 
mag 

phot.flux 
k_msnr10 
twomass_sixx2_scn 
TWOMASS 
K mag at which SNR=10 is achieved, from k_psp and k_zp_ap 
real 
4 
mag 


k_n_snr10 
twomass_scn 
TWOMASS 
Number of point sources at Ksband with SNR>10 (instrumental mag <=14.3) 
int 
4 


meta.number 
k_n_snr10 
twomass_sixx2_scn 
TWOMASS 
number of K point sources with SNR>10 (instrumental m<=14.3) 
int 
4 



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


stat.fit.param 
k_peak 
twomass_xsc 
TWOMASS 
K peak pixel brightness. 
real 
4 
mag 

phot.mag.sb 
k_perc_darea 
twomass_xsc 
TWOMASS 
K 5sigma to 3sigma percent area change. 
smallint 
2 


FIT_PARAM 
k_phi 
twomass_sixx2_xsc 
TWOMASS 
K angle to 3sigma major axis (E of N) 
smallint 
2 
deg 


k_phi 
twomass_xsc 
TWOMASS 
K angle to 3sigma major axis (E of N). 
smallint 
2 
degrees 

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


stat.fit.param 
k_psp 
twomass_scn 
TWOMASS 
Ksband photometric sensitivity paramater (PSP). 
real 
4 


instr.sensitivity 
k_psp 
twomass_sixx2_scn 
TWOMASS 
K photometric sensitivity param: k_shape_avg*(k_fbg_avg^.29) 
real 
4 



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


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


k_r_c 
twomass_xsc 
TWOMASS 
K Kron circular aperture radius. 
real 
4 
arcsec 

phys.angSize;src 
k_r_e 
twomass_xsc 
TWOMASS 
K Kron elliptical aperture semimajor axis. 
real 
4 
arcsec 

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

phys.angSize;src 
k_r_i20c 
twomass_xsc 
TWOMASS 
K 20mag/sq." isophotal circular aperture radius. 
real 
4 
arcsec 

phys.angSize;src 
k_r_i20e 
twomass_xsc 
TWOMASS 
K 20mag/sq." isophotal elliptical ap. semimajor axis. 
real 
4 
arcsec 

phys.angSize;src 
k_r_i21c 
twomass_xsc 
TWOMASS 
K 21mag/sq." isophotal circular aperture radius. 
real 
4 
arcsec 

phys.angSize;src 
k_r_i21e 
twomass_xsc 
TWOMASS 
K 21mag/sq." isophotal elliptical ap. semimajor axis. 
real 
4 
arcsec 

phys.angSize;src 
k_resid_ann 
twomass_xsc 
TWOMASS 
K residual annulus background median. 
real 
4 
DN 

meta.code 
k_sc_1mm 
twomass_xsc 
TWOMASS 
K 1st moment (score) (LCSB: super blk 2,4,8 SNR). 
real 
4 


meta.code 
k_sc_2mm 
twomass_xsc 
TWOMASS 
K 2nd moment (score) (LCSB: SNRMAX  super SNR max). 
real 
4 


meta.code 
k_sc_msh 
twomass_xsc 
TWOMASS 
K median shape score. 
real 
4 


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


meta.code 
k_sc_r1 
twomass_xsc 
TWOMASS 
K r1 (score). 
real 
4 


meta.code 
k_sc_r23 
twomass_xsc 
TWOMASS 
K r23 (score) (LCSB: TSNR  integrated SNR for r=15). 
real 
4 


meta.code 
k_sc_sh 
twomass_xsc 
TWOMASS 
K shape (score). 
real 
4 


meta.code 
k_sc_vint 
twomass_xsc 
TWOMASS 
K vint (score). 
real 
4 


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


meta.code 
k_seetrack 
twomass_xsc 
TWOMASS 
K band seetracking score. 
real 
4 


meta.code 
k_sh0 
twomass_xsc 
TWOMASS 
K ridge shape (LCSB: BSNR limit). 
real 
4 


FIT_PARAM 
k_shape_avg 
twomass_scn 
TWOMASS 
Ksband average seeing shape for scan. 
real 
4 


instr.obsty.seeing 
k_shape_avg 
twomass_sixx2_scn 
TWOMASS 
K band average seeing shape for scan 
real 
4 



k_shape_rms 
twomass_scn 
TWOMASS 
RMSerror of Ksband average seeing shape. 
real 
4 


instr.obsty.seeing 
k_shape_rms 
twomass_sixx2_scn 
TWOMASS 
rms of K band avg seeing shape for scan 
real 
4 



k_sig_sh0 
twomass_xsc 
TWOMASS 
K ridge shape sigma (LCSB: B2SNR limit). 
real 
4 


FIT_PARAM 
k_snr 
twomass_psc 
TWOMASS 
Ksband "scan" signaltonoise ratio. 
real 
4 
mag 

instr.det.noise 
k_snr 
twomass_sixx2_psc 
TWOMASS 
K band "scan" signaltonoise ratio 
real 
4 



k_subst2 
twomass_xsc 
TWOMASS 
K residual background #2 (score). 
real 
4 


meta.code 
k_zp_ap 
twomass_scn 
TWOMASS 
Photometric zeropoint for Ksband aperture photometry. 
real 
4 
mag 

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


k_zperr_ap 
twomass_scn 
TWOMASS 
RMSerror of zeropoint for Ksband aperture photometry 
real 
4 
mag 

stat.error 
k_zperr_ap 
twomass_sixx2_scn 
TWOMASS 
K band ap. calibration rms error of zeropoint for scan 
real 
4 
mag 


KBESTR 
spectra 
SIXDF 
crosscorrelation template 
int 
4 



kCorr 
twompzPhotoz 
TWOMPZ 
K 20mag/sq." isophotal fiducial ell. ap. magnitude with Galactic dust correction {image primary HDU keyword: Kcorr} 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
kCorrErr 
twompzPhotoz 
TWOMPZ 
K 1sigma uncertainty in 20mag/sq." aperture {image primary HDU keyword: k_msig_k20fe} 
real 
4 
mag 
0.9999995e9 

KEXT 
twomass 
SIXDF 
KEXT magnitude 
real 
4 
mag 


KEXT_K 
twomass 
SIXDF 
KEXT minus K (corrected) 
real 
4 
mag 


Kmag 
mcps_lmcSource, mcps_smcSource 
MCPS 
The K' band magnitude (from 2MASS) (0.00 if star not detected.) 
real 
4 
mag 


kMag 
ukirtFSstars 
VIDEOv20100513 
K band total magnitude on the MKO(UFTI) system 
real 
4 
mag 

phot.mag 
kMag 
ukirtFSstars 
VIKINGv20110714 
K band total magnitude on the MKO(UFTI) system 
real 
4 
mag 

phot.mag 
Kmag2MASS 
spitzer_smcSource 
SPITZER 
The 2MASS K band magnitude. 
real 
4 
mag 


Kmag_2MASS 
ravedr5Source 
RAVE 
K selected default magnitude from 2MASS 
real 
4 
mag 
magnitude 
phot.mag;em.IR.K 
Kmag_DENIS 
ravedr5Source 
RAVE 
K selected default magnitude 
real 
4 
mag 
magnitude 
phot.mag;em.IR.K 
kMagErr 
ukirtFSstars 
VIDEOv20100513 
K band magnitude error 
real 
4 
mag 

stat.error 
kMagErr 
ukirtFSstars 
VIKINGv20110714 
K band magnitude error 
real 
4 
mag 

stat.error 
kronFlux 
vhsDetection 
VHSDR2 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count;em.opt 
kronFlux 
vhsDetection 
VHSDR3 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vhsDetection 
VHSDR4 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vhsDetection 
VHSv20120926 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vhsDetection 
VHSv20130417 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vhsDetection 
VHSv20140409 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vhsDetection 
VHSv20150108 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vhsDetection 
VHSv20160114 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vhsDetection 
VHSv20160507 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vhsDetection 
VHSv20170630 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vhsDetection 
VHSv20171207 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vhsDetection 
VHSv20180419 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vhsDetection, vhsListRemeasurement 
VHSDR1 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count;em.opt 
kronFlux 
videoDetection 
VIDEODR2 
flux within Kron radius circular aperture (SE: FLUX_AUTO) {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count;em.opt 
kronFlux 
videoDetection 
VIDEODR3 
flux within Kron radius circular aperture (SE: FLUX_AUTO) {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
videoDetection 
VIDEODR4 
flux within Kron radius circular aperture (SE: FLUX_AUTO) {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
videoDetection 
VIDEODR5 
flux within Kron radius circular aperture (SE: FLUX_AUTO) {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
videoDetection 
VIDEOv20100513 
flux within Kron radius circular aperture (SE: FLUX_AUTO) {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count;em.opt 
kronFlux 
videoDetection 
VIDEOv20111208 
flux within Kron radius circular aperture (SE: FLUX_AUTO) {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count;em.opt 
kronFlux 
videoListRemeasurement 
VIDEOv20100513 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count;em.opt 
kronFlux 
vikingDetection 
VIKINGDR2 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count;em.opt 
kronFlux 
vikingDetection 
VIKINGDR3 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vikingDetection 
VIKINGDR4 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vikingDetection 
VIKINGv20111019 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count;em.opt 
kronFlux 
vikingDetection 
VIKINGv20130417 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vikingDetection 
VIKINGv20140402 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vikingDetection 
VIKINGv20150421 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vikingDetection 
VIKINGv20151230 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vikingDetection 
VIKINGv20160406 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vikingDetection 
VIKINGv20161202 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vikingDetection 
VIKINGv20170715 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vikingDetection 
VIKINGv20181012 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vikingDetection, vikingListRemeasurement 
VIKINGv20110714 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count;em.opt 
kronFlux 
vikingMapRemeasurement 
VIKINGZYSELJv20160909 
flux within Kron radius circular aperture (SE: FLUX_AUTO; CASU: default) {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count;em.opt 
kronFlux 
vikingMapRemeasurement 
VIKINGZYSELJv20170124 
flux within Kron radius circular aperture (SE: FLUX_AUTO; CASU: default) {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count;em.opt 
kronFlux 
vmcDetection 
VMCDR1 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count;em.opt 
kronFlux 
vmcDetection 
VMCDR2 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vmcDetection 
VMCDR3 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vmcDetection 
VMCDR4 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vmcDetection 
VMCv20110909 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count;em.opt 
kronFlux 
vmcDetection 
VMCv20120126 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count;em.opt 
kronFlux 
vmcDetection 
VMCv20121128 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vmcDetection 
VMCv20130304 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vmcDetection 
VMCv20130805 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vmcDetection 
VMCv20140428 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vmcDetection 
VMCv20140903 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vmcDetection 
VMCv20150309 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vmcDetection 
VMCv20151218 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vmcDetection 
VMCv20160311 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vmcDetection 
VMCv20160822 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vmcDetection 
VMCv20170109 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vmcDetection 
VMCv20170411 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vmcDetection 
VMCv20171101 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vmcDetection 
VMCv20180702 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vmcDetection 
VMCv20181120 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFlux 
vmcDetection, vmcListRemeasurement 
VMCv20110816 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count;em.opt 
kronFlux 
vvvDetection 
VVVDR4 
flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} 
real 
4 
ADU 

phot.count 
kronFluxErr 
vhsDetection 
VHSDR2 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vhsDetection 
VHSDR3 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vhsDetection 
VHSDR4 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vhsDetection 
VHSv20120926 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vhsDetection 
VHSv20130417 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vhsDetection 
VHSv20140409 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vhsDetection 
VHSv20150108 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vhsDetection 
VHSv20160114 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vhsDetection 
VHSv20160507 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vhsDetection 
VHSv20170630 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vhsDetection 
VHSv20171207 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vhsDetection 
VHSv20180419 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vhsDetection, vhsListRemeasurement 
VHSDR1 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
videoDetection 
VIDEODR2 
error on Kron flux (SE: FLUXERR_AUTO) {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
videoDetection 
VIDEODR3 
error on Kron flux (SE: FLUXERR_AUTO) {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
videoDetection 
VIDEODR4 
error on Kron flux (SE: FLUXERR_AUTO) {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
videoDetection 
VIDEODR5 
error on Kron flux (SE: FLUXERR_AUTO) {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
videoDetection 
VIDEOv20100513 
error on Kron flux (SE: FLUXERR_AUTO) {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
videoDetection 
VIDEOv20111208 
error on Kron flux (SE: FLUXERR_AUTO) {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
videoListRemeasurement 
VIDEOv20100513 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vikingDetection 
VIKINGDR2 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vikingDetection 
VIKINGDR3 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vikingDetection 
VIKINGDR4 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vikingDetection 
VIKINGv20111019 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vikingDetection 
VIKINGv20130417 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vikingDetection 
VIKINGv20140402 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vikingDetection 
VIKINGv20150421 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vikingDetection 
VIKINGv20151230 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vikingDetection 
VIKINGv20160406 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vikingDetection 
VIKINGv20161202 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vikingDetection 
VIKINGv20170715 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vikingDetection 
VIKINGv20181012 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vikingDetection, vikingListRemeasurement 
VIKINGv20110714 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vikingMapRemeasurement 
VIKINGZYSELJv20160909 
error on Kron flux (SE: FLUXERR_AUTO; CASU: default) {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vikingMapRemeasurement 
VIKINGZYSELJv20170124 
error on Kron flux (SE: FLUXERR_AUTO; CASU: default) {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vmcDetection 
VMCDR1 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vmcDetection 
VMCDR2 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vmcDetection 
VMCDR3 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vmcDetection 
VMCDR4 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vmcDetection 
VMCv20110909 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vmcDetection 
VMCv20120126 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vmcDetection 
VMCv20121128 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vmcDetection 
VMCv20130304 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vmcDetection 
VMCv20130805 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vmcDetection 
VMCv20140428 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vmcDetection 
VMCv20140903 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vmcDetection 
VMCv20150309 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vmcDetection 
VMCv20151218 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vmcDetection 
VMCv20160311 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vmcDetection 
VMCv20160822 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vmcDetection 
VMCv20170109 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vmcDetection 
VMCv20170411 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vmcDetection 
VMCv20171101 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vmcDetection 
VMCv20180702 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vmcDetection 
VMCv20181120 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vmcDetection, vmcListRemeasurement 
VMCv20110816 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronFluxErr 
vvvDetection 
VVVDR4 
error on Kron flux {catalogue TType keyword: Kron_flux_err} 
real 
4 
ADU 

stat.error 
kronJky 
vikingMapRemeasurement 
VIKINGZYSELJv20160909 
Calibrated Kron flux within aperture r_k (CASU: default) 
real 
4 
jansky 

phot.mag 
kronJky 
vikingMapRemeasurement 
VIKINGZYSELJv20170124 
Calibrated Kron flux within aperture r_k (CASU: default) 
real 
4 
jansky 

phot.mag 
kronJkyErr 
vikingMapRemeasurement 
VIKINGZYSELJv20160909 
error on calibrated Kron flux 
real 
4 
jansky (CASU: default) 

stat.error 
kronJkyErr 
vikingMapRemeasurement 
VIKINGZYSELJv20170124 
error on calibrated Kron flux 
real 
4 
jansky (CASU: default) 

stat.error 
kronLup 
vikingMapRemeasurement 
VIKINGZYSELJv20160909 
Calibrated Kron luptitude within aperture r_k (CASU: default) 
real 
4 
lup 

phot.mag 
kronLup 
vikingMapRemeasurement 
VIKINGZYSELJv20170124 
Calibrated Kron luptitude within aperture r_k (CASU: default) 
real 
4 
lup 

phot.mag 
kronLupErr 
vikingMapRemeasurement 
VIKINGZYSELJv20160909 
error on calibrated Kron luptitude 
real 
4 
lup (CASU: default) 

stat.error 
kronLupErr 
vikingMapRemeasurement 
VIKINGZYSELJv20170124 
error on calibrated Kron luptitude 
real 
4 
lup (CASU: default) 

stat.error 
kronMag 
vhsDetection 
VHSDR2 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vhsDetection 
VHSDR3 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vhsDetection 
VHSDR4 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vhsDetection 
VHSv20120926 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vhsDetection 
VHSv20130417 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vhsDetection 
VHSv20140409 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vhsDetection 
VHSv20150108 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vhsDetection 
VHSv20160114 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vhsDetection 
VHSv20160507 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vhsDetection 
VHSv20170630 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vhsDetection 
VHSv20171207 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vhsDetection 
VHSv20180419 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vhsDetection, vhsListRemeasurement 
VHSDR1 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
videoDetection 
VIDEODR2 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
videoDetection 
VIDEODR3 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
videoDetection 
VIDEODR4 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
videoDetection 
VIDEODR5 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
videoDetection 
VIDEOv20111208 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
videoDetection, videoListRemeasurement 
VIDEOv20100513 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vikingDetection 
VIKINGDR2 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vikingDetection 
VIKINGDR3 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vikingDetection 
VIKINGDR4 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vikingDetection 
VIKINGv20111019 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vikingDetection 
VIKINGv20130417 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vikingDetection 
VIKINGv20140402 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vikingDetection 
VIKINGv20150421 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vikingDetection 
VIKINGv20151230 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vikingDetection 
VIKINGv20160406 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vikingDetection 
VIKINGv20161202 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vikingDetection 
VIKINGv20170715 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vikingDetection 
VIKINGv20181012 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vikingDetection, vikingListRemeasurement 
VIKINGv20110714 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vikingMapRemeasurement 
VIKINGZYSELJv20160909 
Calibrated Kron magnitude within aperture r_k (CASU: default) 
real 
4 
mag 

phot.mag 
kronMag 
vikingMapRemeasurement 
VIKINGZYSELJv20170124 
Calibrated Kron magnitude within aperture r_k (CASU: default) 
real 
4 
mag 

phot.mag 
kronMag 
vmcDetection 
VMCDR1 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vmcDetection 
VMCDR2 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vmcDetection 
VMCDR3 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vmcDetection 
VMCDR4 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vmcDetection 
VMCv20110909 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vmcDetection 
VMCv20120126 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vmcDetection 
VMCv20121128 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vmcDetection 
VMCv20130304 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vmcDetection 
VMCv20130805 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vmcDetection 
VMCv20140428 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vmcDetection 
VMCv20140903 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vmcDetection 
VMCv20150309 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vmcDetection 
VMCv20151218 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vmcDetection 
VMCv20160311 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vmcDetection 
VMCv20160822 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vmcDetection 
VMCv20170109 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vmcDetection 
VMCv20170411 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vmcDetection 
VMCv20171101 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vmcDetection 
VMCv20180702 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vmcDetection 
VMCv20181120 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vmcDetection, vmcListRemeasurement 
VMCv20110816 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMag 
vvvDetection 
VVVDR4 
Calibrated Kron magnitude within circular aperture r_k 
real 
4 
mag 

phot.mag 
kronMagErr 
vhsDetection 
VHSDR2 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error 
kronMagErr 
vhsDetection 
VHSDR3 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error 
kronMagErr 
vhsDetection 
VHSDR4 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error;phot.mag 
kronMagErr 
vhsDetection 
VHSv20120926 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error 
kronMagErr 
vhsDetection 
VHSv20130417 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error 
kronMagErr 
vhsDetection 
VHSv20140409 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error 
kronMagErr 
vhsDetection 
VHSv20150108 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error;phot.mag 
kronMagErr 
vhsDetection 
VHSv20160114 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error;phot.mag 
kronMagErr 
vhsDetection 
VHSv20160507 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error;phot.mag 
kronMagErr 
vhsDetection 
VHSv20170630 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error;phot.mag 
kronMagErr 
vhsDetection 
VHSv20171207 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error;phot.mag 
kronMagErr 
vhsDetection 
VHSv20180419 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error;phot.mag 
kronMagErr 
vhsDetection, vhsListRemeasurement 
VHSDR1 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error 
kronMagErr 
videoDetection 
VIDEODR2 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error 
kronMagErr 
videoDetection 
VIDEODR3 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error 
kronMagErr 
videoDetection 
VIDEODR4 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error;phot.mag 
kronMagErr 
videoDetection 
VIDEODR5 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error;phot.mag 
kronMagErr 
videoDetection 
VIDEOv20111208 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error 
kronMagErr 
videoDetection, videoListRemeasurement 
VIDEOv20100513 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error 
kronMagErr 
vikingDetection 
VIKINGDR2 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error 
kronMagErr 
vikingDetection 
VIKINGDR3 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error 
kronMagErr 
vikingDetection 
VIKINGDR4 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error 
kronMagErr 
vikingDetection 
VIKINGv20111019 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error 
kronMagErr 
vikingDetection 
VIKINGv20130417 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error 
kronMagErr 
vikingDetection 
VIKINGv20140402 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error 
kronMagErr 
vikingDetection 
VIKINGv20150421 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error;phot.mag 
kronMagErr 
vikingDetection 
VIKINGv20151230 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error;phot.mag 
kronMagErr 
vikingDetection 
VIKINGv20160406 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error;phot.mag 
kronMagErr 
vikingDetection 
VIKINGv20161202 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error;phot.mag 
kronMagErr 
vikingDetection 
VIKINGv20170715 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error;phot.mag 
kronMagErr 
vikingDetection 
VIKINGv20181012 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error;phot.mag 
kronMagErr 
vikingDetection, vikingListRemeasurement 
VIKINGv20110714 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error 
kronMagErr 
vikingMapRemeasurement 
VIKINGZYSELJv20160909 
error on calibrated Kron magnitude 
real 
4 
mag (CASU: default) 

stat.error 
kronMagErr 
vikingMapRemeasurement 
VIKINGZYSELJv20170124 
error on calibrated Kron magnitude 
real 
4 
mag (CASU: default) 

stat.error 
kronMagErr 
vmcDetection 
VMCDR1 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error 
kronMagErr 
vmcDetection 
VMCDR2 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error 
kronMagErr 
vmcDetection 
VMCDR3 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error;phot.mag 
kronMagErr 
vmcDetection 
VMCDR4 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error;phot.mag 
kronMagErr 
vmcDetection 
VMCv20110909 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error 
kronMagErr 
vmcDetection 
VMCv20120126 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error 
kronMagErr 
vmcDetection 
VMCv20121128 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error 
kronMagErr 
vmcDetection 
VMCv20130304 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error 
kronMagErr 
vmcDetection 
VMCv20130805 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error 
kronMagErr 
vmcDetection 
VMCv20140428 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error 
kronMagErr 
vmcDetection 
VMCv20140903 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error;phot.mag 
kronMagErr 
vmcDetection 
VMCv20150309 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error;phot.mag 
kronMagErr 
vmcDetection 
VMCv20151218 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error;phot.mag 
kronMagErr 
vmcDetection 
VMCv20160311 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error;phot.mag 
kronMagErr 
vmcDetection 
VMCv20160822 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error;phot.mag 
kronMagErr 
vmcDetection 
VMCv20170109 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error;phot.mag 
kronMagErr 
vmcDetection 
VMCv20170411 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error;phot.mag 
kronMagErr 
vmcDetection 
VMCv20171101 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error;phot.mag 
kronMagErr 
vmcDetection 
VMCv20180702 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error;phot.mag 
kronMagErr 
vmcDetection 
VMCv20181120 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error;phot.mag 
kronMagErr 
vmcDetection, vmcListRemeasurement 
VMCv20110816 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error 
kronMagErr 
vvvDetection 
VVVDR4 
error on calibrated Kron magnitude 
real 
4 
mag 

stat.error;phot.mag 
kronRad 
vhsDetection 
VHSDR2 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize;src 
kronRad 
vhsDetection 
VHSDR3 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vhsDetection 
VHSDR4 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vhsDetection 
VHSv20120926 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vhsDetection 
VHSv20130417 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vhsDetection 
VHSv20140409 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vhsDetection 
VHSv20150108 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vhsDetection 
VHSv20160114 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vhsDetection 
VHSv20160507 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vhsDetection 
VHSv20170630 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vhsDetection 
VHSv20171207 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vhsDetection 
VHSv20180419 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vhsDetection, vhsListRemeasurement 
VHSDR1 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize;src 
kronRad 
videoDetection 
VIDEODR2 
Kron radius as defined in SE by Graham and Driver (2005) (SE: KRON_RADIUS*A_IMAGE) {catalogue TType keyword: Kron_radius} r_k = ∑R² I(R) / ∑R I(R) 
real 
4 
pixels 

phys.angSize;src 
Since <FLUX>_RADIUS is expressed in multiples of the major axis, <FLUX>_RADIUS is multiplied by A_IMAGE to convert to pixels. 
kronRad 
videoDetection 
VIDEODR3 
Kron radius as defined in SE by Graham and Driver (2005) (SE: KRON_RADIUS*A_IMAGE) {catalogue TType keyword: Kron_radius} r_k = ∑R² I(R) / ∑R I(R) 
real 
4 
pixels 

phys.angSize 
Since <FLUX>_RADIUS is expressed in multiples of the major axis, <FLUX>_RADIUS is multiplied by A_IMAGE to convert to pixels. 
kronRad 
videoDetection 
VIDEODR4 
Kron radius as defined in SE by Graham and Driver (2005) (SE: KRON_RADIUS*A_IMAGE) {catalogue TType keyword: Kron_radius} r_k = ∑R² I(R) / ∑R I(R) 
real 
4 
pixels 

phys.angSize 
Since <FLUX>_RADIUS is expressed in multiples of the major axis, <FLUX>_RADIUS is multiplied by A_IMAGE to convert to pixels. 
kronRad 
videoDetection 
VIDEODR5 
Kron radius as defined in SE by Graham and Driver (2005) (SE: KRON_RADIUS*A_IMAGE) {catalogue TType keyword: Kron_radius} r_k = ∑R² I(R) / ∑R I(R) 
real 
4 
pixels 

phys.angSize 
Since <FLUX>_RADIUS is expressed in multiples of the major axis, <FLUX>_RADIUS is multiplied by A_IMAGE to convert to pixels. 
kronRad 
videoDetection 
VIDEOv20100513 
Kron radius as defined in SE by Graham and Driver (2005) (SE: KRON_RADIUS*A_IMAGE) {catalogue TType keyword: Kron_radius} r_k = ∑R² I(R) / ∑R I(R) 
real 
4 
pixels 

phys.angSize;src 
Since <FLUX>_RADIUS is expressed in multiples of the major axis, <FLUX>_RADIUS is multiplied by A_IMAGE to convert to pixels. 
kronRad 
videoDetection 
VIDEOv20111208 
Kron radius as defined in SE by Graham and Driver (2005) (SE: KRON_RADIUS*A_IMAGE) {catalogue TType keyword: Kron_radius} r_k = ∑R² I(R) / ∑R I(R) 
real 
4 
pixels 

phys.angSize;src 
Since <FLUX>_RADIUS is expressed in multiples of the major axis, <FLUX>_RADIUS is multiplied by A_IMAGE to convert to pixels. 
kronRad 
videoListRemeasurement 
VIDEOv20100513 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize;src 
kronRad 
vikingDetection 
VIKINGDR2 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize;src 
kronRad 
vikingDetection 
VIKINGDR3 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vikingDetection 
VIKINGDR4 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vikingDetection 
VIKINGv20111019 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize;src 
kronRad 
vikingDetection 
VIKINGv20130417 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vikingDetection 
VIKINGv20140402 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vikingDetection 
VIKINGv20150421 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vikingDetection 
VIKINGv20151230 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vikingDetection 
VIKINGv20160406 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vikingDetection 
VIKINGv20161202 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vikingDetection 
VIKINGv20170715 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vikingDetection 
VIKINGv20181012 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vikingDetection, vikingListRemeasurement 
VIKINGv20110714 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize;src 
kronRad 
vikingMapRemeasurement 
VIKINGZYSELJv20160909 
Kron radius as defined in SE by Graham and Driver (2005) (SE: KRON_RADIUS*A_IMAGE; CASU: default) {catalogue TType keyword: Kron_radius} r_k = ∑R² I(R) / ∑R I(R) 
real 
4 
pixels 

phys.angSize;src 
Since <FLUX>_RADIUS is expressed in multiples of the major axis, <FLUX>_RADIUS is multiplied by A_IMAGE to convert to pixels. 
kronRad 
vikingMapRemeasurement 
VIKINGZYSELJv20170124 
Kron radius as defined in SE by Graham and Driver (2005) (SE: KRON_RADIUS*A_IMAGE; CASU: default) {catalogue TType keyword: Kron_radius} r_k = ∑R² I(R) / ∑R I(R) 
real 
4 
pixels 

phys.angSize;src 
Since <FLUX>_RADIUS is expressed in multiples of the major axis, <FLUX>_RADIUS is multiplied by A_IMAGE to convert to pixels. 
kronRad 
vmcDetection 
VMCDR1 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize;src 
kronRad 
vmcDetection 
VMCDR2 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vmcDetection 
VMCDR3 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vmcDetection 
VMCDR4 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vmcDetection 
VMCv20110909 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize;src 
kronRad 
vmcDetection 
VMCv20120126 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize;src 
kronRad 
vmcDetection 
VMCv20121128 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vmcDetection 
VMCv20130304 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vmcDetection 
VMCv20130805 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vmcDetection 
VMCv20140428 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vmcDetection 
VMCv20140903 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vmcDetection 
VMCv20150309 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vmcDetection 
VMCv20151218 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vmcDetection 
VMCv20160311 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vmcDetection 
VMCv20160822 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vmcDetection 
VMCv20170109 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vmcDetection 
VMCv20170411 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vmcDetection 
VMCv20171101 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vmcDetection 
VMCv20180702 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vmcDetection 
VMCv20181120 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
kronRad 
vmcDetection, vmcListRemeasurement 
VMCv20110816 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize;src 
kronRad 
vvvDetection 
VVVDR4 
r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} 
real 
4 
pixels 

phys.angSize 
ks_1eNum 
vvvPsfDophotZYJHKsMergeLog 
VVVDR4 
the extension number of this 1st epoch Ks frame 
tinyint 
1 


meta.number;em.IR.K 
ks_1mfID 
vvvPsfDophotZYJHKsMergeLog 
VVVDR4 
the UID of the relevant 1st epoch Ks tile multiframe 
bigint 
8 


meta.id;obs.field;em.IR.K 
ks_1Mjd 
vvvPsfDophotZYJHKsMergeLog 
VVVDR4 
the MJD of the 1st epoch Ks tile multiframe 
float 
8 


time;em.IR.K 
ks_2eNum 
vvvPsfDophotZYJHKsMergeLog 
VVVDR4 
the extension number of this 2nd epoch Ks frame 
tinyint 
1 


meta.number;em.IR.K 
ks_2mfID 
vvvPsfDophotZYJHKsMergeLog 
VVVDR4 
the UID of the relevant 2nd epoch Ks tile multiframe 
bigint 
8 


meta.id;obs.field;em.IR.K 
ks_2Mjd 
vvvPsfDophotZYJHKsMergeLog 
VVVDR4 
the MJD of the 2nd epoch Ks tile multiframe 
float 
8 


time;em.IR.K 
ksAmpl 
vmcCepheidVariables 
VMCDR3 
Amplitude of Ks band magnitude variation {catalogue TType keyword: A(Ks)} 
real 
4 
mag 
0.9999995e9 
src.var.amplitude;em.IR.K 
ksAmpl 
vmcCepheidVariables 
VMCDR4 
PeaktoPeak amplitude in Ks band {catalogue TType keyword: A(Ks)} 
real 
4 
mag 
0.9999995e9 
src.var.amplitude;em.IR.K 
ksAmpl 
vmcCepheidVariables 
VMCv20121128 
Amplitude of Ks band magnitude variation {catalogue TType keyword: A(Ks)} 
real 
4 
mag 
0.9999995e9 
src.var.amplitude;em.IR.NIR 
ksAmpl 
vmcCepheidVariables 
VMCv20140428 
Amplitude of Ks band magnitude variation {catalogue TType keyword: A(Ks)} 
real 
4 
mag 
0.9999995e9 
src.var.amplitude;em.IR.K 
ksAmpl 
vmcCepheidVariables 
VMCv20140903 
Amplitude of Ks band magnitude variation {catalogue TType keyword: A(Ks)} 
real 
4 
mag 
0.9999995e9 
src.var.amplitude;em.IR.K 
ksAmpl 
vmcCepheidVariables 
VMCv20150309 
Amplitude of Ks band magnitude variation {catalogue TType keyword: A(Ks)} 
real 
4 
mag 
0.9999995e9 
src.var.amplitude;em.IR.K 
ksAmpl 
vmcCepheidVariables 
VMCv20151218 
Amplitude of Ks band magnitude variation {catalogue TType keyword: A(Ks)} 
real 
4 
mag 
0.9999995e9 
src.var.amplitude;em.IR.K 
ksAmpl 
vmcCepheidVariables 
VMCv20160311 
PeaktoPeak amplitude in Ks band {catalogue TType keyword: A(Ks)} 
real 
4 
mag 
0.9999995e9 
src.var.amplitude;em.IR.K 
ksAmpl 
vmcCepheidVariables 
VMCv20160822 
PeaktoPeak amplitude in Ks band {catalogue TType keyword: A(Ks)} 
real 
4 
mag 
0.9999995e9 
src.var.amplitude;em.IR.K 
ksAmpl 
vmcCepheidVariables 
VMCv20170109 
PeaktoPeak amplitude in Ks band {catalogue TType keyword: A(Ks)} 
real 
4 
mag 
0.9999995e9 
src.var.amplitude;em.IR.K 
ksAmpl 
vmcCepheidVariables 
VMCv20170411 
PeaktoPeak amplitude in Ks band {catalogue TType keyword: A(Ks)} 
real 
4 
mag 
0.9999995e9 
src.var.amplitude;em.IR.K 
ksAmpl 
vmcCepheidVariables 
VMCv20171101 
PeaktoPeak amplitude in Ks band {catalogue TType keyword: A(Ks)} 
real 
4 
mag 
0.9999995e9 
src.var.amplitude;em.IR.K 
ksAmpl 
vmcCepheidVariables 
VMCv20180702 
PeaktoPeak amplitude in Ks band {catalogue TType keyword: A(Ks)} 
real 
4 
mag 
0.9999995e9 
src.var.amplitude;em.IR.K 
ksAmpl 
vmcCepheidVariables 
VMCv20181120 
PeaktoPeak amplitude in Ks band {catalogue TType keyword: A(Ks)} 
real 
4 
mag 
0.9999995e9 
src.var.amplitude;em.IR.K 
ksAmpl 
vmcRRlyraeVariables 
VMCDR4 
Amplitude in K_s band provided by GRATIS {catalogue TType keyword: AMPL_K} 
real 
4 
mag 
0.9999995e9 
src.var.amplitude;em.IR.K 
ksAmpl 
vmcRRlyraeVariables 
VMCv20160822 
Amplitude in K_s band provided by GRATIS {catalogue TType keyword: AMPL_K} 
real 
4 
mag 
0.9999995e9 
src.var.amplitude;em.IR.K 
ksAmpl 
vmcRRlyraeVariables 
VMCv20170109 
Amplitude in K_s band provided by GRATIS {catalogue TType keyword: AMPL_K} 
real 
4 
mag 
0.9999995e9 
src.var.amplitude;em.IR.K 
ksAmpl 
vmcRRlyraeVariables 
VMCv20170411 
Amplitude in K_s band provided by GRATIS {catalogue TType keyword: AMPL_K} 
real 
4 
mag 
0.9999995e9 
src.var.amplitude;em.IR.K 
ksAmpl 
vmcRRlyraeVariables 
VMCv20171101 
Amplitude in K_s band provided by GRATIS {catalogue TType keyword: AMPL_K} 
real 
4 
mag 
0.9999995e9 
src.var.amplitude;em.IR.K 
ksAmpl 
vmcRRlyraeVariables 
VMCv20180702 
Amplitude in K_s band provided by GRATIS {catalogue TType keyword: AMPL_K} 
real 
4 
mag 
0.9999995e9 
src.var.amplitude;em.IR.K 
ksAmpl 
vmcRRlyraeVariables 
VMCv20181120 
Amplitude in K_s band provided by GRATIS {catalogue TType keyword: AMPL_K} 
real 
4 
mag 
0.9999995e9 
src.var.amplitude;em.IR.K 
ksAmplErr 
vmcCepheidVariables 
VMCDR4 
Error in PeaktoPeak amplitude in Ks band {catalogue TType keyword: e_A(Ks)} 
real 
4 
mag 
0.9999995e9 
stat.error;src.var.amplitude;em.IR.K 
ksAmplErr 
vmcCepheidVariables 
VMCv20160311 
Error in PeaktoPeak amplitude in Ks band {catalogue TType keyword: e_A(Ks)} 
real 
4 
mag 
0.9999995e9 
stat.error;src.var.amplitude;em.IR.K 
ksAmplErr 
vmcCepheidVariables 
VMCv20160822 
Error in PeaktoPeak amplitude in Ks band {catalogue TType keyword: e_A(Ks)} 
real 
4 
mag 
0.9999995e9 
stat.error;src.var.amplitude;em.IR.K 
ksAmplErr 
vmcCepheidVariables 
VMCv20170109 
Error in PeaktoPeak amplitude in Ks band {catalogue TType keyword: e_A(Ks)} 
real 
4 
mag 
0.9999995e9 
stat.error;src.var.amplitude;em.IR.K 
ksAmplErr 
vmcCepheidVariables 
VMCv20170411 
Error in PeaktoPeak amplitude in Ks band {catalogue TType keyword: e_A(Ks)} 
real 
4 
mag 
0.9999995e9 
stat.error;src.var.amplitude;em.IR.K 
ksAmplErr 
vmcCepheidVariables 
VMCv20171101 
Error in PeaktoPeak amplitude in Ks band {catalogue TType keyword: e_A(Ks)} 
real 
4 
mag 
0.9999995e9 
stat.error;src.var.amplitude;em.IR.K 
ksAmplErr 
vmcCepheidVariables 
VMCv20180702 
Error in PeaktoPeak amplitude in Ks band {catalogue TType keyword: e_A(Ks)} 
real 
4 
mag 
0.9999995e9 
stat.error;src.var.amplitude;em.IR.K 
ksAmplErr 
vmcCepheidVariables 
VMCv20181120 
Error in PeaktoPeak amplitude in Ks band {catalogue TType keyword: e_A(Ks)} 
real 
4 
mag 
0.9999995e9 
stat.error;src.var.amplitude;em.IR.K 
ksAperJky3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Default point source Ks aperture corrected (2.0 arcsec aperture diameter) calibrated flux If in doubt use this flux estimator 
real 
4 
jansky 
0.9999995e9 
phot.flux 
ksAperJky3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Default point source Ks aperture corrected (2.0 arcsec aperture diameter) calibrated flux If in doubt use this flux estimator 
real 
4 
jansky 
0.9999995e9 
phot.flux 
ksAperJky3Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Error in default point/extended source Ks (2.0 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
stat.error 
ksAperJky3Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Error in default point/extended source Ks (2.0 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
stat.error 
ksAperJky4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Point source Ks aperture corrected (2.8 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
ksAperJky4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Point source Ks aperture corrected (2.8 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
ksAperJky4Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Error in point/extended source Ks (2.8 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
stat.error 
ksAperJky4Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Error in point/extended source Ks (2.8 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
stat.error 
ksAperJky6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Point source Ks aperture corrected (5.7 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
ksAperJky6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Point source Ks aperture corrected (5.7 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
ksAperJky6Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Error in point/extended source Ks (5.7 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
stat.error 
ksAperJky6Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Error in point/extended source Ks (5.7 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
stat.error 
ksAperJkyNoAperCorr3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Default extended source Ks (2.0 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux If in doubt use this flux estimator 
real 
4 
jansky 
0.9999995e9 
phot.flux 
ksAperJkyNoAperCorr3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Default extended source Ks (2.0 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux If in doubt use this flux estimator 
real 
4 
jansky 
0.9999995e9 
phot.flux 
ksAperJkyNoAperCorr4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Extended source Ks (2.8 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
ksAperJkyNoAperCorr4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Extended source Ks (2.8 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
ksAperJkyNoAperCorr6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Extended source Ks (5.7 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
ksAperJkyNoAperCorr6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Extended source Ks (5.7 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
ksAperLup3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Default point source Ks aperture corrected (2.0 arcsec aperture diameter) luptitude If in doubt use this flux estimator 
real 
4 
lup 
0.9999995e9 
phot.lup 
ksAperLup3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Default point source Ks aperture corrected (2.0 arcsec aperture diameter) luptitude If in doubt use this flux estimator 
real 
4 
lup 
0.9999995e9 
phot.lup 
ksAperLup3Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Error in default point/extended source Ks (2.0 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
stat.error 
ksAperLup3Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Error in default point/extended source Ks (2.0 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
stat.error 
ksAperLup4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Point source Ks aperture corrected (2.8 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
ksAperLup4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Point source Ks aperture corrected (2.8 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
ksAperLup4Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Error in point/extended source Ks (2.8 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
stat.error 
ksAperLup4Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Error in point/extended source Ks (2.8 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
stat.error 
ksAperLup6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Point source Ks aperture corrected (5.7 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
ksAperLup6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Point source Ks aperture corrected (5.7 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
ksAperLup6Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Error in point/extended source Ks (5.7 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
stat.error 
ksAperLup6Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Error in point/extended source Ks (5.7 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
stat.error 
ksAperLupNoAperCorr3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Default extended source Ks (2.0 arcsec aperture diameter, but no aperture correction applied) aperture luptitude If in doubt use this flux estimator 
real 
4 
lup 
0.9999995e9 
phot.lup 
ksAperLupNoAperCorr3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Default extended source Ks (2.0 arcsec aperture diameter, but no aperture correction applied) aperture luptitude If in doubt use this flux estimator 
real 
4 
lup 
0.9999995e9 
phot.lup 
ksAperLupNoAperCorr4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Extended source Ks (2.8 arcsec aperture diameter, but no aperture correction applied) aperture luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
ksAperLupNoAperCorr4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Extended source Ks (2.8 arcsec aperture diameter, but no aperture correction applied) aperture luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
ksAperLupNoAperCorr6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Extended source Ks (5.7 arcsec aperture diameter, but no aperture correction applied) aperture luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
ksAperLupNoAperCorr6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Extended source Ks (5.7 arcsec aperture diameter, but no aperture correction applied) aperture luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
ksAperMag1 
vmcSynopticSource 
VMCDR1 
Extended source Ks aperture corrected mag (0.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag1 
vmcSynopticSource 
VMCDR2 
Extended source Ks aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag1 
vmcSynopticSource 
VMCDR3 
Extended source Ks aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag1 
vmcSynopticSource 
VMCDR4 
Extended source Ks aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag1 
vmcSynopticSource 
VMCv20110816 
Extended source Ks aperture corrected mag (0.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag1 
vmcSynopticSource 
VMCv20110909 
Extended source Ks aperture corrected mag (0.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag1 
vmcSynopticSource 
VMCv20120126 
Extended source Ks aperture corrected mag (0.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag1 
vmcSynopticSource 
VMCv20121128 
Extended source Ks aperture corrected mag (0.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag1 
vmcSynopticSource 
VMCv20130304 
Extended source Ks aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag1 
vmcSynopticSource 
VMCv20130805 
Extended source Ks aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag1 
vmcSynopticSource 
VMCv20140428 
Extended source Ks aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag1 
vmcSynopticSource 
VMCv20140903 
Extended source Ks aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag1 
vmcSynopticSource 
VMCv20150309 
Extended source Ks aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag1 
vmcSynopticSource 
VMCv20151218 
Extended source Ks aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag1 
vmcSynopticSource 
VMCv20160311 
Extended source Ks aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag1 
vmcSynopticSource 
VMCv20160822 
Extended source Ks aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag1 
vmcSynopticSource 
VMCv20170109 
Extended source Ks aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag1 
vmcSynopticSource 
VMCv20170411 
Extended source Ks aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag1 
vmcSynopticSource 
VMCv20171101 
Extended source Ks aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag1 
vmcSynopticSource 
VMCv20180702 
Extended source Ks aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag1 
vmcSynopticSource 
VMCv20181120 
Extended source Ks aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag1 
vvvSource 
VVVDR4 
Point source Ks aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag1 
vvvSynopticSource 
VVVDR4 
Extended source Ks aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag1Err 
vmcSynopticSource 
VMCDR1 
Error in extended source Ks mag (0.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag1Err 
vmcSynopticSource 
VMCDR2 
Error in extended source Ks mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag1Err 
vmcSynopticSource 
VMCDR3 
Error in extended source Ks mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag1Err 
vmcSynopticSource 
VMCDR4 
Error in extended source Ks mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag1Err 
vmcSynopticSource 
VMCv20110816 
Error in extended source Ks mag (0.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag1Err 
vmcSynopticSource 
VMCv20110909 
Error in extended source Ks mag (0.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag1Err 
vmcSynopticSource 
VMCv20120126 
Error in extended source Ks mag (0.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag1Err 
vmcSynopticSource 
VMCv20121128 
Error in extended source Ks mag (0.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag1Err 
vmcSynopticSource 
VMCv20130304 
Error in extended source Ks mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag1Err 
vmcSynopticSource 
VMCv20130805 
Error in extended source Ks mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag1Err 
vmcSynopticSource 
VMCv20140428 
Error in extended source Ks mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K 
ksAperMag1Err 
vmcSynopticSource 
VMCv20140903 
Error in extended source Ks mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag1Err 
vmcSynopticSource 
VMCv20150309 
Error in extended source Ks mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag1Err 
vmcSynopticSource 
VMCv20151218 
Error in extended source Ks mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag1Err 
vmcSynopticSource 
VMCv20160311 
Error in extended source Ks mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag1Err 
vmcSynopticSource 
VMCv20160822 
Error in extended source Ks mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag1Err 
vmcSynopticSource 
VMCv20170109 
Error in extended source Ks mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag1Err 
vmcSynopticSource 
VMCv20170411 
Error in extended source Ks mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag1Err 
vmcSynopticSource 
VMCv20171101 
Error in extended source Ks mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag1Err 
vmcSynopticSource 
VMCv20180702 
Error in extended source Ks mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag1Err 
vmcSynopticSource 
VMCv20181120 
Error in extended source Ks mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag1Err 
vvvSource 
VVVDR4 
Error in point source Ks mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag1Err 
vvvSynopticSource 
VVVDR4 
Error in extended source Ks mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag2 
vmcSynopticSource 
VMCDR1 
Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag2 
vmcSynopticSource 
VMCDR2 
Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag2 
vmcSynopticSource 
VMCDR3 
Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag2 
vmcSynopticSource 
VMCDR4 
Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag2 
vmcSynopticSource 
VMCv20110816 
Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag2 
vmcSynopticSource 
VMCv20110909 
Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag2 
vmcSynopticSource 
VMCv20120126 
Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag2 
vmcSynopticSource 
VMCv20121128 
Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag2 
vmcSynopticSource 
VMCv20130304 
Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag2 
vmcSynopticSource 
VMCv20130805 
Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag2 
vmcSynopticSource 
VMCv20140428 
Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag2 
vmcSynopticSource 
VMCv20140903 
Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag2 
vmcSynopticSource 
VMCv20150309 
Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag2 
vmcSynopticSource 
VMCv20151218 
Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag2 
vmcSynopticSource 
VMCv20160311 
Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag2 
vmcSynopticSource 
VMCv20160822 
Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag2 
vmcSynopticSource 
VMCv20170109 
Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag2 
vmcSynopticSource 
VMCv20170411 
Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag2 
vmcSynopticSource 
VMCv20171101 
Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag2 
vmcSynopticSource 
VMCv20180702 
Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag2 
vmcSynopticSource 
VMCv20181120 
Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag2 
vvvSynopticSource 
VVVDR4 
Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag2Err 
vmcSynopticSource 
VMCDR1 
Error in extended source Ks mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag2Err 
vmcSynopticSource 
VMCDR2 
Error in extended source Ks mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag2Err 
vmcSynopticSource 
VMCDR3 
Error in extended source Ks mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag2Err 
vmcSynopticSource 
VMCDR4 
Error in extended source Ks mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag2Err 
vmcSynopticSource 
VMCv20110816 
Error in extended source Ks mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag2Err 
vmcSynopticSource 
VMCv20110909 
Error in extended source Ks mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag2Err 
vmcSynopticSource 
VMCv20120126 
Error in extended source Ks mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag2Err 
vmcSynopticSource 
VMCv20121128 
Error in extended source Ks mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag2Err 
vmcSynopticSource 
VMCv20130304 
Error in extended source Ks mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag2Err 
vmcSynopticSource 
VMCv20130805 
Error in extended source Ks mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag2Err 
vmcSynopticSource 
VMCv20140428 
Error in extended source Ks mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K 
ksAperMag2Err 
vmcSynopticSource 
VMCv20140903 
Error in extended source Ks mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag2Err 
vmcSynopticSource 
VMCv20150309 
Error in extended source Ks mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag2Err 
vmcSynopticSource 
VMCv20151218 
Error in extended source Ks mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag2Err 
vmcSynopticSource 
VMCv20160311 
Error in extended source Ks mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag2Err 
vmcSynopticSource 
VMCv20160822 
Error in extended source Ks mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag2Err 
vmcSynopticSource 
VMCv20170109 
Error in extended source Ks mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag2Err 
vmcSynopticSource 
VMCv20170411 
Error in extended source Ks mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag2Err 
vmcSynopticSource 
VMCv20171101 
Error in extended source Ks mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag2Err 
vmcSynopticSource 
VMCv20180702 
Error in extended source Ks mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag2Err 
vmcSynopticSource 
VMCv20181120 
Error in extended source Ks mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag2Err 
vvvSynopticSource 
VVVDR4 
Error in extended source Ks mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag3 
vhsSource 
VHSDR1 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag3 
vhsSource 
VHSDR2 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag3 
vhsSource 
VHSDR3 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vhsSource 
VHSDR4 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vhsSource 
VHSv20120926 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag3 
vhsSource 
VHSv20130417 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag3 
vhsSource 
VHSv20140409 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vhsSource 
VHSv20150108 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vhsSource 
VHSv20160114 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vhsSource 
VHSv20160507 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vhsSource 
VHSv20170630 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vhsSource 
VHSv20171207 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vhsSource 
VHSv20180419 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
videoSource 
VIDEODR2 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag3 
videoSource 
VIDEODR3 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag3 
videoSource 
VIDEODR4 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
videoSource 
VIDEODR5 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
videoSource 
VIDEOv20100513 
Default point/extended source Ks mag, no aperture correction applied If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag3 
videoSource 
VIDEOv20111208 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag3 
vikingSource 
VIKINGDR2 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag3 
vikingSource 
VIKINGDR3 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag3 
vikingSource 
VIKINGDR4 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vikingSource 
VIKINGv20110714 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag3 
vikingSource 
VIKINGv20111019 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag3 
vikingSource 
VIKINGv20130417 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag3 
vikingSource 
VIKINGv20140402 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vikingSource 
VIKINGv20150421 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vikingSource 
VIKINGv20151230 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vikingSource 
VIKINGv20160406 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vikingSource 
VIKINGv20161202 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vikingSource 
VIKINGv20170715 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vikingSource 
VIKINGv20181012 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Default point source Ks aperture corrected (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Default point source Ks aperture corrected (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag3 
vmcSource 
VMCDR1 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag3 
vmcSource 
VMCDR2 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vmcSource 
VMCDR3 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vmcSource 
VMCDR4 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vmcSource 
VMCv20110816 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag3 
vmcSource 
VMCv20110909 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag3 
vmcSource 
VMCv20120126 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag3 
vmcSource 
VMCv20121128 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag3 
vmcSource 
VMCv20130304 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag3 
vmcSource 
VMCv20130805 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vmcSource 
VMCv20140428 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vmcSource 
VMCv20140903 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vmcSource 
VMCv20150309 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vmcSource 
VMCv20151218 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vmcSource 
VMCv20160311 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vmcSource 
VMCv20160822 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vmcSource 
VMCv20170109 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vmcSource 
VMCv20170411 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vmcSource 
VMCv20171101 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vmcSource 
VMCv20180702 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vmcSource 
VMCv20181120 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vmcSynopticSource 
VMCDR1 
Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag3 
vmcSynopticSource 
VMCDR2 
Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vmcSynopticSource 
VMCDR3 
Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vmcSynopticSource 
VMCDR4 
Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vmcSynopticSource 
VMCv20110816 
Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag3 
vmcSynopticSource 
VMCv20110909 
Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag3 
vmcSynopticSource 
VMCv20120126 
Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag3 
vmcSynopticSource 
VMCv20121128 
Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag3 
vmcSynopticSource 
VMCv20130304 
Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag3 
vmcSynopticSource 
VMCv20130805 
Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vmcSynopticSource 
VMCv20140428 
Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vmcSynopticSource 
VMCv20140903 
Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vmcSynopticSource 
VMCv20150309 
Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vmcSynopticSource 
VMCv20151218 
Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vmcSynopticSource 
VMCv20160311 
Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vmcSynopticSource 
VMCv20160822 
Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vmcSynopticSource 
VMCv20170109 
Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vmcSynopticSource 
VMCv20170411 
Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vmcSynopticSource 
VMCv20171101 
Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vmcSynopticSource 
VMCv20180702 
Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vmcSynopticSource 
VMCv20181120 
Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vvvSource 
VVVDR4 
Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3 
vvvSynopticSource 
VVVDR4 
Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag3Err 
vhsSource 
VHSDR1 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag3Err 
vhsSource 
VHSDR2 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag3Err 
vhsSource 
VHSDR3 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K 
ksAperMag3Err 
vhsSource 
VHSDR4 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag3Err 
vhsSource 
VHSv20120926 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag3Err 
vhsSource 
VHSv20130417 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag3Err 
vhsSource 
VHSv20140409 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K 
ksAperMag3Err 
vhsSource 
VHSv20150108 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag3Err 
vhsSource 
VHSv20160114 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag3Err 
vhsSource 
VHSv20160507 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag3Err 
vhsSource 
VHSv20170630 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag3Err 
vhsSource 
VHSv20171207 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag3Err 
vhsSource 
VHSv20180419 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag3Err 
videoSource 
VIDEODR2 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag3Err 
videoSource 
VIDEODR3 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag3Err 
videoSource 
VIDEODR4 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag3Err 
videoSource 
VIDEODR5 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag3Err 
videoSource 
VIDEOv20100513 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag3Err 
videoSource 
VIDEOv20111208 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag3Err 
vikingSource 
VIKINGDR2 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag3Err 
vikingSource 
VIKINGDR3 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag3Err 
vikingSource 
VIKINGDR4 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K 
ksAperMag3Err 
vikingSource 
VIKINGv20110714 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag3Err 
vikingSource 
VIKINGv20111019 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag3Err 
vikingSource 
VIKINGv20130417 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag3Err 
vikingSource 
VIKINGv20140402 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag3Err 
vikingSource 
VIKINGv20150421 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag3Err 
vikingSource 
VIKINGv20151230 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag3Err 
vikingSource 
VIKINGv20160406 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag3Err 
vikingSource 
VIKINGv20161202 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag3Err 
vikingSource 
VIKINGv20170715 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag3Err 
vikingSource 
VIKINGv20181012 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag3Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Error in default point/extended source Ks (2.0 arcsec aperture diameter) magnitude 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag3Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Error in default point/extended source Ks (2.0 arcsec aperture diameter) magnitude 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag3Err 
vmcSource 
VMCDR2 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag3Err 
vmcSource 
VMCDR3 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag3Err 
vmcSource 
VMCDR4 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag3Err 
vmcSource 
VMCv20110816 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag3Err 
vmcSource 
VMCv20110909 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag3Err 
vmcSource 
VMCv20120126 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag3Err 
vmcSource 
VMCv20121128 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag3Err 
vmcSource 
VMCv20130304 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag3Err 
vmcSource 
VMCv20130805 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag3Err 
vmcSource 
VMCv20140428 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K 
ksAperMag3Err 
vmcSource 
VMCv20140903 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag3Err 
vmcSource 
VMCv20150309 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag3Err 
vmcSource 
VMCv20151218 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag3Err 
vmcSource 
VMCv20160311 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag3Err 
vmcSource 
VMCv20160822 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag3Err 
vmcSource 
VMCv20170109 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag3Err 
vmcSource 
VMCv20170411 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag3Err 
vmcSource 
VMCv20171101 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag3Err 
vmcSource 
VMCv20180702 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag3Err 
vmcSource 
VMCv20181120 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag3Err 
vmcSource, vmcSynopticSource 
VMCDR1 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag3Err 
vvvSource 
VVVDR4 
Error in default point source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag3Err 
vvvSynopticSource 
VVVDR4 
Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag4 
vhsSource 
VHSDR1 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag4 
vhsSource 
VHSDR2 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag4 
vhsSource 
VHSDR3 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vhsSource 
VHSDR4 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vhsSource 
VHSv20120926 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag4 
vhsSource 
VHSv20130417 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag4 
vhsSource 
VHSv20140409 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vhsSource 
VHSv20150108 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vhsSource 
VHSv20160114 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vhsSource 
VHSv20160507 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vhsSource 
VHSv20170630 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vhsSource 
VHSv20171207 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vhsSource 
VHSv20180419 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
videoSource 
VIDEODR2 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag4 
videoSource 
VIDEODR3 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag4 
videoSource 
VIDEODR4 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
videoSource 
VIDEODR5 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
videoSource 
VIDEOv20100513 
Extended source Ks mag, no aperture correction applied 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag4 
videoSource 
VIDEOv20111208 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag4 
vikingSource 
VIKINGDR2 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag4 
vikingSource 
VIKINGDR3 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag4 
vikingSource 
VIKINGDR4 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vikingSource 
VIKINGv20110714 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag4 
vikingSource 
VIKINGv20111019 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag4 
vikingSource 
VIKINGv20130417 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag4 
vikingSource 
VIKINGv20140402 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vikingSource 
VIKINGv20150421 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vikingSource 
VIKINGv20151230 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vikingSource 
VIKINGv20160406 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vikingSource 
VIKINGv20161202 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vikingSource 
VIKINGv20170715 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vikingSource 
VIKINGv20181012 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Point source Ks aperture corrected (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Point source Ks aperture corrected (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag4 
vmcSource 
VMCDR1 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag4 
vmcSource 
VMCDR2 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vmcSource 
VMCDR3 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vmcSource 
VMCDR4 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vmcSource 
VMCv20110816 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag4 
vmcSource 
VMCv20110909 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag4 
vmcSource 
VMCv20120126 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag4 
vmcSource 
VMCv20121128 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag4 
vmcSource 
VMCv20130304 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag4 
vmcSource 
VMCv20130805 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vmcSource 
VMCv20140428 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vmcSource 
VMCv20140903 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vmcSource 
VMCv20150309 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vmcSource 
VMCv20151218 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vmcSource 
VMCv20160311 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vmcSource 
VMCv20160822 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vmcSource 
VMCv20170109 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vmcSource 
VMCv20170411 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vmcSource 
VMCv20171101 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vmcSource 
VMCv20180702 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vmcSource 
VMCv20181120 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vmcSynopticSource 
VMCDR1 
Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag4 
vmcSynopticSource 
VMCDR2 
Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vmcSynopticSource 
VMCDR3 
Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vmcSynopticSource 
VMCDR4 
Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vmcSynopticSource 
VMCv20110816 
Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag4 
vmcSynopticSource 
VMCv20110909 
Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag4 
vmcSynopticSource 
VMCv20120126 
Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag4 
vmcSynopticSource 
VMCv20121128 
Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag4 
vmcSynopticSource 
VMCv20130304 
Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag4 
vmcSynopticSource 
VMCv20130805 
Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vmcSynopticSource 
VMCv20140428 
Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vmcSynopticSource 
VMCv20140903 
Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vmcSynopticSource 
VMCv20150309 
Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vmcSynopticSource 
VMCv20151218 
Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vmcSynopticSource 
VMCv20160311 
Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vmcSynopticSource 
VMCv20160822 
Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vmcSynopticSource 
VMCv20170109 
Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vmcSynopticSource 
VMCv20170411 
Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vmcSynopticSource 
VMCv20171101 
Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vmcSynopticSource 
VMCv20180702 
Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vmcSynopticSource 
VMCv20181120 
Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vvvSource 
VVVDR4 
Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4 
vvvSynopticSource 
VVVDR4 
Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag4Err 
vhsSource 
VHSDR1 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag4Err 
vhsSource 
VHSDR2 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag4Err 
vhsSource 
VHSDR3 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K 
ksAperMag4Err 
vhsSource 
VHSDR4 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag4Err 
vhsSource 
VHSv20120926 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag4Err 
vhsSource 
VHSv20130417 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag4Err 
vhsSource 
VHSv20140409 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K 
ksAperMag4Err 
vhsSource 
VHSv20150108 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag4Err 
vhsSource 
VHSv20160114 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag4Err 
vhsSource 
VHSv20160507 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag4Err 
vhsSource 
VHSv20170630 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag4Err 
vhsSource 
VHSv20171207 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag4Err 
vhsSource 
VHSv20180419 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag4Err 
videoSource 
VIDEODR2 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag4Err 
videoSource 
VIDEODR3 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag4Err 
videoSource 
VIDEODR4 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag4Err 
videoSource 
VIDEODR5 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag4Err 
videoSource 
VIDEOv20100513 
Error in extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag4Err 
videoSource 
VIDEOv20111208 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag4Err 
vikingSource 
VIKINGDR2 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag4Err 
vikingSource 
VIKINGDR3 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag4Err 
vikingSource 
VIKINGDR4 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K 
ksAperMag4Err 
vikingSource 
VIKINGv20110714 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag4Err 
vikingSource 
VIKINGv20111019 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag4Err 
vikingSource 
VIKINGv20130417 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag4Err 
vikingSource 
VIKINGv20140402 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag4Err 
vikingSource 
VIKINGv20150421 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag4Err 
vikingSource 
VIKINGv20151230 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag4Err 
vikingSource 
VIKINGv20160406 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag4Err 
vikingSource 
VIKINGv20161202 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag4Err 
vikingSource 
VIKINGv20170715 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag4Err 
vikingSource 
VIKINGv20181012 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag4Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Error in point/extended source Ks (2.8 arcsec aperture diameter) magnitude 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag4Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Error in point/extended source Ks (2.8 arcsec aperture diameter) magnitude 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag4Err 
vmcSource 
VMCDR1 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag4Err 
vmcSource 
VMCDR2 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag4Err 
vmcSource 
VMCDR3 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag4Err 
vmcSource 
VMCDR4 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag4Err 
vmcSource 
VMCv20110816 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag4Err 
vmcSource 
VMCv20110909 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag4Err 
vmcSource 
VMCv20120126 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag4Err 
vmcSource 
VMCv20121128 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag4Err 
vmcSource 
VMCv20130304 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag4Err 
vmcSource 
VMCv20130805 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag4Err 
vmcSource 
VMCv20140428 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K 
ksAperMag4Err 
vmcSource 
VMCv20140903 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag4Err 
vmcSource 
VMCv20150309 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag4Err 
vmcSource 
VMCv20151218 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag4Err 
vmcSource 
VMCv20160311 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag4Err 
vmcSource 
VMCv20160822 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag4Err 
vmcSource 
VMCv20170109 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag4Err 
vmcSource 
VMCv20170411 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag4Err 
vmcSource 
VMCv20171101 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag4Err 
vmcSource 
VMCv20180702 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag4Err 
vmcSource 
VMCv20181120 
Error in point/extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag4Err 
vmcSynopticSource 
VMCDR1 
Error in extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag4Err 
vmcSynopticSource 
VMCDR2 
Error in extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag4Err 
vmcSynopticSource 
VMCDR3 
Error in extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag4Err 
vmcSynopticSource 
VMCDR4 
Error in extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag4Err 
vmcSynopticSource 
VMCv20110816 
Error in extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag4Err 
vmcSynopticSource 
VMCv20110909 
Error in extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag4Err 
vmcSynopticSource 
VMCv20120126 
Error in extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag4Err 
vmcSynopticSource 
VMCv20121128 
Error in extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag4Err 
vmcSynopticSource 
VMCv20130304 
Error in extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag4Err 
vmcSynopticSource 
VMCv20130805 
Error in extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag4Err 
vmcSynopticSource 
VMCv20140428 
Error in extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K 
ksAperMag4Err 
vmcSynopticSource 
VMCv20140903 
Error in extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag4Err 
vmcSynopticSource 
VMCv20150309 
Error in extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag4Err 
vmcSynopticSource 
VMCv20151218 
Error in extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag4Err 
vmcSynopticSource 
VMCv20160311 
Error in extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag4Err 
vmcSynopticSource 
VMCv20160822 
Error in extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag4Err 
vmcSynopticSource 
VMCv20170109 
Error in extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag4Err 
vmcSynopticSource 
VMCv20170411 
Error in extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag4Err 
vmcSynopticSource 
VMCv20171101 
Error in extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag4Err 
vmcSynopticSource 
VMCv20180702 
Error in extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag4Err 
vmcSynopticSource 
VMCv20181120 
Error in extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag4Err 
vvvSource 
VVVDR4 
Error in point source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag4Err 
vvvSynopticSource 
VVVDR4 
Error in extended source Ks mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag5 
vmcSynopticSource 
VMCDR1 
Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag5 
vmcSynopticSource 
VMCDR2 
Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag5 
vmcSynopticSource 
VMCDR3 
Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag5 
vmcSynopticSource 
VMCDR4 
Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag5 
vmcSynopticSource 
VMCv20110816 
Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag5 
vmcSynopticSource 
VMCv20110909 
Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag5 
vmcSynopticSource 
VMCv20120126 
Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag5 
vmcSynopticSource 
VMCv20121128 
Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag5 
vmcSynopticSource 
VMCv20130304 
Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag5 
vmcSynopticSource 
VMCv20130805 
Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag5 
vmcSynopticSource 
VMCv20140428 
Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag5 
vmcSynopticSource 
VMCv20140903 
Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag5 
vmcSynopticSource 
VMCv20150309 
Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag5 
vmcSynopticSource 
VMCv20151218 
Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag5 
vmcSynopticSource 
VMCv20160311 
Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag5 
vmcSynopticSource 
VMCv20160822 
Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag5 
vmcSynopticSource 
VMCv20170109 
Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag5 
vmcSynopticSource 
VMCv20170411 
Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag5 
vmcSynopticSource 
VMCv20171101 
Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag5 
vmcSynopticSource 
VMCv20180702 
Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag5 
vmcSynopticSource 
VMCv20181120 
Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag5 
vvvSynopticSource 
VVVDR4 
Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag5Err 
vmcSynopticSource 
VMCDR1 
Error in extended source Ks mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag5Err 
vmcSynopticSource 
VMCDR2 
Error in extended source Ks mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag5Err 
vmcSynopticSource 
VMCDR3 
Error in extended source Ks mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag5Err 
vmcSynopticSource 
VMCDR4 
Error in extended source Ks mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag5Err 
vmcSynopticSource 
VMCv20110816 
Error in extended source Ks mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag5Err 
vmcSynopticSource 
VMCv20110909 
Error in extended source Ks mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag5Err 
vmcSynopticSource 
VMCv20120126 
Error in extended source Ks mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag5Err 
vmcSynopticSource 
VMCv20121128 
Error in extended source Ks mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag5Err 
vmcSynopticSource 
VMCv20130304 
Error in extended source Ks mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag5Err 
vmcSynopticSource 
VMCv20130805 
Error in extended source Ks mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag5Err 
vmcSynopticSource 
VMCv20140428 
Error in extended source Ks mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K 
ksAperMag5Err 
vmcSynopticSource 
VMCv20140903 
Error in extended source Ks mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag5Err 
vmcSynopticSource 
VMCv20150309 
Error in extended source Ks mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag5Err 
vmcSynopticSource 
VMCv20151218 
Error in extended source Ks mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag5Err 
vmcSynopticSource 
VMCv20160311 
Error in extended source Ks mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag5Err 
vmcSynopticSource 
VMCv20160822 
Error in extended source Ks mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag5Err 
vmcSynopticSource 
VMCv20170109 
Error in extended source Ks mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag5Err 
vmcSynopticSource 
VMCv20170411 
Error in extended source Ks mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag5Err 
vmcSynopticSource 
VMCv20171101 
Error in extended source Ks mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag5Err 
vmcSynopticSource 
VMCv20180702 
Error in extended source Ks mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag5Err 
vmcSynopticSource 
VMCv20181120 
Error in extended source Ks mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag5Err 
vvvSynopticSource 
VVVDR4 
Error in extended source Ks mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag6 
vhsSource 
VHSDR1 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag6 
vhsSource 
VHSDR2 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag6 
vhsSource 
VHSDR3 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag6 
vhsSource 
VHSDR4 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag6 
vhsSource 
VHSv20120926 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag6 
vhsSource 
VHSv20130417 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag6 
vhsSource 
VHSv20140409 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag6 
vhsSource 
VHSv20150108 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag6 
vhsSource 
VHSv20160114 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag6 
vhsSource 
VHSv20160507 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag6 
vhsSource 
VHSv20170630 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag6 
vhsSource 
VHSv20171207 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag6 
vhsSource 
VHSv20180419 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag6 
videoSource 
VIDEODR2 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag6 
videoSource 
VIDEODR3 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag6 
videoSource 
VIDEODR4 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag6 
videoSource 
VIDEODR5 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag6 
videoSource 
VIDEOv20100513 
Extended source Ks mag, no aperture correction applied 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag6 
videoSource 
VIDEOv20111208 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag6 
vikingSource 
VIKINGDR2 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag6 
vikingSource 
VIKINGDR3 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag6 
vikingSource 
VIKINGDR4 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag6 
vikingSource 
VIKINGv20110714 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag6 
vikingSource 
VIKINGv20111019 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag6 
vikingSource 
VIKINGv20130417 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag6 
vikingSource 
VIKINGv20140402 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag6 
vikingSource 
VIKINGv20150421 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag6 
vikingSource 
VIKINGv20151230 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag6 
vikingSource 
VIKINGv20160406 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag6 
vikingSource 
VIKINGv20161202 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag6 
vikingSource 
VIKINGv20170715 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag6 
vikingSource 
VIKINGv20181012 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Point source Ks aperture corrected (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Point source Ks aperture corrected (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag6 
vmcSource 
VMCDR1 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag6 
vmcSource 
VMCDR2 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag6 
vmcSource 
VMCDR3 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag6 
vmcSource 
VMCDR4 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag6 
vmcSource 
VMCv20110816 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag6 
vmcSource 
VMCv20110909 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag6 
vmcSource 
VMCv20120126 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag6 
vmcSource 
VMCv20121128 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag6 
vmcSource 
VMCv20130304 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMag6 
vmcSource 
VMCv20130805 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag6 
vmcSource 
VMCv20140428 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag6 
vmcSource 
VMCv20140903 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag6 
vmcSource 
VMCv20150309 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag6 
vmcSource 
VMCv20151218 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag6 
vmcSource 
VMCv20160311 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag6 
vmcSource 
VMCv20160822 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag6 
vmcSource 
VMCv20170109 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag6 
vmcSource 
VMCv20170411 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag6 
vmcSource 
VMCv20171101 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag6 
vmcSource 
VMCv20180702 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag6 
vmcSource 
VMCv20181120 
Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMag6Err 
vhsSource 
VHSDR1 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag6Err 
vhsSource 
VHSDR2 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag6Err 
vhsSource 
VHSDR3 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K 
ksAperMag6Err 
vhsSource 
VHSDR4 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag6Err 
vhsSource 
VHSv20120926 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag6Err 
vhsSource 
VHSv20130417 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag6Err 
vhsSource 
VHSv20140409 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K 
ksAperMag6Err 
vhsSource 
VHSv20150108 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag6Err 
vhsSource 
VHSv20160114 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag6Err 
vhsSource 
VHSv20160507 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag6Err 
vhsSource 
VHSv20170630 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag6Err 
vhsSource 
VHSv20171207 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag6Err 
vhsSource 
VHSv20180419 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag6Err 
videoSource 
VIDEODR2 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag6Err 
videoSource 
VIDEODR3 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag6Err 
videoSource 
VIDEODR4 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag6Err 
videoSource 
VIDEODR5 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag6Err 
videoSource 
VIDEOv20100513 
Error in extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag6Err 
videoSource 
VIDEOv20111208 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag6Err 
vikingSource 
VIKINGDR2 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag6Err 
vikingSource 
VIKINGDR3 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag6Err 
vikingSource 
VIKINGDR4 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K 
ksAperMag6Err 
vikingSource 
VIKINGv20110714 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag6Err 
vikingSource 
VIKINGv20111019 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag6Err 
vikingSource 
VIKINGv20130417 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag6Err 
vikingSource 
VIKINGv20140402 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag6Err 
vikingSource 
VIKINGv20150421 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag6Err 
vikingSource 
VIKINGv20151230 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag6Err 
vikingSource 
VIKINGv20160406 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag6Err 
vikingSource 
VIKINGv20161202 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag6Err 
vikingSource 
VIKINGv20170715 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag6Err 
vikingSource 
VIKINGv20181012 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag6Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Error in point/extended source Ks (5.7 arcsec aperture diameter) magnitude 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag6Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Error in point/extended source Ks (5.7 arcsec aperture diameter) magnitude 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag6Err 
vmcSource 
VMCDR1 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag6Err 
vmcSource 
VMCDR2 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag6Err 
vmcSource 
VMCDR3 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag6Err 
vmcSource 
VMCDR4 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag6Err 
vmcSource 
VMCv20110816 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag6Err 
vmcSource 
VMCv20110909 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag6Err 
vmcSource 
VMCv20120126 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag6Err 
vmcSource 
VMCv20121128 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag6Err 
vmcSource 
VMCv20130304 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag6Err 
vmcSource 
VMCv20130805 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
ksAperMag6Err 
vmcSource 
VMCv20140428 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K 
ksAperMag6Err 
vmcSource 
VMCv20140903 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag6Err 
vmcSource 
VMCv20150309 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K;phot.mag 
ksAperMag6Err 
vmcSource 
VMCv20151218 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag6Err 
vmcSource 
VMCv20160311 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag6Err 
vmcSource 
VMCv20160822 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag6Err 
vmcSource 
VMCv20170109 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag6Err 
vmcSource 
VMCv20170411 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag6Err 
vmcSource 
VMCv20171101 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag6Err 
vmcSource 
VMCv20180702 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMag6Err 
vmcSource 
VMCv20181120 
Error in point/extended source Ks mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.K 
ksAperMagNoAperCorr3 
vhsSource 
VHSDR1 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr3 
vhsSource 
VHSDR2 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr3 
vhsSource 
VHSDR3 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr3 
vhsSource 
VHSDR4 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr3 
vhsSource 
VHSv20120926 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr3 
vhsSource 
VHSv20130417 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr3 
vhsSource 
VHSv20140409 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr3 
vhsSource 
VHSv20150108 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr3 
vhsSource 
VHSv20160114 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr3 
vhsSource 
VHSv20160507 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr3 
vhsSource 
VHSv20170630 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr3 
vhsSource 
VHSv20171207 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr3 
vhsSource 
VHSv20180419 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr3 
videoSource 
VIDEODR2 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr3 
videoSource 
VIDEODR3 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr3 
videoSource 
VIDEODR4 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr3 
videoSource 
VIDEODR5 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr3 
videoSource 
VIDEOv20111208 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr3 
vikingSource 
VIKINGDR2 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr3 
vikingSource 
VIKINGDR3 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr3 
vikingSource 
VIKINGDR4 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr3 
vikingSource 
VIKINGv20110714 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr3 
vikingSource 
VIKINGv20111019 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr3 
vikingSource 
VIKINGv20130417 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr3 
vikingSource 
VIKINGv20140402 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr3 
vikingSource 
VIKINGv20150421 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr3 
vikingSource 
VIKINGv20151230 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr3 
vikingSource 
VIKINGv20160406 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr3 
vikingSource 
VIKINGv20161202 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr3 
vikingSource 
VIKINGv20170715 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr3 
vikingSource 
VIKINGv20181012 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Default extended source Ks (2.0 arcsec aperture diameter, but no aperture correction applied) aperture magnitude If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Default extended source Ks (2.0 arcsec aperture diameter, but no aperture correction applied) aperture magnitude If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr3 
vmcSource 
VMCDR1 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr3 
vmcSource 
VMCDR2 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr3 
vmcSource 
VMCDR3 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr3 
vmcSource 
VMCDR4 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr3 
vmcSource 
VMCv20110816 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr3 
vmcSource 
VMCv20110909 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr3 
vmcSource 
VMCv20120126 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr3 
vmcSource 
VMCv20121128 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr3 
vmcSource 
VMCv20130304 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr3 
vmcSource 
VMCv20130805 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr3 
vmcSource 
VMCv20140428 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr3 
vmcSource 
VMCv20140903 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr3 
vmcSource 
VMCv20150309 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr3 
vmcSource 
VMCv20151218 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr3 
vmcSource 
VMCv20160311 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr3 
vmcSource 
VMCv20160822 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr3 
vmcSource 
VMCv20170109 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr3 
vmcSource 
VMCv20170411 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr3 
vmcSource 
VMCv20171101 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr3 
vmcSource 
VMCv20180702 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr3 
vmcSource 
VMCv20181120 
Default extended source Ks aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr4 
vhsSource 
VHSDR1 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr4 
vhsSource 
VHSDR2 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr4 
vhsSource 
VHSDR3 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr4 
vhsSource 
VHSDR4 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr4 
vhsSource 
VHSv20120926 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr4 
vhsSource 
VHSv20130417 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr4 
vhsSource 
VHSv20140409 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr4 
vhsSource 
VHSv20150108 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr4 
vhsSource 
VHSv20160114 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr4 
vhsSource 
VHSv20160507 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr4 
vhsSource 
VHSv20170630 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr4 
vhsSource 
VHSv20171207 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr4 
vhsSource 
VHSv20180419 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr4 
videoSource 
VIDEODR2 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr4 
videoSource 
VIDEODR3 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr4 
videoSource 
VIDEODR4 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr4 
videoSource 
VIDEODR5 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr4 
videoSource 
VIDEOv20111208 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr4 
vikingSource 
VIKINGDR2 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr4 
vikingSource 
VIKINGDR3 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr4 
vikingSource 
VIKINGDR4 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr4 
vikingSource 
VIKINGv20110714 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr4 
vikingSource 
VIKINGv20111019 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr4 
vikingSource 
VIKINGv20130417 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr4 
vikingSource 
VIKINGv20140402 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr4 
vikingSource 
VIKINGv20150421 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr4 
vikingSource 
VIKINGv20151230 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr4 
vikingSource 
VIKINGv20160406 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr4 
vikingSource 
VIKINGv20161202 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr4 
vikingSource 
VIKINGv20170715 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr4 
vikingSource 
VIKINGv20181012 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Extended source Ks (2.8 arcsec aperture diameter, but no aperture correction applied) aperture magnitude 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Extended source Ks (2.8 arcsec aperture diameter, but no aperture correction applied) aperture magnitude 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr4 
vmcSource 
VMCDR1 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr4 
vmcSource 
VMCDR2 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr4 
vmcSource 
VMCDR3 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr4 
vmcSource 
VMCDR4 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr4 
vmcSource 
VMCv20110816 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr4 
vmcSource 
VMCv20110909 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr4 
vmcSource 
VMCv20120126 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr4 
vmcSource 
VMCv20121128 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr4 
vmcSource 
VMCv20130304 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr4 
vmcSource 
VMCv20130805 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr4 
vmcSource 
VMCv20140428 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr4 
vmcSource 
VMCv20140903 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr4 
vmcSource 
VMCv20150309 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr4 
vmcSource 
VMCv20151218 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr4 
vmcSource 
VMCv20160311 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr4 
vmcSource 
VMCv20160822 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr4 
vmcSource 
VMCv20170109 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr4 
vmcSource 
VMCv20170411 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr4 
vmcSource 
VMCv20171101 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr4 
vmcSource 
VMCv20180702 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr4 
vmcSource 
VMCv20181120 
Extended source Ks aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr6 
vhsSource 
VHSDR1 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr6 
vhsSource 
VHSDR2 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr6 
vhsSource 
VHSDR3 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr6 
vhsSource 
VHSDR4 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr6 
vhsSource 
VHSv20120926 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr6 
vhsSource 
VHSv20130417 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr6 
vhsSource 
VHSv20140409 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr6 
vhsSource 
VHSv20150108 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr6 
vhsSource 
VHSv20160114 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr6 
vhsSource 
VHSv20160507 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr6 
vhsSource 
VHSv20170630 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr6 
vhsSource 
VHSv20171207 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr6 
vhsSource 
VHSv20180419 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr6 
videoSource 
VIDEODR2 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr6 
videoSource 
VIDEODR3 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr6 
videoSource 
VIDEODR4 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr6 
videoSource 
VIDEODR5 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr6 
videoSource 
VIDEOv20111208 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr6 
vikingSource 
VIKINGDR2 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr6 
vikingSource 
VIKINGDR3 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr6 
vikingSource 
VIKINGDR4 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr6 
vikingSource 
VIKINGv20110714 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr6 
vikingSource 
VIKINGv20111019 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr6 
vikingSource 
VIKINGv20130417 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr6 
vikingSource 
VIKINGv20140402 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr6 
vikingSource 
VIKINGv20150421 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr6 
vikingSource 
VIKINGv20151230 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr6 
vikingSource 
VIKINGv20160406 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr6 
vikingSource 
VIKINGv20161202 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr6 
vikingSource 
VIKINGv20170715 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr6 
vikingSource 
VIKINGv20181012 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Extended source Ks (5.7 arcsec aperture diameter, but no aperture correction applied) aperture magnitude 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Extended source Ks (5.7 arcsec aperture diameter, but no aperture correction applied) aperture magnitude 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr6 
vmcSource 
VMCDR1 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr6 
vmcSource 
VMCDR2 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr6 
vmcSource 
VMCDR3 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr6 
vmcSource 
VMCDR4 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr6 
vmcSource 
VMCv20110816 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr6 
vmcSource 
VMCv20110909 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr6 
vmcSource 
VMCv20120126 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr6 
vmcSource 
VMCv20121128 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr6 
vmcSource 
VMCv20130304 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
ksAperMagNoAperCorr6 
vmcSource 
VMCv20130805 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr6 
vmcSource 
VMCv20140428 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr6 
vmcSource 
VMCv20140903 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr6 
vmcSource 
VMCv20150309 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr6 
vmcSource 
VMCv20151218 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr6 
vmcSource 
VMCv20160311 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr6 
vmcSource 
VMCv20160822 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr6 
vmcSource 
VMCv20170109 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr6 
vmcSource 
VMCv20170411 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr6 
vmcSource 
VMCv20171101 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr6 
vmcSource 
VMCv20180702 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksAperMagNoAperCorr6 
vmcSource 
VMCv20181120 
Extended source Ks aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K 
ksaStratAst 
videoVarFrameSetInfo 
VIDEODR2 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks 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. 
ksaStratAst 
videoVarFrameSetInfo 
VIDEODR3 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks 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. 
ksaStratAst 
videoVarFrameSetInfo 
VIDEODR4 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
ksaStratAst 
videoVarFrameSetInfo 
VIDEODR5 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
ksaStratAst 
videoVarFrameSetInfo 
VIDEOv20100513 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks 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. 
ksaStratAst 
videoVarFrameSetInfo 
VIDEOv20111208 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks 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. 
ksaStratAst 
vikingVarFrameSetInfo 
VIKINGDR2 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks 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. 
ksaStratAst 
vikingVarFrameSetInfo 
VIKINGv20110714 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks 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. 
ksaStratAst 
vikingVarFrameSetInfo 
VIKINGv20111019 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks 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. 
ksaStratAst 
vmcVarFrameSetInfo 
VMCDR1 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks 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. 
ksaStratAst 
vmcVarFrameSetInfo 
VMCDR2 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks 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. 
ksaStratAst 
vmcVarFrameSetInfo 
VMCDR3 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
ksaStratAst 
vmcVarFrameSetInfo 
VMCDR4 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
ksaStratAst 
vmcVarFrameSetInfo 
VMCv20110816 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks 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. 
ksaStratAst 
vmcVarFrameSetInfo 
VMCv20110909 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks 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. 
ksaStratAst 
vmcVarFrameSetInfo 
VMCv20120126 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks 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. 
ksaStratAst 
vmcVarFrameSetInfo 
VMCv20121128 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks 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. 
ksaStratAst 
vmcVarFrameSetInfo 
VMCv20130304 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks 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. 
ksaStratAst 
vmcVarFrameSetInfo 
VMCv20130805 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks 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. 
ksaStratAst 
vmcVarFrameSetInfo 
VMCv20140428 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
ksaStratAst 
vmcVarFrameSetInfo 
VMCv20140903 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
ksaStratAst 
vmcVarFrameSetInfo 
VMCv20150309 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
ksaStratAst 
vmcVarFrameSetInfo 
VMCv20151218 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
ksaStratAst 
vmcVarFrameSetInfo 
VMCv20160311 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
ksaStratAst 
vmcVarFrameSetInfo 
VMCv20160822 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
ksaStratAst 
vmcVarFrameSetInfo 
VMCv20170109 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
ksaStratAst 
vmcVarFrameSetInfo 
VMCv20170411 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
ksaStratAst 
vmcVarFrameSetInfo 
VMCv20171101 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
ksaStratAst 
vmcVarFrameSetInfo 
VMCv20180702 
Parameter, c0 from FerreiraLopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Ks band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
ksaStratAst 
vmcVarFrameSetInfo 
VMCv20181120 
Parameter, c0 from FerreiraLopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Ks band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
ksaStratAst 
vvvVarFrameSetInfo 
VVVDR4 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
ksaStratPht 
videoVarFrameSetInfo 
VIDEODR2 
Strateva parameter, a, in fit to photometric rms vs magnitude in Ks 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. 
ksaStratPht 
videoVarFrameSetInfo 
VIDEODR3 
Strateva parameter, a, in fit to photometric rms vs magnitude in Ks 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. 
ksaStratPht 
videoVarFrameSetInfo 
VIDEODR4 
Strateva parameter, a, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
ksaStratPht 
videoVarFrameSetInfo 
VIDEODR5 
Strateva parameter, a, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
ksaStratPht 
videoVarFrameSetInfo 
VIDEOv20100513 
Strateva parameter, a, in fit to photometric rms vs magnitude in Ks 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. 
ksaStratPht 
videoVarFrameSetInfo 
VIDEOv20111208 
Strateva parameter, a, in fit to photometric rms vs magnitude in Ks 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. 
ksaStratPht 
vikingVarFrameSetInfo 
VIKINGDR2 
Strateva parameter, a, in fit to photometric rms vs magnitude in Ks 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. 
ksaStratPht 
vikingVarFrameSetInfo 
VIKINGv20110714 
Strateva parameter, a, in fit to photometric rms vs magnitude in Ks 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. 
ksaStratPht 
vikingVarFrameSetInfo 
VIKINGv20111019 
Strateva parameter, a, in fit to photometric rms vs magnitude in Ks 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. 
ksaStratPht 
vmcVarFrameSetInfo 
VMCDR1 
Strateva parameter, a, in fit to photometric rms vs magnitude in Ks 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. 
ksaStratPht 
vmcVarFrameSetInfo 
VMCDR2 
Strateva parameter, a, in fit to photometric rms vs magnitude in Ks 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. 
ksaStratPht 
vmcVarFrameSetInfo 
VMCDR3 
Strateva parameter, a, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
ksaStratPht 
vmcVarFrameSetInfo 
VMCDR4 
Strateva parameter, a, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
ksaStratPht 
vmcVarFrameSetInfo 
VMCv20110816 
Strateva parameter, a, in fit to photometric rms vs magnitude in Ks 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. 
ksaStratPht 
vmcVarFrameSetInfo 
VMCv20110909 
Strateva parameter, a, in fit to photometric rms vs magnitude in Ks 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. 
ksaStratPht 
vmcVarFrameSetInfo 
VMCv20120126 
Strateva parameter, a, in fit to photometric rms vs magnitude in Ks 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. 
ksaStratPht 
vmcVarFrameSetInfo 
VMCv20121128 
Strateva parameter, a, in fit to photometric rms vs magnitude in Ks 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. 
ksaStratPht 
vmcVarFrameSetInfo 
VMCv20130304 
Strateva parameter, a, in fit to photometric rms vs magnitude in Ks 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. 
ksaStratPht 
vmcVarFrameSetInfo 
VMCv20130805 
Strateva parameter, a, in fit to photometric rms vs magnitude in Ks 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. 
ksaStratPht 
vmcVarFrameSetInfo 
VMCv20140428 
Strateva parameter, a, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
ksaStratPht 
vmcVarFrameSetInfo 
VMCv20140903 
Strateva parameter, a, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
ksaStratPht 
vmcVarFrameSetInfo 
VMCv20150309 
Strateva parameter, a, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
ksaStratPht 
vmcVarFrameSetInfo 
VMCv20151218 
Strateva parameter, a, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
ksaStratPht 
vmcVarFrameSetInfo 
VMCv20160311 
Strateva parameter, a, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
ksaStratPht 
vmcVarFrameSetInfo 
VMCv20160822 
Strateva parameter, a, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
ksaStratPht 
vmcVarFrameSetInfo 
VMCv20170109 
Strateva parameter, a, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
ksaStratPht 
vmcVarFrameSetInfo 
VMCv20170411 
Strateva parameter, a, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
ksaStratPht 
vmcVarFrameSetInfo 
VMCv20171101 
Strateva parameter, a, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
ksaStratPht 
vmcVarFrameSetInfo 
VMCv20180702 
Parameter, c0 from FerreiraLopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Ks band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
ksaStratPht 
vmcVarFrameSetInfo 
VMCv20181120 
Parameter, c0 from FerreiraLopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Ks band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
ksaStratPht 
vvvVarFrameSetInfo 
VVVDR4 
Strateva parameter, a, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
ksAverageConf 
vhsSource 
VHSDR1 
average confidence in 2 arcsec diameter default aperture (aper3) Ks 
real 
4 

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

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

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

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

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

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

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

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

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

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

0.9999995e9 
stat.likelihood;em.IR.K 
ksAverageConf 
vhsSource 
VHSv20171207 
average confidence in 2 arcsec diameter default aperture (aper3) Ks 
real 
4 

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

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

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

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

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

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

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

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

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

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

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

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

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

0.9999995e9 
stat.likelihood;em.IR.K 
ksAverageConf 
vikingSource 
VIKINGv20181012 
average confidence in 2 arcsec diameter default aperture (aper3) Ks 
real 
4 

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

99999999 
meta.code 
ksAverageConf 
vvvSource, vvvSynopticSource 
VVVDR4 
average confidence in 2 arcsec diameter default aperture (aper3) Ks 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.K 
ksbestAper 
videoVariability 
VIDEODR2 
Best aperture (16) for photometric statistics in the Ks 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) 
ksbestAper 
videoVariability 
VIDEODR3 
Best aperture (16) for photometric statistics in the Ks 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) 
ksbestAper 
videoVariability 
VIDEODR4 
Best aperture (16) for photometric statistics in the Ks band 
int 
4 

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

9999 
meta.code.class;em.IR.K 
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) 
ksbestAper 
videoVariability 
VIDEOv20100513 
Best aperture (16) for photometric statistics in the Ks 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) 
ksbestAper 
videoVariability 
VIDEOv20111208 
Best aperture (16) for photometric statistics in the Ks 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) 
ksbestAper 
vikingVariability 
VIKINGDR2 
Best aperture (16) for photometric statistics in the Ks 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) 
ksbestAper 
vikingVariability 
VIKINGv20110714 
Best aperture (16) for photometric statistics in the Ks 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) 
ksbestAper 
vikingVariability 
VIKINGv20111019 
Best aperture (16) for photometric statistics in the Ks 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) 
ksbestAper 
vmcVariability 
VMCDR1 
Best aperture (16) for photometric statistics in the Ks 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) 
ksbestAper 
vmcVariability 
VMCDR2 
Best aperture (16) for photometric statistics in the Ks 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) 
ksbestAper 
vmcVariability 
VMCDR3 
Best aperture (16) for photometric statistics in the Ks band 
int 
4 

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

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

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

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

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

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

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

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

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

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

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

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

9999 
meta.code.class;em.IR.K 
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) 
ksbestAper 
vvvVariability 
VVVDR4 
Best aperture (16) for photometric statistics in the Ks band 
int 
4 

9999 
meta.code.class;em.IR.K 
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) 
ksbStratAst 
videoVarFrameSetInfo 
VIDEODR2 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks 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. 
ksbStratAst 
videoVarFrameSetInfo 
VIDEODR3 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks 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. 
ksbStratAst 
videoVarFrameSetInfo 
VIDEODR4 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
ksbStratAst 
videoVarFrameSetInfo 
VIDEODR5 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
ksbStratAst 
videoVarFrameSetInfo 
VIDEOv20100513 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks 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. 
ksbStratAst 
videoVarFrameSetInfo 
VIDEOv20111208 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks 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. 
ksbStratAst 
vikingVarFrameSetInfo 
VIKINGDR2 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks 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. 
ksbStratAst 
vikingVarFrameSetInfo 
VIKINGv20110714 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks 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. 
ksbStratAst 
vikingVarFrameSetInfo 
VIKINGv20111019 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks 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. 
ksbStratAst 
vmcVarFrameSetInfo 
VMCDR1 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks 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. 
ksbStratAst 
vmcVarFrameSetInfo 
VMCDR2 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks 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. 
ksbStratAst 
vmcVarFrameSetInfo 
VMCDR3 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
ksbStratAst 
vmcVarFrameSetInfo 
VMCDR4 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
ksbStratAst 
vmcVarFrameSetInfo 
VMCv20110816 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks 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. 
ksbStratAst 
vmcVarFrameSetInfo 
VMCv20110909 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks 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. 
ksbStratAst 
vmcVarFrameSetInfo 
VMCv20120126 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks 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. 
ksbStratAst 
vmcVarFrameSetInfo 
VMCv20121128 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks 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. 
ksbStratAst 
vmcVarFrameSetInfo 
VMCv20130304 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks 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. 
ksbStratAst 
vmcVarFrameSetInfo 
VMCv20130805 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks 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. 
ksbStratAst 
vmcVarFrameSetInfo 
VMCv20140428 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
ksbStratAst 
vmcVarFrameSetInfo 
VMCv20140903 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
ksbStratAst 
vmcVarFrameSetInfo 
VMCv20150309 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
ksbStratAst 
vmcVarFrameSetInfo 
VMCv20151218 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
ksbStratAst 
vmcVarFrameSetInfo 
VMCv20160311 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
ksbStratAst 
vmcVarFrameSetInfo 
VMCv20160822 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
ksbStratAst 
vmcVarFrameSetInfo 
VMCv20170109 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
ksbStratAst 
vmcVarFrameSetInfo 
VMCv20170411 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
ksbStratAst 
vmcVarFrameSetInfo 
VMCv20171101 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
ksbStratAst 
vmcVarFrameSetInfo 
VMCv20180702 
Parameter, c1 from FerreiraLopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Ks band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
ksbStratAst 
vmcVarFrameSetInfo 
VMCv20181120 
Parameter, c1 from FerreiraLopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Ks band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
ksbStratAst 
vvvVarFrameSetInfo 
VVVDR4 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
ksbStratPht 
videoVarFrameSetInfo 
VIDEODR2 
Strateva parameter, b, in fit to photometric rms vs magnitude in Ks 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. 
ksbStratPht 
videoVarFrameSetInfo 
VIDEODR3 
Strateva parameter, b, in fit to photometric rms vs magnitude in Ks 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. 
ksbStratPht 
videoVarFrameSetInfo 
VIDEODR4 
Strateva parameter, b, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
ksbStratPht 
videoVarFrameSetInfo 
VIDEODR5 
Strateva parameter, b, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
ksbStratPht 
videoVarFrameSetInfo 
VIDEOv20100513 
Strateva parameter, b, in fit to photometric rms vs magnitude in Ks 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. 
ksbStratPht 
videoVarFrameSetInfo 
VIDEOv20111208 
Strateva parameter, b, in fit to photometric rms vs magnitude in Ks 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. 
ksbStratPht 
vikingVarFrameSetInfo 
VIKINGDR2 
Strateva parameter, b, in fit to photometric rms vs magnitude in Ks 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. 
ksbStratPht 
vikingVarFrameSetInfo 
VIKINGv20110714 
Strateva parameter, b, in fit to photometric rms vs magnitude in Ks 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. 
ksbStratPht 
vikingVarFrameSetInfo 
VIKINGv20111019 
Strateva parameter, b, in fit to photometric rms vs magnitude in Ks 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. 
ksbStratPht 
vmcVarFrameSetInfo 
VMCDR1 
Strateva parameter, b, in fit to photometric rms vs magnitude in Ks 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. 
ksbStratPht 
vmcVarFrameSetInfo 
VMCDR2 
Strateva parameter, b, in fit to photometric rms vs magnitude in Ks 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. 
ksbStratPht 
vmcVarFrameSetInfo 
VMCDR3 
Strateva parameter, b, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
ksbStratPht 
vmcVarFrameSetInfo 
VMCDR4 
Strateva parameter, b, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
ksbStratPht 
vmcVarFrameSetInfo 
VMCv20110816 
Strateva parameter, b, in fit to photometric rms vs magnitude in Ks 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. 
ksbStratPht 
vmcVarFrameSetInfo 
VMCv20110909 
Strateva parameter, b, in fit to photometric rms vs magnitude in Ks 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. 
ksbStratPht 
vmcVarFrameSetInfo 
VMCv20120126 
Strateva parameter, b, in fit to photometric rms vs magnitude in Ks 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. 
ksbStratPht 
vmcVarFrameSetInfo 
VMCv20121128 
Strateva parameter, b, in fit to photometric rms vs magnitude in Ks 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. 
ksbStratPht 
vmcVarFrameSetInfo 
VMCv20130304 
Strateva parameter, b, in fit to photometric rms vs magnitude in Ks 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. 
ksbStratPht 
vmcVarFrameSetInfo 
VMCv20130805 
Strateva parameter, b, in fit to photometric rms vs magnitude in Ks 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. 
ksbStratPht 
vmcVarFrameSetInfo 
VMCv20140428 
Strateva parameter, b, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
ksbStratPht 
vmcVarFrameSetInfo 
VMCv20140903 
Strateva parameter, b, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
ksbStratPht 
vmcVarFrameSetInfo 
VMCv20150309 
Strateva parameter, b, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
ksbStratPht 
vmcVarFrameSetInfo 
VMCv20151218 
Strateva parameter, b, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
ksbStratPht 
vmcVarFrameSetInfo 
VMCv20160311 
Strateva parameter, b, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
ksbStratPht 
vmcVarFrameSetInfo 
VMCv20160822 
Strateva parameter, b, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
ksbStratPht 
vmcVarFrameSetInfo 
VMCv20170109 
Strateva parameter, b, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
ksbStratPht 
vmcVarFrameSetInfo 
VMCv20170411 
Strateva parameter, b, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
ksbStratPht 
vmcVarFrameSetInfo 
VMCv20171101 
Strateva parameter, b, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
ksbStratPht 
vmcVarFrameSetInfo 
VMCv20180702 
Parameter, c1 from FerreiraLopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Ks band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
ksbStratPht 
vmcVarFrameSetInfo 
VMCv20181120 
Parameter, c1 from FerreiraLopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Ks band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
ksbStratPht 
vvvVarFrameSetInfo 
VVVDR4 
Strateva parameter, b, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
kschiSqAst 
videoVarFrameSetInfo 
VIDEODR2 
Goodness of fit of Strateva function to astrometric data in Ks 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. 
kschiSqAst 
videoVarFrameSetInfo 
VIDEODR3 
Goodness of fit of Strateva function to astrometric data in Ks 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. 
kschiSqAst 
videoVarFrameSetInfo 
VIDEODR4 
Goodness of fit of Strateva function to astrometric data in Ks band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
kschiSqAst 
videoVarFrameSetInfo 
VIDEODR5 
Goodness of fit of Strateva function to astrometric data in Ks band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
kschiSqAst 
videoVarFrameSetInfo 
VIDEOv20100513 
Goodness of fit of Strateva function to astrometric data in Ks 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. 
kschiSqAst 
videoVarFrameSetInfo 
VIDEOv20111208 
Goodness of fit of Strateva function to astrometric data in Ks 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. 
kschiSqAst 
vikingVarFrameSetInfo 
VIKINGDR2 
Goodness of fit of Strateva function to astrometric data in Ks 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. 
kschiSqAst 
vikingVarFrameSetInfo 
VIKINGv20110714 
Goodness of fit of Strateva function to astrometric data in Ks 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. 
kschiSqAst 
vikingVarFrameSetInfo 
VIKINGv20111019 
Goodness of fit of Strateva function to astrometric data in Ks 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. 
kschiSqAst 
vmcVarFrameSetInfo 
VMCDR1 
Goodness of fit of Strateva function to astrometric data in Ks 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. 
kschiSqAst 
vmcVarFrameSetInfo 
VMCDR2 
Goodness of fit of Strateva function to astrometric data in Ks 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. 
kschiSqAst 
vmcVarFrameSetInfo 
VMCDR3 
Goodness of fit of Strateva function to astrometric data in Ks band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
kschiSqAst 
vmcVarFrameSetInfo 
VMCDR4 
Goodness of fit of Strateva function to astrometric data in Ks band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
kschiSqAst 
vmcVarFrameSetInfo 
VMCv20110816 
Goodness of fit of Strateva function to astrometric data in Ks 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. 
kschiSqAst 
vmcVarFrameSetInfo 
VMCv20110909 
Goodness of fit of Strateva function to astrometric data in Ks 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. 
kschiSqAst 
vmcVarFrameSetInfo 
VMCv20120126 
Goodness of fit of Strateva function to astrometric data in Ks 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. 
kschiSqAst 
vmcVarFrameSetInfo 
VMCv20121128 
Goodness of fit of Strateva function to astrometric data in Ks 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. 
kschiSqAst 
vmcVarFrameSetInfo 
VMCv20130304 
Goodness of fit of Strateva function to astrometric data in Ks 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. 
kschiSqAst 
vmcVarFrameSetInfo 
VMCv20130805 
Goodness of fit of Strateva function to astrometric data in Ks 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. 
kschiSqAst 
vmcVarFrameSetInfo 
VMCv20140428 
Goodness of fit of Strateva function to astrometric data in Ks band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
kschiSqAst 
vmcVarFrameSetInfo 
VMCv20140903 
Goodness of fit of Strateva function to astrometric data in Ks band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
kschiSqAst 
vmcVarFrameSetInfo 
VMCv20150309 
Goodness of fit of Strateva function to astrometric data in Ks band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
kschiSqAst 
vmcVarFrameSetInfo 
VMCv20151218 
Goodness of fit of Strateva function to astrometric data in Ks band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
kschiSqAst 
vmcVarFrameSetInfo 
VMCv20160311 
Goodness of fit of Strateva function to astrometric data in Ks band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
kschiSqAst 
vmcVarFrameSetInfo 
VMCv20160822 
Goodness of fit of Strateva function to astrometric data in Ks band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
kschiSqAst 
vmcVarFrameSetInfo 
VMCv20170109 
Goodness of fit of Strateva function to astrometric data in Ks band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
kschiSqAst 
vmcVarFrameSetInfo 
VMCv20170411 
Goodness of fit of Strateva function to astrometric data in Ks band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
kschiSqAst 
vmcVarFrameSetInfo 
VMCv20171101 
Goodness of fit of Strateva function to astrometric data in Ks band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
kschiSqAst 
vmcVarFrameSetInfo 
VMCv20180702 
Goodness of fit of Strateva function to astrometric data in Ks band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
kschiSqAst 
vmcVarFrameSetInfo 
VMCv20181120 
Goodness of fit of Strateva function to astrometric data in Ks band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
kschiSqAst 
vvvVarFrameSetInfo 
VVVDR4 
Goodness of fit of Strateva function to astrometric data in Ks band 
real 
4 

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

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

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

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
kschiSqpd 
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. 
kschiSqpd 
vikingVariability 
VIKINGDR2 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
kschiSqpd 
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. 
kschiSqpd 
vikingVariability 
VIKINGv20111019 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
kschiSqpd 
vmcVariability 
VMCDR1 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
kschiSqpd 
vmcVariability 
VMCDR2 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
kschiSqpd 
vmcVariability 
VMCDR3 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

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

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

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
kschiSqpd 
vmcVariability 
VMCv20110909 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
kschiSqpd 
vmcVariability 
VMCv20120126 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
kschiSqpd 
vmcVariability 
VMCv20121128 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
kschiSqpd 
vmcVariability 
VMCv20130304 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
kschiSqpd 
vmcVariability 
VMCv20130805 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
kschiSqpd 
vmcVariability 
VMCv20140428 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

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

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

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

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

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

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

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

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

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

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

0.9999995e9 
stat.fit.chi2;em.IR.K 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This 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. 
kschiSqpd 
vvvVariability 
VVVDR4 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2;em.IR.K 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This 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. 
kschiSqPht 
videoVarFrameSetInfo 
VIDEODR2 
Goodness of fit of Strateva function to photometric data in Ks 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. 
kschiSqPht 
videoVarFrameSetInfo 
VIDEODR3 
Goodness of fit of Strateva function to photometric data in Ks 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. 
kschiSqPht 
videoVarFrameSetInfo 
VIDEODR4 
Goodness of fit of Strateva function to photometric data in Ks band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
kschiSqPht 
videoVarFrameSetInfo 
VIDEODR5 
Goodness of fit of Strateva function to photometric data in Ks band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
kschiSqPht 
videoVarFrameSetInfo 
VIDEOv20100513 
Goodness of fit of Strateva function to photometric data in Ks 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. 
kschiSqPht 
videoVarFrameSetInfo 
VIDEOv20111208 
Goodness of fit of Strateva function to photometric data in Ks 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. 
kschiSqPht 
vikingVarFrameSetInfo 
VIKINGDR2 
Goodness of fit of Strateva function to photometric data in Ks 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. 
kschiSqPht 
vikingVarFrameSetInfo 
VIKINGv20110714 
Goodness of fit of Strateva function to photometric data in Ks 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. 
kschiSqPht 
vikingVarFrameSetInfo 
VIKINGv20111019 
Goodness of fit of Strateva function to photometric data in Ks 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. 
kschiSqPht 
vmcVarFrameSetInfo 
VMCDR1 
Goodness of fit of Strateva function to photometric data in Ks 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. 
kschiSqPht 
vmcVarFrameSetInfo 
VMCDR2 
Goodness of fit of Strateva function to photometric data in Ks 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. 
kschiSqPht 
vmcVarFrameSetInfo 
VMCDR3 
Goodness of fit of Strateva function to photometric data in Ks band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
kschiSqPht 
vmcVarFrameSetInfo 
VMCDR4 
Goodness of fit of Strateva function to photometric data in Ks band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
kschiSqPht 
vmcVarFrameSetInfo 
VMCv20110816 
Goodness of fit of Strateva function to photometric data in Ks 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. 
kschiSqPht 
vmcVarFrameSetInfo 
VMCv20110909 
Goodness of fit of Strateva function to photometric data in Ks 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. 
kschiSqPht 
vmcVarFrameSetInfo 
VMCv20120126 
Goodness of fit of Strateva function to photometric data in Ks 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. 
kschiSqPht 
vmcVarFrameSetInfo 
VMCv20121128 
Goodness of fit of Strateva function to photometric data in Ks 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. 
kschiSqPht 
vmcVarFrameSetInfo 
VMCv20130304 
Goodness of fit of Strateva function to photometric data in Ks 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. 
kschiSqPht 
vmcVarFrameSetInfo 
VMCv20130805 
Goodness of fit of Strateva function to photometric data in Ks 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. 
kschiSqPht 
vmcVarFrameSetInfo 
VMCv20140428 
Goodness of fit of Strateva function to photometric data in Ks band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
kschiSqPht 
vmcVarFrameSetInfo 
VMCv20140903 
Goodness of fit of Strateva function to photometric data in Ks band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
kschiSqPht 
vmcVarFrameSetInfo 
VMCv20150309 
Goodness of fit of Strateva function to photometric data in Ks band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
kschiSqPht 
vmcVarFrameSetInfo 
VMCv20151218 
Goodness of fit of Strateva function to photometric data in Ks band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
kschiSqPht 
vmcVarFrameSetInfo 
VMCv20160311 
Goodness of fit of Strateva function to photometric data in Ks band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
kschiSqPht 
vmcVarFrameSetInfo 
VMCv20160822 
Goodness of fit of Strateva function to photometric data in Ks band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
kschiSqPht 
vmcVarFrameSetInfo 
VMCv20170109 
Goodness of fit of Strateva function to photometric data in Ks band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
kschiSqPht 
vmcVarFrameSetInfo 
VMCv20170411 
Goodness of fit of Strateva function to photometric data in Ks band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
kschiSqPht 
vmcVarFrameSetInfo 
VMCv20171101 
Goodness of fit of Strateva function to photometric data in Ks band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
kschiSqPht 
vmcVarFrameSetInfo 
VMCv20180702 
Goodness of fit of Strateva function to photometric data in Ks band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
kschiSqPht 
vmcVarFrameSetInfo 
VMCv20181120 
Goodness of fit of Strateva function to photometric data in Ks band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
kschiSqPht 
vvvVarFrameSetInfo 
VVVDR4 
Goodness of fit of Strateva function to photometric data in Ks band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
ksClass 
vhsSource 
VHSDR2 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class 
ksClass 
vhsSource 
VHSDR3 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class;em.IR.K 
ksClass 
vhsSource 
VHSDR4 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class;em.IR.K 
ksClass 
vhsSource 
VHSv20120926 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class 
ksClass 
vhsSource 
VHSv20130417 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class 
ksClass 
vhsSource 
VHSv20140409 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class;em.IR.K 
ksClass 
vhsSource 
VHSv20150108 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class;em.IR.K 
ksClass 
vhsSource 
VHSv20160114 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class;em.IR.K 
ksClass 
vhsSource 
VHSv20160507 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class;em.IR.K 
ksClass 
vhsSource 
VHSv20170630 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class;em.IR.K 
ksClass 
vhsSource 
VHSv20171207 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class;em.IR.K 
ksClass 
vhsSource 
VHSv20180419 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class;em.IR.K 
ksClass 
vhsSource, vhsSourceRemeasurement 
VHSDR1 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class 
ksClass 
videoSource 
VIDEODR2 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class 
ksClass 
videoSource 
VIDEODR3 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class 
ksClass 
videoSource 
VIDEODR4 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class;em.IR.K 
ksClass 
videoSource 
VIDEODR5 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class;em.IR.K 
ksClass 
videoSource 
VIDEOv20111208 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class 
ksClass 
videoSource, videoSourceRemeasurement 
VIDEOv20100513 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class 
ksClass 
vikingSource 
VIKINGDR2 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class 
ksClass 
vikingSource 
VIKINGDR3 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class 
ksClass 
vikingSource 
VIKINGDR4 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class;em.IR.K 
ksClass 
vikingSource 
VIKINGv20111019 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class 
ksClass 
vikingSource 
VIKINGv20130417 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class 
ksClass 
vikingSource 
VIKINGv20140402 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class 
ksClass 
vikingSource 
VIKINGv20150421 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class;em.IR.K 
ksClass 
vikingSource 
VIKINGv20151230 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class;em.IR.K 
ksClass 
vikingSource 
VIKINGv20160406 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class;em.IR.K 
ksClass 
vikingSource 
VIKINGv20161202 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class;em.IR.K 
ksClass 
vikingSource 
VIKINGv20170715 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class;em.IR.K 
ksClass 
vikingSource 
VIKINGv20181012 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class;em.IR.K 
ksClass 
vikingSource, vikingSourceRemeasurement 
VIKINGv20110714 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class 
ksClass 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class 
ksClass 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class 
ksClass 
vmcSource 
VMCDR2 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class 
ksClass 
vmcSource 
VMCDR3 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class;em.IR.K 
ksClass 
vmcSource 
VMCDR4 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class;em.IR.K 
ksClass 
vmcSource 
VMCv20110909 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class 
ksClass 
vmcSource 
VMCv20120126 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class 
ksClass 
vmcSource 
VMCv20121128 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class 
ksClass 
vmcSource 
VMCv20130304 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class 
ksClass 
vmcSource 
VMCv20130805 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class 
ksClass 
vmcSource 
VMCv20140428 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class;em.IR.K 
ksClass 
vmcSource 
VMCv20140903 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class;em.IR.K 
ksClass 
vmcSource 
VMCv20150309 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class;em.IR.K 
ksClass 
vmcSource 
VMCv20151218 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class;em.IR.K 
ksClass 
vmcSource 
VMCv20160311 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class;em.IR.K 
ksClass 
vmcSource 
VMCv20160822 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class;em.IR.K 
ksClass 
vmcSource 
VMCv20170109 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class;em.IR.K 
ksClass 
vmcSource 
VMCv20170411 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class;em.IR.K 
ksClass 
vmcSource 
VMCv20171101 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class;em.IR.K 
ksClass 
vmcSource 
VMCv20180702 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class;em.IR.K 
ksClass 
vmcSource 
VMCv20181120 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class;em.IR.K 
ksClass 
vmcSource, vmcSourceRemeasurement 
VMCv20110816 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class 
ksClass 
vmcSource, vmcSynopticSource 
VMCDR1 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class 
ksClass 
vvvSource, vvvSynopticSource 
VVVDR4 
discrete image classification flag in Ks 
smallint 
2 

9999 
src.class;em.IR.K 
ksClassStat 
vhsSource 
VHSDR2 
N(0,1) stellarnessofprofile statistic in Ks 
real 
4 

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

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

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

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

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

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

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

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

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

0.9999995e9 
stat;em.IR.K 
ksClassStat 
vhsSource 
VHSv20171207 
N(0,1) stellarnessofprofile statistic in Ks 
real 
4 

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

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

0.9999995e9 
stat 
ksClassStat 
videoSource 
VIDEODR2 
SExtractor classification statistic in Ks 
real 
4 

0.9999995e9 
stat 
ksClassStat 
videoSource 
VIDEODR3 
SExtractor classification statistic in Ks 
real 
4 

0.9999995e9 
stat 
ksClassStat 
videoSource 
VIDEODR4 
SExtractor classification statistic in Ks 
real 
4 

0.9999995e9 
stat;em.IR.K 
ksClassStat 
videoSource 
VIDEODR5 
SExtractor classification statistic in Ks 
real 
4 

0.9999995e9 
stat;em.IR.K 
ksClassStat 
videoSource 
VIDEOv20100513 
SExtractor classification statistic in Ks 
real 
4 

0.9999995e9 
stat 
ksClassStat 
videoSource 
VIDEOv20111208 
SExtractor classification statistic in Ks 
real 
4 

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

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

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

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

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

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

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

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

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

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

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

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

0.9999995e9 
stat;em.IR.K 
ksClassStat 
vikingSource 
VIKINGv20181012 
N(0,1) stellarnessofprofile statistic in Ks 
real 
4 

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

0.9999995e9 
stat 
ksClassStat 
vvvSource 
VVVDR4 
SExtractor classification statistic in Ks 
real 
4 

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

0.9999995e9 
stat;em.IR.K 
kscStratAst 
videoVarFrameSetInfo 
VIDEODR2 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks 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. 
kscStratAst 
videoVarFrameSetInfo 
VIDEODR3 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks 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. 
kscStratAst 
videoVarFrameSetInfo 
VIDEODR4 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
kscStratAst 
videoVarFrameSetInfo 
VIDEODR5 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
kscStratAst 
videoVarFrameSetInfo 
VIDEOv20100513 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks 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. 
kscStratAst 
videoVarFrameSetInfo 
VIDEOv20111208 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks 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. 
kscStratAst 
vikingVarFrameSetInfo 
VIKINGDR2 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks 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. 
kscStratAst 
vikingVarFrameSetInfo 
VIKINGv20110714 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks 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. 
kscStratAst 
vikingVarFrameSetInfo 
VIKINGv20111019 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks 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. 
kscStratAst 
vmcVarFrameSetInfo 
VMCDR1 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks 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. 
kscStratAst 
vmcVarFrameSetInfo 
VMCDR2 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks 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. 
kscStratAst 
vmcVarFrameSetInfo 
VMCDR3 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
kscStratAst 
vmcVarFrameSetInfo 
VMCDR4 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
kscStratAst 
vmcVarFrameSetInfo 
VMCv20110816 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks 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. 
kscStratAst 
vmcVarFrameSetInfo 
VMCv20110909 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks 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. 
kscStratAst 
vmcVarFrameSetInfo 
VMCv20120126 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks 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. 
kscStratAst 
vmcVarFrameSetInfo 
VMCv20121128 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks 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. 
kscStratAst 
vmcVarFrameSetInfo 
VMCv20130304 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks 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. 
kscStratAst 
vmcVarFrameSetInfo 
VMCv20130805 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks 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. 
kscStratAst 
vmcVarFrameSetInfo 
VMCv20140428 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
kscStratAst 
vmcVarFrameSetInfo 
VMCv20140903 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
kscStratAst 
vmcVarFrameSetInfo 
VMCv20150309 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
kscStratAst 
vmcVarFrameSetInfo 
VMCv20151218 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
kscStratAst 
vmcVarFrameSetInfo 
VMCv20160311 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
kscStratAst 
vmcVarFrameSetInfo 
VMCv20160822 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
kscStratAst 
vmcVarFrameSetInfo 
VMCv20170109 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
kscStratAst 
vmcVarFrameSetInfo 
VMCv20170411 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
kscStratAst 
vmcVarFrameSetInfo 
VMCv20171101 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
kscStratAst 
vmcVarFrameSetInfo 
VMCv20180702 
Parameter, c2 from FerreiraLopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Ks band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
kscStratAst 
vmcVarFrameSetInfo 
VMCv20181120 
Parameter, c2 from FerreiraLopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Ks band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
kscStratAst 
vvvVarFrameSetInfo 
VVVDR4 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
kscStratPht 
videoVarFrameSetInfo 
VIDEODR2 
Strateva parameter, c, in fit to photometric rms vs magnitude in Ks 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. 
kscStratPht 
videoVarFrameSetInfo 
VIDEODR3 
Strateva parameter, c, in fit to photometric rms vs magnitude in Ks 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. 
kscStratPht 
videoVarFrameSetInfo 
VIDEODR4 
Strateva parameter, c, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
kscStratPht 
videoVarFrameSetInfo 
VIDEODR5 
Strateva parameter, c, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
kscStratPht 
videoVarFrameSetInfo 
VIDEOv20100513 
Strateva parameter, c, in fit to photometric rms vs magnitude in Ks 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. 
kscStratPht 
videoVarFrameSetInfo 
VIDEOv20111208 
Strateva parameter, c, in fit to photometric rms vs magnitude in Ks 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. 
kscStratPht 
vikingVarFrameSetInfo 
VIKINGDR2 
Strateva parameter, c, in fit to photometric rms vs magnitude in Ks 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. 
kscStratPht 
vikingVarFrameSetInfo 
VIKINGv20110714 
Strateva parameter, c, in fit to photometric rms vs magnitude in Ks 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. 
kscStratPht 
vikingVarFrameSetInfo 
VIKINGv20111019 
Strateva parameter, c, in fit to photometric rms vs magnitude in Ks 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. 
kscStratPht 
vmcVarFrameSetInfo 
VMCDR1 
Strateva parameter, c, in fit to photometric rms vs magnitude in Ks 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. 
kscStratPht 
vmcVarFrameSetInfo 
VMCDR2 
Strateva parameter, c, in fit to photometric rms vs magnitude in Ks 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. 
kscStratPht 
vmcVarFrameSetInfo 
VMCDR3 
Strateva parameter, c, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
kscStratPht 
vmcVarFrameSetInfo 
VMCDR4 
Strateva parameter, c, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
kscStratPht 
vmcVarFrameSetInfo 
VMCv20110816 
Strateva parameter, c, in fit to photometric rms vs magnitude in Ks 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. 
kscStratPht 
vmcVarFrameSetInfo 
VMCv20110909 
Strateva parameter, c, in fit to photometric rms vs magnitude in Ks 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. 
kscStratPht 
vmcVarFrameSetInfo 
VMCv20120126 
Strateva parameter, c, in fit to photometric rms vs magnitude in Ks 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. 
kscStratPht 
vmcVarFrameSetInfo 
VMCv20121128 
Strateva parameter, c, in fit to photometric rms vs magnitude in Ks 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. 
kscStratPht 
vmcVarFrameSetInfo 
VMCv20130304 
Strateva parameter, c, in fit to photometric rms vs magnitude in Ks 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. 
kscStratPht 
vmcVarFrameSetInfo 
VMCv20130805 
Strateva parameter, c, in fit to photometric rms vs magnitude in Ks 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. 
kscStratPht 
vmcVarFrameSetInfo 
VMCv20140428 
Strateva parameter, c, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
kscStratPht 
vmcVarFrameSetInfo 
VMCv20140903 
Strateva parameter, c, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
kscStratPht 
vmcVarFrameSetInfo 
VMCv20150309 
Strateva parameter, c, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
kscStratPht 
vmcVarFrameSetInfo 
VMCv20151218 
Strateva parameter, c, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
kscStratPht 
vmcVarFrameSetInfo 
VMCv20160311 
Strateva parameter, c, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
kscStratPht 
vmcVarFrameSetInfo 
VMCv20160822 
Strateva parameter, c, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
kscStratPht 
vmcVarFrameSetInfo 
VMCv20170109 
Strateva parameter, c, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
kscStratPht 
vmcVarFrameSetInfo 
VMCv20170411 
Strateva parameter, c, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
kscStratPht 
vmcVarFrameSetInfo 
VMCv20171101 
Strateva parameter, c, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
kscStratPht 
vmcVarFrameSetInfo 
VMCv20180702 
Parameter, c2 from FerreiraLopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Ks band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
kscStratPht 
vmcVarFrameSetInfo 
VMCv20181120 
Parameter, c2 from FerreiraLopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Ks band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
kscStratPht 
vvvVarFrameSetInfo 
VVVDR4 
Strateva parameter, c, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.K 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was 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. 
ksDeblend 
vhsSourceRemeasurement 
VHSDR1 
placeholder flag indicating parent/child relation in Ks 
int 
4 

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

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

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

99999999 
meta.code 
ksDeblend 
vmcSourceRemeasurement 
VMCv20110816 
placeholder flag indicating parent/child relation in Ks 
int 
4 

99999999 
meta.code 
ksDeblend 
vmcSourceRemeasurement 
VMCv20110909 
placeholder flag indicating parent/child relation in Ks 
int 
4 

99999999 
meta.code 
ksEll 
vhsSource 
VHSDR2 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity 
ksEll 
vhsSource 
VHSDR3 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.K 
ksEll 
vhsSource 
VHSDR4 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.K 
ksEll 
vhsSource 
VHSv20120926 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity 
ksEll 
vhsSource 
VHSv20130417 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity 
ksEll 
vhsSource 
VHSv20140409 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.K 
ksEll 
vhsSource 
VHSv20150108 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.K 
ksEll 
vhsSource 
VHSv20160114 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.K 
ksEll 
vhsSource 
VHSv20160507 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.K 
ksEll 
vhsSource 
VHSv20170630 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.K 
ksEll 
vhsSource 
VHSv20171207 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.K 
ksEll 
vhsSource 
VHSv20180419 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.K 
ksEll 
vhsSource, vhsSourceRemeasurement 
VHSDR1 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

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

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

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

0.9999995e9 
src.ellipticity;em.IR.K 
ksEll 
videoSource 
VIDEODR5 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.K 
ksEll 
videoSource 
VIDEOv20111208 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

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

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

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

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

0.9999995e9 
src.ellipticity;em.IR.K 
ksEll 
vikingSource 
VIKINGv20111019 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

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

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

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

0.9999995e9 
src.ellipticity;em.IR.K 
ksEll 
vikingSource 
VIKINGv20151230 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.K 
ksEll 
vikingSource 
VIKINGv20160406 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.K 
ksEll 
vikingSource 
VIKINGv20161202 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.K 
ksEll 
vikingSource 
VIKINGv20170715 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.K 
ksEll 
vikingSource 
VIKINGv20181012 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.K 
ksEll 
vikingSource, vikingSourceRemeasurement 
VIKINGv20110714 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

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

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

0.9999995e9 
src.ellipticity 
ksEll 
vmcSource 
VMCDR2 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity 
ksEll 
vmcSource 
VMCDR3 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.K 
ksEll 
vmcSource 
VMCDR4 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.K 
ksEll 
vmcSource 
VMCv20110909 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity 
ksEll 
vmcSource 
VMCv20120126 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity 
ksEll 
vmcSource 
VMCv20121128 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity 
ksEll 
vmcSource 
VMCv20130304 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity 
ksEll 
vmcSource 
VMCv20130805 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity 
ksEll 
vmcSource 
VMCv20140428 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.K 
ksEll 
vmcSource 
VMCv20140903 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.K 
ksEll 
vmcSource 
VMCv20150309 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.K 
ksEll 
vmcSource 
VMCv20151218 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.K 
ksEll 
vmcSource 
VMCv20160311 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.K 
ksEll 
vmcSource 
VMCv20160822 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.K 
ksEll 
vmcSource 
VMCv20170109 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.K 
ksEll 
vmcSource 
VMCv20170411 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.K 
ksEll 
vmcSource 
VMCv20171101 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.K 
ksEll 
vmcSource 
VMCv20180702 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.K 
ksEll 
vmcSource 
VMCv20181120 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.K 
ksEll 
vmcSource, vmcSourceRemeasurement 
VMCv20110816 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

0.9999995e9 
src.ellipticity 
ksEll 
vmcSource, vmcSynopticSource 
VMCDR1 
1b/a, where a/b=semimajor/minor axes in Ks 
real 
4 

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

0.9999995e9 
src.ellipticity;em.IR.K 
kseNum 
vhsMergeLog 
VHSDR1 
the extension number of this Ks frame 
tinyint 
1 


meta.number 
kseNum 
vhsMergeLog 
VHSDR2 
the extension number of this Ks frame 
tinyint 
1 


meta.number 
kseNum 
vhsMergeLog 
VHSDR3 
the extension number of this Ks frame 
tinyint 
1 


meta.number;em.IR.K 
kseNum 
vhsMergeLog 
VHSDR4 
the extension number of this Ks frame 
tinyint 
1 


meta.number;em.IR.K 
kseNum 
vhsMergeLog 
VHSv20120926 
the extension number of this Ks frame 
tinyint 
1 


meta.number 
kseNum 
vhsMergeLog 
VHSv20130417 
the extension number of this Ks frame 
tinyint 
1 


meta.number 
kseNum 
vhsMergeLog 
VHSv20140409 
the extension number of this Ks frame 
tinyint 
1 


meta.number;em.IR.K 
kseNum 
vhsMergeLog 
VHSv20150108 
the extension number of this Ks frame 
tinyint 
1 


meta.number;em.IR.K 
kseNum 
vhsMergeLog 
VHSv20160114 
the extension number of this Ks frame 
tinyint 
1 


meta.number;em.IR.K 
kseNum 
vhsMergeLog 
VHSv20160507 
the extension number of this Ks frame 
tinyint 
1 


meta.number;em.IR.K 
kseNum 
vhsMergeLog 
VHSv20170630 
the extension number of this Ks frame 
tinyint 
1 


meta.number;em.IR.K 
kseNum 
vhsMergeLog 
VHSv20171207 
the extension number of this Ks frame 
tinyint 
1 


meta.number;em.IR.K 
kseNum 
vhsMergeLog 
VHSv20180419 
the extension number of this Ks frame 
tinyint 
1 


meta.number;em.IR.K 
kseNum 
videoMergeLog 
VIDEODR2 
the extension number of this Ks frame 
tinyint 
1 


meta.number 
kseNum 
videoMergeLog 
VIDEODR3 
the extension number of this Ks frame 
tinyint 
1 


meta.number 
kseNum 
videoMergeLog 
VIDEODR4 
the extension number of this Ks frame 
tinyint 
1 


meta.number;em.IR.K 
kseNum 
videoMergeLog 
VIDEODR5 
the extension number of this Ks frame 
tinyint 
1 


meta.number;em.IR.K 
kseNum 
videoMergeLog 
VIDEOv20100513 
the extension number of this Ks frame 
tinyint 
1 


meta.number 
kseNum 
videoMergeLog 
VIDEOv20111208 
the extension number of this Ks frame 
tinyint 
1 


meta.number 
kseNum 
vikingMergeLog 
VIKINGDR2 
the extension number of this Ks frame 
tinyint 
1 


meta.number 
kseNum 
vikingMergeLog 
VIKINGDR3 
the extension number of this Ks frame 
tinyint 
1 


meta.number 
kseNum 
vikingMergeLog 
VIKINGDR4 
the extension number of this Ks frame 
tinyint 
1 


meta.number;em.IR.K 
kseNum 
vikingMergeLog 
VIKINGv20110714 
the extension number of this Ks frame 
tinyint 
1 


meta.number 
kseNum 
vikingMergeLog 
VIKINGv20111019 
the extension number of this Ks frame 
tinyint 
1 


meta.number 
kseNum 
vikingMergeLog 
VIKINGv20130417 
the extension number of this Ks frame 
tinyint 
1 


meta.number 
kseNum 
vikingMergeLog 
VIKINGv20140402 
the extension number of this Ks frame 
tinyint 
1 


meta.number 
kseNum 
vikingMergeLog 
VIKINGv20150421 
the extension number of this Ks frame 
tinyint 
1 


meta.number;em.IR.K 
kseNum 
vikingMergeLog 
VIKINGv20151230 
the extension number of this Ks frame 
tinyint 
1 


meta.number;em.IR.K 
kseNum 
vikingMergeLog 
VIKINGv20160406 
the extension number of this Ks frame 
tinyint 
1 


meta.number;em.IR.K 
kseNum 
vikingMergeLog 
VIKINGv20161202 
the extension number of this Ks frame 
tinyint 
1 


meta.number;em.IR.K 
kseNum 
vikingMergeLog 
VIKINGv20170715 
the extension number of this Ks frame 
tinyint 
1 


meta.number;em.IR.K 
kseNum 
vikingMergeLog 
VIKINGv20181012 
the extension number of this Ks frame 
tinyint 
1 


meta.number;em.IR.K 
kseNum 
vikingZY_selJ_RemeasMergeLog 
VIKINGZYSELJv20160909 
the extension number of this Ks frame 
tinyint 
1 


meta.number 
kseNum 
vikingZY_selJ_RemeasMergeLog 
VIKINGZYSELJv20170124 
the extension number of this Ks frame 
tinyint 
1 


meta.number 
kseNum 
vmcMergeLog 
VMCDR2 
the extension number of this Ks frame 
tinyint 
1 


meta.number 
kseNum 
vmcMergeLog 
VMCDR3 
the extension number of this Ks frame 
tinyint 
1 


meta.number;em.IR.K 
kseNum 
vmcMergeLog 
VMCDR4 
the extension number of this Ks frame 
tinyint 
1 


meta.number;em.IR.K 
kseNum 
vmcMergeLog 
VMCv20110816 
the extension number of this Ks frame 
tinyint 
1 


meta.number 
kseNum 
vmcMergeLog 
VMCv20110909 
the extension number of this Ks frame 
tinyint 
1 


meta.number 
kseNum 
vmcMergeLog 
VMCv20120126 
the extension number of this Ks frame 
tinyint 
1 


meta.number 
kseNum 
vmcMergeLog 
VMCv20121128 
the extension number of this Ks frame 
tinyint 
1 


meta.number 
kseNum 
vmcMergeLog 
VMCv20130304 
the extension number of this Ks frame 
tinyint 
1 


meta.number 
kseNum 
vmcMergeLog 
VMCv20130805 
the extension number of this Ks frame 
tinyint 
1 


meta.number 
kseNum 
vmcMergeLog 
VMCv20140428 
the extension number of this Ks frame 
tinyint 
1 


meta.number;em.IR.K 
kseNum 
vmcMergeLog 
VMCv20140903 
the extension number of this Ks frame 
tinyint 
1 


meta.number;em.IR.K 
kseNum 
vmcMergeLog 
VMCv20150309 
the extension number of this Ks frame 
tinyint 
1 


meta.number;em.IR.K 
kseNum 
vmcMergeLog 
VMCv20151218 
the extension number of this Ks frame 
tinyint 
1 


meta.number;em.IR.K 
kseNum 
vmcMergeLog 
VMCv20160311 
the extension number of this Ks frame 
tinyint 
1 


meta.number;em.IR.K 
kseNum 
vmcMergeLog 
VMCv20160822 
the extension number of this Ks frame 
tinyint 
1 


meta.number;em.IR.K 
kseNum 
vmcMergeLog 
VMCv20170109 
the extension number of this Ks frame 
tinyint 
1 


meta.number;em.IR.K 
kseNum 
vmcMergeLog 
VMCv20170411 
the extension number of this Ks frame 
tinyint 
1 


meta.number;em.IR.K 
kseNum 
vmcMergeLog 
VMCv20171101 
the extension number of this Ks frame 
tinyint 
1 


meta.number;em.IR.K 
kseNum 
vmcMergeLog 
VMCv20180702 
the extension number of this Ks frame 
tinyint 
1 


meta.number;em.IR.K 
kseNum 
vmcMergeLog 
VMCv20181120 
the extension number of this Ks frame 
tinyint 
1 


meta.number;em.IR.K 
kseNum 
vmcMergeLog, vmcSynopticMergeLog 
VMCDR1 
the extension number of this Ks frame 
tinyint 
1 


meta.number 
kseNum 
vvvMergeLog, vvvPsfDaophotJKsMergeLog, vvvSynopticMergeLog 
VVVDR4 
the extension number of this Ks frame 
tinyint 
1 


meta.number;em.IR.K 
ksErrBits 
vhsSource 
VHSDR1 
processing warning/error bitwise flags in Ks 
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. 
ksErrBits 
vhsSource 
VHSDR2 
processing warning/error bitwise flags in Ks 
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. 
ksErrBits 
vhsSource 
VHSDR3 
processing warning/error bitwise flags in Ks 
int 
4 

99999999 
meta.code;em.IR.K 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
ksErrBits 
vhsSource 
VHSDR4 
processing warning/error bitwise flags in Ks 
int 
4 

99999999 
meta.code;em.IR.K 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
ksErrBits 
vhsSource 
VHSv20120926 
processing warning/error bitwise flags in Ks 
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. 
ksErrBits 
vhsSource 
VHSv20130417 
processing warning/error bitwise flags in Ks 
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. 
ksErrBits 
vhsSource 
VHSv20140409 
processing warning/error bitwise flags in Ks 
int 
4 

99999999 
meta.code;em.IR.K 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
ksErrBits 
vhsSource 
VHSv20150108 
processing warning/error bitwise flags in Ks 
int 
4 

99999999 
meta.code;em.IR.K 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
ksErrBits 
vhsSource 
VHSv20160114 
processing warning/error bitwise flags in Ks 
int 
4 

99999999 
meta.code;em.IR.K 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
ksErrBits 
vhsSource 
VHSv20160507 
processing warning/error bitwise flags in Ks 
int 
4 

99999999 
meta.code;em.IR.K 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
ksErrBits 
vhsSource 
VHSv20170630 
processing warning/error bitwise flags in Ks 
int 
4 

99999999 
meta.code;em.IR.K 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
ksErrBits 
vhsSource 
VHSv20171207 
processing warning/error bitwise flags in Ks 
int 
4 

99999999 
meta.code;em.IR.K 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
ksErrBits 
vhsSource 
VHSv20180419 
processing warning/error bitwise flags in Ks 
int 
4 

99999999 
meta.code;em.IR.K 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
ksErrBits 
vhsSourceRemeasurement 
VHSDR1 
processing warning/error bitwise flags in Ks 
int 
4 

99999999 
meta.code 
ksErrBits 
videoSource 
VIDEODR2 
processing warning/error bitwise flags in Ks 
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  

ksErrBits 
videoSource 
VIDEODR3 
processing warning/error bitwise flags in Ks 
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  

ksErrBits 
videoSource 
VIDEODR4 
processing warning/error bitwise flags in Ks 
int 
4 

99999999 
meta.code;em.IR.K 
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  

ksErrBits 
videoSource 
VIDEODR5 
processing warning/error bitwise flags in Ks 
int 
4 

99999999 
meta.code;em.IR.K 
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  

ksErrBits 
videoSource 
VIDEOv20100513 
processing warning/error bitwise flags in Ks 
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  

ksErrBits 
videoSource 
VIDEOv20111208 
processing warning/error bitwise flags in Ks 
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  

ksErrBits 
videoSourceRemeasurement 
VIDEOv20100513 
processing warning/error bitwise flags in Ks 
int 
4 

99999999 
meta.code 
ksErrBits 
vikingSource 
VIKINGDR2 
processing warning/error bitwise flags in Ks 
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. 
ksErrBits 
vikingSource 
VIKINGDR3 
processing warning/error bitwise flags in Ks 
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. 
ksErrBits 
vikingSource 
VIKINGDR4 
processing warning/error bitwise flags in Ks 
int 
4 

99999999 
meta.code;em.IR.K 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
ksErrBits 
vikingSource 
VIKINGv20110714 
processing warning/error bitwise flags in Ks 
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. 
ksErrBits 
vikingSource 
VIKINGv20111019 
processing warning/error bitwise flags in Ks 
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. 
ksErrBits 
vikingSource 
VIKINGv20130417 
processing warning/error bitwise flags in Ks 
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. 
ksErrBits 
vikingSource 
VIKINGv20140402 
processing warning/error bitwise flags in Ks 
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. 
ksErrBits 
vikingSource 
VIKINGv20150421 
processing warning/error bitwise flags in Ks 
int 
4 

99999999 
meta.code;em.IR.K 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
ksErrBits 
vikingSource 
VIKINGv20151230 
processing warning/error bitwise flags in Ks 
int 
4 

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

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

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

99999999 
meta.code;em.IR.K 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
ksErrBits 
vikingSource 
VIKINGv20181012 
processing warning/error bitwise flags in Ks 
int 
4 

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

99999999 
meta.code 
ksErrBits 
vikingSourceRemeasurement 
VIKINGv20111019 
processing warning/error bitwise flags in Ks 
int 
4 

99999999 
meta.code 
ksErrBits 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
processing warning/error bitwise flags in Ks 
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. 
ksErrBits 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
processing warning/error bitwise flags in Ks 
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. 
ksErrBits 
vmcSource 
VMCDR2 
processing warning/error bitwise flags in Ks 
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. 
ksErrBits 
vmcSource 
VMCDR3 
processing warning/error bitwise flags in Ks 
int 
4 

99999999 
meta.code;em.IR.K 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
ksErrBits 
vmcSource 
VMCDR4 
processing warning/error bitwise flags in Ks 
int 
4 

99999999 
meta.code;em.IR.K 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
ksErrBits 
vmcSource 
VMCv20110816 
processing warning/error bitwise flags in Ks 
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. 
ksErrBits 
vmcSource 
VMCv20110909 
processing warning/error bitwise flags in Ks 
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. 
ksErrBits 
vmcSource 
VMCv20120126 
processing warning/error bitwise flags in Ks 
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. 
ksErrBits 
vmcSource 
VMCv20121128 
processing warning/error bitwise flags in Ks 
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. 
ksErrBits 
vmcSource 
VMCv20130304 
processing warning/error bitwise flags in Ks 
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. 
ksErrBits 
vmcSource 
VMCv20130805 
processing warning/error bitwise flags in Ks 
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. 
ksErrBits 
vmcSource 
VMCv20140428 
processing warning/error bitwise flags in Ks 
int 
4 

99999999 
meta.code;em.IR.K 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
ksErrBits 
vmcSource 
VMCv20140903 
processing warning/error bitwise flags in Ks 
int 
4 

99999999 
meta.code;em.IR.K 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
ksErrBits 
vmcSource 
VMCv20150309 
processing warning/error bitwise flags in Ks 
int 
4 

99999999 
meta.code;em.IR.K 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
ksErrBits 
vmcSource 
VMCv20151218 
processing warning/error bitwise flags in Ks 
int 
4 

99999999 
meta.code;em.IR.K 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
ksErrBits 
vmcSource 
VMCv20160311 
processing warning/error bitwise flags in Ks 
int 
4 

99999999 
meta.code;em.IR.K 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
ksErrBits 
vmcSource 
VMCv20160822 
processing warning/error bitwise flags in Ks 
int 
4 

99999999 
meta.code;em.IR.K 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
ksErrBits 
vmcSource 
VMCv20170109 
processing warning/error bitwise flags in Ks 
int 
4 

99999999 
meta.code;em.IR.K 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
ksErrBits 
vmcSource 
VMCv20170411 
processing warning/error bitwise flags in Ks 
int 
4 

99999999 
meta.code;em.IR.K 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
ksErrBits 
vmcSource 
VMCv20171101 
processing warning/error bitwise flags in Ks 
int 
4 

99999999 
meta.code;em.IR.K 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
ksErrBits 
vmcSource 
VMCv20180702 
processing warning/error bitwise flags in Ks 
int 
4 

99999999 
meta.code;em.IR.K 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
ksErrBits 
vmcSource 
VMCv20181120 
processing warning/error bitwise flags in Ks 
int 
4 

99999999 
meta.code;em.IR.K 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
ksErrBits 
vmcSource, vmcSynopticSource 
VMCDR1 
processing warning/error bitwise flags in Ks 
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. 
ksErrBits 
vmcSourceRemeasurement 
VMCv20110816 
processing warning/error bitwise flags in Ks 
int 
4 

99999999 
meta.code 
ksErrBits 
vmcSourceRemeasurement 
VMCv20110909 
processing warning/error bitwise flags in Ks 
int 
4 

99999999 
meta.code 
ksErrBits 
vvvSource, vvvSynopticSource 
VVVDR4 
processing warning/error bitwise flags in Ks 
int 
4 

99999999 
meta.code;em.IR.K 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
ksEta 
vhsSource 
VHSDR1 
Offset of Ks 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. 
ksEta 
vhsSource 
VHSDR2 
Offset of Ks 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. 
ksEta 
vhsSource 
VHSDR3 
Offset of Ks detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.K 
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. 
ksEta 
vhsSource 
VHSDR4 
Offset of Ks detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.K 
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. 
ksEta 
vhsSource 
VHSv20120926 
Offset of Ks 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. 
ksEta 
vhsSource 
VHSv20130417 
Offset of Ks 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. 
ksEta 
vhsSource 
VHSv20140409 
Offset of Ks detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.K 
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. 
ksEta 
vhsSource 
VHSv20150108 
Offset of Ks detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.K 
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. 
ksEta 
vhsSource 
VHSv20160114 
Offset of Ks detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.K 
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. 
ksEta 
vhsSource 
VHSv20160507 
Offset of Ks detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.K 
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. 
ksEta 
vhsSource 
VHSv20170630 
Offset of Ks detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.K 
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. 
ksEta 
vhsSource 
VHSv20171207 
Offset of Ks detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.K 
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. 
ksEta 
vhsSource 
VHSv20180419 
Offset of Ks detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.K 
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. 
ksEta 
videoSource 
VIDEODR2 
Offset of Ks 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. 
ksEta 
videoSource 
VIDEODR3 
Offset of Ks 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. 
ksEta 
videoSource 
VIDEODR4 
Offset of Ks detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.K 
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. 
ksEta 
videoSource 
VIDEODR5 
Offset of Ks detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.K 
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. 
ksEta 
videoSource 
VIDEOv20100513 
Offset of Ks 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. 
ksEta 
videoSource 
VIDEOv20111208 
Offset of Ks 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. 
ksEta 
vikingSource 
VIKINGDR2 
Offset of Ks 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. 
ksEta 
vikingSource 
VIKINGDR3 
Offset of Ks 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. 
ksEta 
vikingSource 
VIKINGDR4 
Offset of Ks detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.K 
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. 
ksEta 
vikingSource 
VIKINGv20110714 
Offset of Ks 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. 
ksEta 
vikingSource 
VIKINGv20111019 
Offset of Ks 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. 
ksEta 
vikingSource 
VIKINGv20130417 
Offset of Ks 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. 
ksEta 
vikingSource 
VIKINGv20140402 
Offset of Ks 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. 
ksEta 
vikingSource 
VIKINGv20150421 
Offset of Ks detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.K 
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. 
ksEta 
vikingSource 
VIKINGv20151230 
Offset of Ks detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.K 
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. 
ksEta 
vikingSource 
VIKINGv20160406 
Offset of Ks detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.K 
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. 
ksEta 
vikingSource 
VIKINGv20161202 
Offset of Ks detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.K 
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. 
ksEta 
vikingSource 
VIKINGv20170715 
Offset of Ks detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.K 
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. 
ksEta 
vikingSource 
VIKINGv20181012 
Offset of Ks detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.K 
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. 
ksEta 
vmcSource 
VMCDR2 
Offset of Ks 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. 
ksEta 
vmcSource 
VMCDR3 
Offset of Ks detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.K 
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. 
ksEta 
vmcSource 
VMCDR4 
Offset of Ks detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.K 
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. 
ksEta 
vmcSource 
VMCv20110816 
Offset of Ks 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. 
ksEta 
vmcSource 
VMCv20110909 
Offset of Ks 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. 
ksEta 
vmcSource 
VMCv20120126 
Offset of Ks 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. 
ksEta 
vmcSource 
VMCv20121128 
Offset of Ks 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. 
ksEta 
vmcSource 
VMCv20130304 
Offset of Ks 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. 
ksEta 
vmcSource 
VMCv20130805 
Offset of Ks 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. 
ksEta 
vmcSource 
VMCv20140428 
Offset of Ks detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.K 
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. 
ksEta 
vmcSource 
VMCv20140903 
Offset of Ks detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.K 
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. 
ksEta 
vmcSource 
VMCv20150309 
Offset of Ks detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.K 
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. 
ksEta 
vmcSource 
VMCv20151218 
Offset of Ks detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.K 
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. 
ksEta 
vmcSource 
VMCv20160311 
Offset of Ks detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.K 
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. 
ksEta 
vmcSource 
VMCv20160822 
Offset of Ks detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.K 
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. 
ksEta 
vmcSource 
VMCv20170109 
Offset of Ks detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.K 
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. 
ksEta 
vmcSource 
VMCv20170411 
Offset of Ks detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.K 
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. 
ksEta 
vmcSource 
VMCv20171101 
Offset of Ks detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.K 
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. 
ksEta 
vmcSource 
VMCv20180702 
Offset of Ks detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.K 
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. 
ksEta 
vmcSource 
VMCv20181120 
Offset of Ks detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.K 
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. 
ksEta 
vmcSource, vmcSynopticSource 
VMCDR1 
Offset of Ks 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. 
ksEta 
vvvSource, vvvSynopticSource 
VVVDR4 
Offset of Ks detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.K 
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. 
ksexpML 
videoVarFrameSetInfo 
VIDEODR2 
Expected magnitude limit of frameSet in this in Ks band. 
real 
4 

0.9999995e9 

ksexpML 
videoVarFrameSetInfo 
VIDEODR3 
Expected magnitude limit of frameSet in this in Ks band. 
real 
4 

0.9999995e9 
phot.mag;stat.max;em.IR.NIR 
ksexpML 
videoVarFrameSetInfo 
VIDEODR4 
Expected magnitude limit of frameSet in this in Ks band. 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K;stat.max 
ksexpML 
videoVarFrameSetInfo 
VIDEODR5 
Expected magnitude limit of frameSet in this in Ks band. 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K;stat.max 
ksexpML 
videoVarFrameSetInfo 
VIDEOv20100513 
Expected magnitude limit of frameSet in this in Ks band. 
real 
4 

0.9999995e9 

ksexpML 
videoVarFrameSetInfo 
VIDEOv20111208 
Expected magnitude limit of frameSet in this in Ks band. 
real 
4 

0.9999995e9 

ksexpML 
vikingVarFrameSetInfo 
VIKINGDR2 
Expected magnitude limit of frameSet in this in Ks band. 
real 
4 

0.9999995e9 

ksexpML 
vikingVarFrameSetInfo 
VIKINGv20110714 
Expected magnitude limit of frameSet in this in Ks band. 
real 
4 

0.9999995e9 

ksexpML 
vikingVarFrameSetInfo 
VIKINGv20111019 
Expected magnitude limit of frameSet in this in Ks band. 
real 
4 

0.9999995e9 

ksexpML 
vmcVarFrameSetInfo 
VMCDR1 
Expected magnitude limit of frameSet in this in Ks band. 
real 
4 

0.9999995e9 

ksexpML 
vmcVarFrameSetInfo 
VMCDR2 
Expected magnitude limit of frameSet in this in Ks band. 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K;stat.max;em.IR.NIR 
ksexpML 
vmcVarFrameSetInfo 
VMCDR3 
Expected magnitude limit of frameSet in this in Ks band. 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K;stat.max 
ksexpML 
vmcVarFrameSetInfo 
VMCDR4 
Expected magnitude limit of frameSet in this in Ks band. 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K;stat.max 
ksexpML 
vmcVarFrameSetInfo 
VMCv20110816 
Expected magnitude limit of frameSet in this in Ks band. 
real 
4 

0.9999995e9 

ksexpML 
vmcVarFrameSetInfo 
VMCv20110909 
Expected magnitude limit of frameSet in this in Ks band. 
real 
4 

0.9999995e9 

ksexpML 
vmcVarFrameSetInfo 
VMCv20120126 
Expected magnitude limit of frameSet in this in Ks band. 
real 
4 

0.9999995e9 

ksexpML 
vmcVarFrameSetInfo 
VMCv20121128 
Expected magnitude limit of frameSet in this in Ks band. 
real 
4 
mag 
0.9999995e9 
phot.mag;stat.max;em.IR.NIR 
ksexpML 
vmcVarFrameSetInfo 
VMCv20130304 
Expected magnitude limit of frameSet in this in Ks band. 
real 
4 
mag 
0.9999995e9 
phot.mag;stat.max;em.IR.NIR 
ksexpML 
vmcVarFrameSetInfo 
VMCv20130805 
Expected magnitude limit of frameSet in this in Ks band. 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K;stat.max;em.IR.NIR 
ksexpML 
vmcVarFrameSetInfo 
VMCv20140428 
Expected magnitude limit of frameSet in this in Ks band. 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K;stat.max 
ksexpML 
vmcVarFrameSetInfo 
VMCv20140903 
Expected magnitude limit of frameSet in this in Ks band. 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K;stat.max 
ksexpML 
vmcVarFrameSetInfo 
VMCv20150309 
Expected magnitude limit of frameSet in this in Ks band. 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K;stat.max 
ksexpML 
vmcVarFrameSetInfo 
VMCv20151218 
Expected magnitude limit of frameSet in this in Ks band. 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K;stat.max 
ksexpML 
vmcVarFrameSetInfo 
VMCv20160311 
Expected magnitude limit of frameSet in this in Ks band. 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K;stat.max 
ksexpML 
vmcVarFrameSetInfo 
VMCv20160822 
Expected magnitude limit of frameSet in this in Ks band. 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K;stat.max 
ksexpML 
vmcVarFrameSetInfo 
VMCv20170109 
Expected magnitude limit of frameSet in this in Ks band. 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K;stat.max 
ksexpML 
vmcVarFrameSetInfo 
VMCv20170411 
Expected magnitude limit of frameSet in this in Ks band. 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K;stat.max 
ksexpML 
vmcVarFrameSetInfo 
VMCv20171101 
Expected magnitude limit of frameSet in this in Ks band. 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K;stat.max 
ksexpML 
vmcVarFrameSetInfo 
VMCv20180702 
Expected magnitude limit of frameSet in this in Ks band. 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K;stat.max 
ksexpML 
vmcVarFrameSetInfo 
VMCv20181120 
Expected magnitude limit of frameSet in this in Ks band. 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K;stat.max 
ksexpML 
vvvVarFrameSetInfo 
VVVDR4 
Expected magnitude limit of frameSet in this in Ks band. 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.K;stat.max 
ksExpRms 
videoVariability 
VIDEODR2 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks 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. 
ksExpRms 
videoVariability 
VIDEODR3 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks 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. 
ksExpRms 
videoVariability 
VIDEODR4 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks band 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This 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. 
ksExpRms 
videoVariability 
VIDEODR5 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks band 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This 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. 
ksExpRms 
videoVariability 
VIDEOv20100513 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks 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. 
ksExpRms 
videoVariability 
VIDEOv20111208 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks 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. 
ksExpRms 
vikingVariability 
VIKINGDR2 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks 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. 
ksExpRms 
vikingVariability 
VIKINGv20110714 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks 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. 
ksExpRms 
vikingVariability 
VIKINGv20111019 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks 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. 
ksExpRms 
vmcVariability 
VMCDR1 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks 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. 
ksExpRms 
vmcVariability 
VMCDR2 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks 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. 
ksExpRms 
vmcVariability 
VMCDR3 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks band 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This 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. 
ksExpRms 
vmcVariability 
VMCDR4 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks band 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This 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. 
ksExpRms 
vmcVariability 
VMCv20110816 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks 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. 
ksExpRms 
vmcVariability 
VMCv20110909 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks 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. 
ksExpRms 
vmcVariability 
VMCv20120126 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks 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. 
ksExpRms 
vmcVariability 
VMCv20121128 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks 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. 
ksExpRms 
vmcVariability 
VMCv20130304 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks 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. 
ksExpRms 
vmcVariability 
VMCv20130805 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks 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. 
ksExpRms 
vmcVariability 
VMCv20140428 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks band 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This 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. 
ksExpRms 
vmcVariability 
VMCv20140903 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks band 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This 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. 
ksExpRms 
vmcVariability 
VMCv20150309 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks band 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This 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. 
ksExpRms 
vmcVariability 
VMCv20151218 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks band 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This 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. 
ksExpRms 
vmcVariability 
VMCv20160311 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks band 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.K 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This 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. 
ksExpRms 