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


h_2mrat 
twomass_scn 
2MASS 
Hband average 2nd image moment ratio. 
real 
4 


stat.fit.param 
h_2mrat 
twomass_sixx2_scn 
2MASS 
H band average 2nd image moment ratio for scan 
real 
4 



h_5sig_ba 
twomass_xsc 
2MASS 
H minor/major axis ratio fit to the 5sigma isophote. 
real 
4 


phys.size.axisRatio 
h_5sig_phi 
twomass_xsc 
2MASS 
H angle to 5sigma major axis (E of N). 
smallint 
2 
degrees 

stat.error 
h_5surf 
twomass_xsc 
2MASS 
H central surface brightness (r<=5). 
real 
4 
mag 

phot.mag.sb 
h_ba 
twomass_xsc 
2MASS 
H minor/major axis ratio fit to the 3sigma isophote. 
real 
4 


phys.size.axisRatio 
h_back 
twomass_xsc 
2MASS 
H coadd median background. 
real 
4 


meta.code 
h_bisym_chi 
twomass_xsc 
2MASS 
H bisymmetric crosscorrelation chi. 
real 
4 


stat.fit.param 
h_bisym_rat 
twomass_xsc 
2MASS 
H bisymmetric flux ratio. 
real 
4 


phot.flux;arith.ratio 
h_bndg_amp 
twomass_xsc 
2MASS 
H banding maximum FT amplitude on this side of coadd. 
real 
4 
DN 

stat.fit.param 
h_bndg_per 
twomass_xsc 
2MASS 
H banding Fourier Transf. period on this side of coadd. 
int 
4 
arcsec 

stat.fit.param 
h_cmsig 
twomass_psc 
2MASS 
Corrected photometric uncertainty for the default Hband magnitude. 
real 
4 
mag 
Hband 
phot.flux 
h_con_indx 
twomass_xsc 
2MASS 
H concentration index r_75%/r_25%. 
real 
4 


phys.size;arith.ratio 
h_d_area 
twomass_xsc 
2MASS 
H 5sigma to 3sigma differential area. 
smallint 
2 


stat.fit.residual 
h_flg_10 
twomass_xsc 
2MASS 
H confusion flag for 10 arcsec circular ap. mag. 
smallint 
2 


meta.code 
h_flg_15 
twomass_xsc 
2MASS 
H confusion flag for 15 arcsec circular ap. mag. 
smallint 
2 


meta.code 
h_flg_20 
twomass_xsc 
2MASS 
H confusion flag for 20 arcsec circular ap. mag. 
smallint 
2 


meta.code 
h_flg_25 
twomass_xsc 
2MASS 
H confusion flag for 25 arcsec circular ap. mag. 
smallint 
2 


meta.code 
h_flg_30 
twomass_xsc 
2MASS 
H confusion flag for 30 arcsec circular ap. mag. 
smallint 
2 


meta.code 
h_flg_40 
twomass_xsc 
2MASS 
H confusion flag for 40 arcsec circular ap. mag. 
smallint 
2 


meta.code 
h_flg_5 
twomass_xsc 
2MASS 
H confusion flag for 5 arcsec circular ap. mag. 
smallint 
2 


meta.code 
h_flg_50 
twomass_xsc 
2MASS 
H confusion flag for 50 arcsec circular ap. mag. 
smallint 
2 


meta.code 
h_flg_60 
twomass_xsc 
2MASS 
H confusion flag for 60 arcsec circular ap. mag. 
smallint 
2 


meta.code 
h_flg_7 
twomass_sixx2_xsc 
2MASS 
H confusion flag for 7 arcsec circular ap. mag 
smallint 
2 



h_flg_7 
twomass_xsc 
2MASS 
H confusion flag for 7 arcsec circular ap. mag. 
smallint 
2 


meta.code 
h_flg_70 
twomass_xsc 
2MASS 
H confusion flag for 70 arcsec circular ap. mag. 
smallint 
2 


meta.code 
h_flg_c 
twomass_xsc 
2MASS 
H confusion flag for Kron circular mag. 
smallint 
2 


meta.code 
h_flg_e 
twomass_xsc 
2MASS 
H confusion flag for Kron elliptical mag. 
smallint 
2 


meta.code 
h_flg_fc 
twomass_xsc 
2MASS 
H confusion flag for fiducial Kron circ. mag. 
smallint 
2 


meta.code 
h_flg_fe 
twomass_xsc 
2MASS 
H confusion flag for fiducial Kron ell. mag. 
smallint 
2 


meta.code 
h_flg_i20c 
twomass_xsc 
2MASS 
H confusion flag for 20mag/sq." iso. circ. mag. 
smallint 
2 


meta.code 
h_flg_i20e 
twomass_xsc 
2MASS 
H confusion flag for 20mag/sq." iso. ell. mag. 
smallint 
2 


meta.code 
h_flg_i21c 
twomass_xsc 
2MASS 
H confusion flag for 21mag/sq." iso. circ. mag. 
smallint 
2 


meta.code 
h_flg_i21e 
twomass_xsc 
2MASS 
H confusion flag for 21mag/sq." iso. ell. mag. 
smallint 
2 


meta.code 
h_flg_j21fc 
twomass_xsc 
2MASS 
H confusion flag for 21mag/sq." iso. fid. circ. mag. 
smallint 
2 


meta.code 
h_flg_j21fe 
twomass_xsc 
2MASS 
H confusion flag for 21mag/sq." iso. fid. ell. mag. 
smallint 
2 


meta.code 
h_flg_k20fc 
twomass_xsc 
2MASS 
H confusion flag for 20mag/sq." iso. fid. circ. mag. 
smallint 
2 


meta.code 
h_flg_k20fe 
twomass_sixx2_xsc 
2MASS 
H confusion flag for 20mag/sq.″ iso. fid. ell. mag 
smallint 
2 



h_flg_k20fe 
twomass_xsc 
2MASS 
H confusion flag for 20mag/sq." iso. fid. ell. mag. 
smallint 
2 


meta.code 
h_k 
twomass_sixx2_psc 
2MASS 
The HKs color, computed from the Hband and Ksband magnitudes (h_m and k_m, respectively) of the source. In cases where the second or third digit in rd_flg is equal to either "0", "4", "6", or "9", no color is computed because the photometry in one or both bands is of lower quality or the source is not detected. 
real 
4 



h_m 
twomass_psc 
2MASS 
Default Hband magnitude 
real 
4 
mag 

phot.flux 
h_m 
twomass_sixx2_psc 
2MASS 
H selected "default" magnitude 
real 
4 
mag 


h_m_10 
twomass_xsc 
2MASS 
H 10 arcsec radius circular aperture magnitude. 
real 
4 
mag 

phot.flux 
h_m_15 
twomass_xsc 
2MASS 
H 15 arcsec radius circular aperture magnitude. 
real 
4 
mag 

phot.flux 
h_m_20 
twomass_xsc 
2MASS 
H 20 arcsec radius circular aperture magnitude. 
real 
4 
mag 

phot.flux 
h_m_25 
twomass_xsc 
2MASS 
H 25 arcsec radius circular aperture magnitude. 
real 
4 
mag 

phot.flux 
h_m_2mass 
allwise_sc 
WISE 
2MASS Hband magnitude or magnitude upper limit of the associated 2MASS PSC source. This column is "null" if there is no associated 2MASS PSC source or if the 2MASS PSC Hband magnitude entry is "null". 
float 
8 
mag 


h_m_2mass 
wise_allskysc 
WISE 
2MASS Hband magnitude or magnitude upper limit of the associated 2MASS PSC source. This column is default if there is no associated 2MASS PSC source or if the 2MASS PSC Hband magnitude entry is default. 
real 
4 
mag 
0.9999995e9 

h_m_2mass 
wise_prelimsc 
WISE 
2MASS Hband magnitude or magnitude upper limit of the associated 2MASS PSC source This column is default if there is no associated 2MASS PSC source or if the 2MASS PSC Hband magnitude entry is default 
real 
4 
mag 
0.9999995e9 

h_m_30 
twomass_xsc 
2MASS 
H 30 arcsec radius circular aperture magnitude. 
real 
4 
mag 

phot.flux 
h_m_40 
twomass_xsc 
2MASS 
H 40 arcsec radius circular aperture magnitude. 
real 
4 
mag 

phot.flux 
h_m_5 
twomass_xsc 
2MASS 
H 5 arcsec radius circular aperture magnitude. 
real 
4 
mag 

phot.flux 
h_m_50 
twomass_xsc 
2MASS 
H 50 arcsec radius circular aperture magnitude. 
real 
4 
mag 

phot.flux 
h_m_60 
twomass_xsc 
2MASS 
H 60 arcsec radius circular aperture magnitude. 
real 
4 
mag 

phot.flux 
h_m_7 
twomass_sixx2_xsc 
2MASS 
H 7 arcsec radius circular aperture magnitude 
real 
4 
mag 


h_m_7 
twomass_xsc 
2MASS 
H 7 arcsec radius circular aperture magnitude. 
real 
4 
mag 

phot.flux 
h_m_70 
twomass_xsc 
2MASS 
H 70 arcsec radius circular aperture magnitude. 
real 
4 
mag 

phot.flux 
h_m_c 
twomass_xsc 
2MASS 
H Kron circular aperture magnitude. 
real 
4 
mag 

phot.flux 
h_m_e 
twomass_xsc 
2MASS 
H Kron elliptical aperture magnitude. 
real 
4 
mag 

phot.flux 
h_m_ext 
twomass_sixx2_xsc 
2MASS 
H mag from fit extrapolation 
real 
4 
mag 


h_m_ext 
twomass_xsc 
2MASS 
H mag from fit extrapolation. 
real 
4 
mag 

phot.flux 
h_m_fc 
twomass_xsc 
2MASS 
H fiducial Kron circular magnitude. 
real 
4 
mag 

phot.flux 
h_m_fe 
twomass_xsc 
2MASS 
H fiducial Kron ell. mag aperture magnitude. 
real 
4 
mag 

phot.flux 
h_m_i20c 
twomass_xsc 
2MASS 
H 20mag/sq." isophotal circular ap. magnitude. 
real 
4 
mag 

phot.flux 
h_m_i20e 
twomass_xsc 
2MASS 
H 20mag/sq." isophotal elliptical ap. magnitude. 
real 
4 
mag 

phot.flux 
h_m_i21c 
twomass_xsc 
2MASS 
H 21mag/sq." isophotal circular ap. magnitude. 
real 
4 
mag 

phot.flux 
h_m_i21e 
twomass_xsc 
2MASS 
H 21mag/sq." isophotal elliptical ap. magnitude. 
real 
4 
mag 

phot.flux 
h_m_j21fc 
twomass_xsc 
2MASS 
H 21mag/sq." isophotal fiducial circ. ap. mag. 
real 
4 
mag 

phot.flux 
h_m_j21fe 
twomass_xsc 
2MASS 
H 21mag/sq." isophotal fiducial ell. ap. magnitude. 
real 
4 
mag 

phot.flux 
h_m_k20fc 
twomass_xsc 
2MASS 
H 20mag/sq." isophotal fiducial circ. ap. mag. 
real 
4 
mag 

phot.flux 
H_M_K20FE 
twomass 
SIXDF 
H 20mag/sq." isophotal fiducial ell. ap. magnitude 
real 
4 
mag 


h_m_k20fe 
twomass_sixx2_xsc 
2MASS 
H 20mag/sq.″ isophotal fiducial ell. ap. magnitude 
real 
4 
mag 


h_m_k20fe 
twomass_xsc 
2MASS 
H 20mag/sq." isophotal fiducial ell. ap. magnitude. 
real 
4 
mag 

phot.flux 
h_m_stdap 
twomass_psc 
2MASS 
Hband "standard" aperture magnitude. 
real 
4 
mag 

phot.flux 
h_m_sys 
twomass_xsc 
2MASS 
H system photometry magnitude. 
real 
4 
mag 

phot.flux 
h_mnsurfb_eff 
twomass_xsc 
2MASS 
H mean surface brightness at the halflight radius. 
real 
4 
mag 

phot.mag.sb 
h_msig 
twomass_sixx2_psc 
2MASS 
H "default" mag uncertainty 
real 
4 
mag 


h_msig_10 
twomass_xsc 
2MASS 
H 1sigma uncertainty in 10 arcsec circular ap. mag. 
real 
4 
mag 

stat.error 
h_msig_15 
twomass_xsc 
2MASS 
H 1sigma uncertainty in 15 arcsec circular ap. mag. 
real 
4 
mag 

stat.error 
h_msig_20 
twomass_xsc 
2MASS 
H 1sigma uncertainty in 20 arcsec circular ap. mag. 
real 
4 
mag 

stat.error 
h_msig_25 
twomass_xsc 
2MASS 
H 1sigma uncertainty in 25 arcsec circular ap. mag. 
real 
4 
mag 

stat.error 
h_msig_2mass 
allwise_sc 
WISE 
2MASS Hband 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 Hband uncertainty entry is "null". 
float 
8 
mag 


h_msig_2mass 
wise_allskysc 
WISE 
2MASS Hband corrected photometric uncertainty of the associated 2MASS PSC source. This column is default if there is no associated 2MASS PSC source or if the 2MASS PSC Hband uncertainty entry is default. 
real 
4 
mag 
0.9999995e9 

h_msig_2mass 
wise_prelimsc 
WISE 
2MASS Hband corrected photometric uncertainty of the associated 2MASS PSC source This column is default if there is no associated 2MASS PSC source or if the 2MASS PSC Hband uncertainty entry is default 
real 
4 
mag 
0.9999995e9 

h_msig_30 
twomass_xsc 
2MASS 
H 1sigma uncertainty in 30 arcsec circular ap. mag. 
real 
4 
mag 

stat.error 
h_msig_40 
twomass_xsc 
2MASS 
H 1sigma uncertainty in 40 arcsec circular ap. mag. 
real 
4 
mag 

stat.error 
h_msig_5 
twomass_xsc 
2MASS 
H 1sigma uncertainty in 5 arcsec circular ap. mag. 
real 
4 
mag 

stat.error 
h_msig_50 
twomass_xsc 
2MASS 
H 1sigma uncertainty in 50 arcsec circular ap. mag. 
real 
4 
mag 

stat.error 
h_msig_60 
twomass_xsc 
2MASS 
H 1sigma uncertainty in 60 arcsec circular ap. mag. 
real 
4 
mag 

stat.error 
h_msig_7 
twomass_sixx2_xsc 
2MASS 
H 1sigma uncertainty in 7 arcsec circular ap. mag 
real 
4 
mag 


h_msig_7 
twomass_xsc 
2MASS 
H 1sigma uncertainty in 7 arcsec circular ap. mag. 
real 
4 
mag 

stat.error 
h_msig_70 
twomass_xsc 
2MASS 
H 1sigma uncertainty in 70 arcsec circular ap. mag. 
real 
4 
mag 

stat.error 
h_msig_c 
twomass_xsc 
2MASS 
H 1sigma uncertainty in Kron circular mag. 
real 
4 
mag 

stat.error 
h_msig_e 
twomass_xsc 
2MASS 
H 1sigma uncertainty in Kron elliptical mag. 
real 
4 
mag 

stat.error 
h_msig_ext 
twomass_sixx2_xsc 
2MASS 
H 1sigma uncertainty in mag from fit extrapolation 
real 
4 
mag 


h_msig_ext 
twomass_xsc 
2MASS 
H 1sigma uncertainty in mag from fit extrapolation. 
real 
4 
mag 

stat.error 
h_msig_fc 
twomass_xsc 
2MASS 
H 1sigma uncertainty in fiducial Kron circ. mag. 
real 
4 
mag 

stat.error 
h_msig_fe 
twomass_xsc 
2MASS 
H 1sigma uncertainty in fiducial Kron ell. mag. 
real 
4 
mag 

stat.error 
h_msig_i20c 
twomass_xsc 
2MASS 
H 1sigma uncertainty in 20mag/sq." iso. circ. mag. 
real 
4 
mag 

stat.error 
h_msig_i20e 
twomass_xsc 
2MASS 
H 1sigma uncertainty in 20mag/sq." iso. ell. mag. 
real 
4 
mag 

stat.error 
h_msig_i21c 
twomass_xsc 
2MASS 
H 1sigma uncertainty in 21mag/sq." iso. circ. mag. 
real 
4 
mag 

stat.error 
h_msig_i21e 
twomass_xsc 
2MASS 
H 1sigma uncertainty in 21mag/sq." iso. ell. mag. 
real 
4 
mag 

stat.error 
h_msig_j21fc 
twomass_xsc 
2MASS 
H 1sigma uncertainty in 21mag/sq." iso.fid.circ.mag. 
real 
4 
mag 

stat.error 
h_msig_j21fe 
twomass_xsc 
2MASS 
H 1sigma uncertainty in 21mag/sq." iso.fid.ell.mag. 
real 
4 
mag 

stat.error 
h_msig_k20fc 
twomass_xsc 
2MASS 
H 1sigma uncertainty in 20mag/sq." iso.fid.circ. mag. 
real 
4 
mag 

stat.error 
h_msig_k20fe 
twomass_sixx2_xsc 
2MASS 
H 1sigma uncertainty in 20mag/sq.″ iso.fid.ell.mag 
real 
4 
mag 


h_msig_k20fe 
twomass_xsc 
2MASS 
H 1sigma uncertainty in 20mag/sq." iso.fid.ell.mag. 
real 
4 
mag 

stat.error 
h_msig_stdap 
twomass_psc 
2MASS 
Uncertainty in the Hband standard aperture magnitude. 
real 
4 
mag 

phot.flux 
h_msig_sys 
twomass_xsc 
2MASS 
H 1sigma uncertainty in system photometry mag. 
real 
4 
mag 

stat.error 
h_msigcom 
twomass_psc 
2MASS 
Combined, or total photometric uncertainty for the default Hband magnitude. 
real 
4 
mag 
Hband 
phot.flux 
h_msigcom 
twomass_sixx2_psc 
2MASS 
combined (total) H band photometric uncertainty 
real 
4 
mag 


h_msnr10 
twomass_scn 
2MASS 
The estimated Hband magnitude at which SNR=10 is achieved for this scan. 
real 
4 
mag 

phot.flux 
h_msnr10 
twomass_sixx2_scn 
2MASS 
H mag at which SNR=10 is achieved, from h_psp and h_zp_ap 
real 
4 
mag 


h_n_snr10 
twomass_scn 
2MASS 
Number of point sources at Hband with SNR>10 (instrumental mag <=15.1) 
int 
4 


meta.number 
h_n_snr10 
twomass_sixx2_scn 
2MASS 
number of H point sources with SNR>10 (instrumental m<=15.1) 
int 
4 



h_pchi 
twomass_xsc 
2MASS 
H chi^2 of fit to rad. profile (LCSB: alpha scale len). 
real 
4 


stat.fit.param 
h_peak 
twomass_xsc 
2MASS 
H peak pixel brightness. 
real 
4 
mag 

phot.mag.sb 
h_perc_darea 
twomass_xsc 
2MASS 
H 5sigma to 3sigma percent area change. 
smallint 
2 


FIT_PARAM 
h_phi 
twomass_xsc 
2MASS 
H angle to 3sigma major axis (E of N). 
smallint 
2 
degrees 

pos.posAng 
h_psfchi 
twomass_psc 
2MASS 
Reduced chisquared goodnessoffit value for the Hband profilefit photometry made on the 1.3 s "Read_2" exposures. 
real 
4 


stat.fit.param 
h_psp 
twomass_scn 
2MASS 
Hband photometric sensitivity paramater (PSP). 
real 
4 


instr.sensitivity 
h_psp 
twomass_sixx2_scn 
2MASS 
H photometric sensitivity param: h_shape_avg*(h_fbg_avg^.29) 
real 
4 



h_pts_noise 
twomass_scn 
2MASS 
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 Hband photometric errors and is expressed in units of mJy. 
real 
4 


instr.det.noise 
h_pts_noise 
twomass_sixx2_scn 
2MASS 
log10 of H band modal point src noise estimate 
real 
4 
logmJy 


h_r_c 
twomass_xsc 
2MASS 
H Kron circular aperture radius. 
real 
4 
arcsec 

phys.angSize;src 
h_r_e 
twomass_xsc 
2MASS 
H Kron elliptical aperture semimajor axis. 
real 
4 
arcsec 

phys.angSize;src 
h_r_eff 
twomass_xsc 
2MASS 
H halflight (integrated halfflux point) radius. 
real 
4 
arcsec 

phys.angSize;src 
h_r_i20c 
twomass_xsc 
2MASS 
H 20mag/sq." isophotal circular aperture radius. 
real 
4 
arcsec 

phys.angSize;src 
h_r_i20e 
twomass_xsc 
2MASS 
H 20mag/sq." isophotal elliptical ap. semimajor axis. 
real 
4 
arcsec 

phys.angSize;src 
h_r_i21c 
twomass_xsc 
2MASS 
H 21mag/sq." isophotal circular aperture radius. 
real 
4 
arcsec 

phys.angSize;src 
h_r_i21e 
twomass_xsc 
2MASS 
H 21mag/sq." isophotal elliptical ap. semimajor axis. 
real 
4 
arcsec 

phys.angSize;src 
h_resid_ann 
twomass_xsc 
2MASS 
H residual annulus background median. 
real 
4 
DN 

meta.code 
h_sc_1mm 
twomass_xsc 
2MASS 
H 1st moment (score) (LCSB: super blk 2,4,8 SNR). 
real 
4 


meta.code 
h_sc_2mm 
twomass_xsc 
2MASS 
H 2nd moment (score) (LCSB: SNRMAX  super SNR max). 
real 
4 


meta.code 
h_sc_msh 
twomass_xsc 
2MASS 
H median shape score. 
real 
4 


meta.code 
h_sc_mxdn 
twomass_xsc 
2MASS 
H mxdn (score) (LCSB: BSNR  block/smoothed SNR). 
real 
4 


meta.code 
h_sc_r1 
twomass_xsc 
2MASS 
H r1 (score). 
real 
4 


meta.code 
h_sc_r23 
twomass_xsc 
2MASS 
H r23 (score) (LCSB: TSNR  integrated SNR for r=15). 
real 
4 


meta.code 
h_sc_sh 
twomass_xsc 
2MASS 
H shape (score). 
real 
4 


meta.code 
h_sc_vint 
twomass_xsc 
2MASS 
H vint (score). 
real 
4 


meta.code 
h_sc_wsh 
twomass_xsc 
2MASS 
H wsh (score) (LCSB: PSNR  peak raw SNR). 
real 
4 


meta.code 
h_seetrack 
twomass_xsc 
2MASS 
H band seetracking score. 
real 
4 


meta.code 
h_sh0 
twomass_xsc 
2MASS 
H ridge shape (LCSB: BSNR limit). 
real 
4 


FIT_PARAM 
h_shape_avg 
twomass_scn 
2MASS 
Hband average seeing shape for scan. 
real 
4 


instr.obsty.seeing 
h_shape_avg 
twomass_sixx2_scn 
2MASS 
H band average seeing shape for scan 
real 
4 



h_shape_rms 
twomass_scn 
2MASS 
RMSerror of Hband average seeing shape. 
real 
4 


instr.obsty.seeing 
h_shape_rms 
twomass_sixx2_scn 
2MASS 
rms of H band avg seeing shape for scan 
real 
4 



h_sig_sh0 
twomass_xsc 
2MASS 
H ridge shape sigma (LCSB: B2SNR limit). 
real 
4 


FIT_PARAM 
h_snr 
twomass_psc 
2MASS 
Hband "scan" signaltonoise ratio. 
real 
4 
mag 

instr.det.noise 
h_snr 
twomass_sixx2_psc 
2MASS 
H band "scan" signaltonoise ratio 
real 
4 



h_subst2 
twomass_xsc 
2MASS 
H residual background #2 (score). 
real 
4 


meta.code 
h_zp_ap 
twomass_scn 
2MASS 
Photometric zeropoint for Hband aperture photometry. 
real 
4 
mag 

phot.mag;arith.zp 
h_zp_ap 
twomass_sixx2_scn 
2MASS 
H band ap. calibration photometric zeropoint for scan 
real 
4 
mag 


h_zperr_ap 
twomass_scn 
2MASS 
RMSerror of zeropoint for Hband aperture photometry 
real 
4 
mag 

stat.error 
h_zperr_ap 
twomass_sixx2_scn 
2MASS 
H band ap. calibration rms error of zeropoint for scan 
real 
4 
mag 


ha 
twomass_scn 
2MASS 
Hour angle at beginning of scan. 
float 
8 
hr 

pos.posAng 
ha 
twomass_sixx2_scn 
2MASS 
beginning hour angle of scan data 
float 
8 
hr 


halfFlux 
svNgc253Detection 
SVNGC253v20100429 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count;em.opt 
halfFlux 
svOrionDetection 
SVORIONv20100429 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count;em.opt 
halfFlux 
ultravistaDetection 
ULTRAVISTAv20100429 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation, not available in SE output {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count;em.opt 
halfFlux 
vhsDetection 
VHSDR1 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count;em.opt 
halfFlux 
vhsDetection 
VHSDR2 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count;em.opt 
halfFlux 
vhsDetection 
VHSDR3 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vhsDetection 
VHSv20120926 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vhsDetection 
VHSv20130417 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vhsDetection 
VHSv20140409 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vhsDetection 
VHSv20150108 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
videoDetection 
VIDEODR2 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation, not available in SE output {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count;em.opt 
halfFlux 
videoDetection 
VIDEODR3 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation, not available in SE output {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
videoDetection 
VIDEODR4 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation, not available in SE output {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
videoDetection 
VIDEOv20100513 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation, not available in SE output {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count;em.opt 
halfFlux 
videoDetection 
VIDEOv20111208 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation, not available in SE output {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count;em.opt 
halfFlux 
vikingDetection 
VIKINGDR2 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count;em.opt 
halfFlux 
vikingDetection 
VIKINGDR3 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vikingDetection 
VIKINGDR4 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vikingDetection 
VIKINGv20110714 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count;em.opt 
halfFlux 
vikingDetection 
VIKINGv20111019 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count;em.opt 
halfFlux 
vikingDetection 
VIKINGv20130417 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vikingDetection 
VIKINGv20140402 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vikingDetection 
VIKINGv20150421 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vmcDetection 
VMCDR1 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count;em.opt 
halfFlux 
vmcDetection 
VMCDR2 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vmcDetection 
VMCDR3 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vmcDetection 
VMCv20110816 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count;em.opt 
halfFlux 
vmcDetection 
VMCv20110909 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count;em.opt 
halfFlux 
vmcDetection 
VMCv20120126 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count;em.opt 
halfFlux 
vmcDetection 
VMCv20121128 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vmcDetection 
VMCv20130304 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vmcDetection 
VMCv20130805 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vmcDetection 
VMCv20140428 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vmcDetection 
VMCv20140903 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vmcDetection 
VMCv20150309 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vvvDetection 
VVVDR1 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vvvDetection 
VVVDR2 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vvvDetection, vvvListRemeasurement 
VVVv20100531 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count;em.opt 
halfFlux 
vvvListRemeasurement 
VVVv20110718 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count;em.opt 
halfFluxErr 
svNgc253Detection 
SVNGC253v20100429 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
svOrionDetection 
SVORIONv20100429 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
ultravistaDetection 
ULTRAVISTAv20100429 
error on Half flux, not available in SE output {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vhsDetection 
VHSDR1 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vhsDetection 
VHSDR2 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vhsDetection 
VHSDR3 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vhsDetection 
VHSv20120926 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vhsDetection 
VHSv20130417 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vhsDetection 
VHSv20140409 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vhsDetection 
VHSv20150108 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
videoDetection 
VIDEODR2 
error on Half flux, not available in SE output {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
videoDetection 
VIDEODR3 
error on Half flux, not available in SE output {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
videoDetection 
VIDEODR4 
error on Half flux, not available in SE output {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
videoDetection 
VIDEOv20100513 
error on Half flux, not available in SE output {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
videoDetection 
VIDEOv20111208 
error on Half flux, not available in SE output {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vikingDetection 
VIKINGDR2 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vikingDetection 
VIKINGDR3 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vikingDetection 
VIKINGDR4 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vikingDetection 
VIKINGv20110714 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vikingDetection 
VIKINGv20111019 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vikingDetection 
VIKINGv20130417 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vikingDetection 
VIKINGv20140402 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vikingDetection 
VIKINGv20150421 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCDR1 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCDR2 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCDR3 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCv20110816 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCv20110909 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCv20120126 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCv20121128 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCv20130304 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCv20130805 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCv20140428 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCv20140903 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCv20150309 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vvvDetection 
VVVDR1 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vvvDetection 
VVVDR2 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vvvDetection, vvvListRemeasurement 
VVVv20100531 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vvvListRemeasurement 
VVVv20110718 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfMag 
svNgc253Detection 
SVNGC253v20100429 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
svOrionDetection 
SVORIONv20100429 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
ultravistaDetection 
ULTRAVISTAv20100429 
Calibrated magnitude within circular aperture halfRad, not available in SE output 
real 
4 
mag 

phot.mag 
halfMag 
vhsDetection 
VHSDR1 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vhsDetection 
VHSDR2 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vhsDetection 
VHSDR3 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vhsDetection 
VHSv20120926 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vhsDetection 
VHSv20130417 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vhsDetection 
VHSv20140409 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vhsDetection 
VHSv20150108 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
videoDetection 
VIDEODR2 
Calibrated magnitude within circular aperture halfRad, not available in SE output 
real 
4 
mag 

phot.mag 
halfMag 
videoDetection 
VIDEODR3 
Calibrated magnitude within circular aperture halfRad, not available in SE output 
real 
4 
mag 

phot.mag 
halfMag 
videoDetection 
VIDEODR4 
Calibrated magnitude within circular aperture halfRad, not available in SE output 
real 
4 
mag 

phot.mag 
halfMag 
videoDetection 
VIDEOv20100513 
Calibrated magnitude within circular aperture halfRad, not available in SE output 
real 
4 
mag 

phot.mag 
halfMag 
videoDetection 
VIDEOv20111208 
Calibrated magnitude within circular aperture halfRad, not available in SE output 
real 
4 
mag 

phot.mag 
halfMag 
vikingDetection 
VIKINGDR2 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vikingDetection 
VIKINGDR3 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vikingDetection 
VIKINGDR4 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vikingDetection 
VIKINGv20110714 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vikingDetection 
VIKINGv20111019 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vikingDetection 
VIKINGv20130417 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vikingDetection 
VIKINGv20140402 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vikingDetection 
VIKINGv20150421 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCDR1 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCDR2 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCDR3 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCv20110816 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCv20110909 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCv20120126 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCv20121128 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCv20130304 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCv20130805 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCv20140428 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCv20140903 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCv20150309 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vvvDetection 
VVVDR1 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vvvDetection 
VVVDR2 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vvvDetection, vvvListRemeasurement 
VVVv20100531 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vvvListRemeasurement 
VVVv20110718 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMagErr 
svNgc253Detection 
SVNGC253v20100429 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
svOrionDetection 
SVORIONv20100429 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
ultravistaDetection 
ULTRAVISTAv20100429 
Calibrated error on Half magnitude, not available in SE output 
real 
4 
mag 

stat.error 
halfMagErr 
vhsDetection 
VHSDR1 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vhsDetection 
VHSDR2 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vhsDetection 
VHSDR3 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vhsDetection 
VHSv20120926 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vhsDetection 
VHSv20130417 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vhsDetection 
VHSv20140409 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vhsDetection 
VHSv20150108 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
videoDetection 
VIDEODR2 
Calibrated error on Half magnitude, not available in SE output 
real 
4 
mag 

stat.error 
halfMagErr 
videoDetection 
VIDEODR3 
Calibrated error on Half magnitude, not available in SE output 
real 
4 
mag 

stat.error 
halfMagErr 
videoDetection 
VIDEODR4 
Calibrated error on Half magnitude, not available in SE output 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
videoDetection 
VIDEOv20100513 
Calibrated error on Half magnitude, not available in SE output 
real 
4 
mag 

stat.error 
halfMagErr 
videoDetection 
VIDEOv20111208 
Calibrated error on Half magnitude, not available in SE output 
real 
4 
mag 

stat.error 
halfMagErr 
vikingDetection 
VIKINGDR2 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vikingDetection 
VIKINGDR3 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vikingDetection 
VIKINGDR4 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vikingDetection 
VIKINGv20110714 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vikingDetection 
VIKINGv20111019 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vikingDetection 
VIKINGv20130417 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vikingDetection 
VIKINGv20140402 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vikingDetection 
VIKINGv20150421 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vmcDetection 
VMCDR1 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vmcDetection 
VMCDR2 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vmcDetection 
VMCDR3 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vmcDetection 
VMCv20110816 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vmcDetection 
VMCv20110909 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vmcDetection 
VMCv20120126 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vmcDetection 
VMCv20121128 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vmcDetection 
VMCv20130304 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vmcDetection 
VMCv20130805 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vmcDetection 
VMCv20140428 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vmcDetection 
VMCv20140903 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vmcDetection 
VMCv20150309 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vvvDetection 
VVVDR1 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vvvDetection 
VVVDR2 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vvvDetection, vvvListRemeasurement 
VVVv20100531 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vvvListRemeasurement 
VVVv20110718 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfRad 
svNgc253Detection 
SVNGC253v20100429 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize;src 
halfRad 
svOrionDetection 
SVORIONv20100429 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize;src 
halfRad 
ultravistaDetection 
ULTRAVISTAv20100429 
SExtractor halflight radius (FRAC_RADIUS), calcuated assuming Kron flux is total flux {catalogue TType keyword: Half_radius} 
real 
4 
pixels 

phys.angSize;src 
halfRad 
vhsDetection 
VHSDR1 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize;src 
halfRad 
vhsDetection 
VHSDR2 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize;src 
halfRad 
vhsDetection 
VHSDR3 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vhsDetection 
VHSv20120926 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vhsDetection 
VHSv20130417 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vhsDetection 
VHSv20140409 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vhsDetection 
VHSv20150108 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
videoDetection 
VIDEODR2 
SExtractor halflight radius (FRAC_RADIUS), calcuated assuming Kron flux is total flux {catalogue TType keyword: Half_radius} 
real 
4 
pixels 

phys.angSize;src 
halfRad 
videoDetection 
VIDEODR3 
SExtractor halflight radius (FRAC_RADIUS), calcuated assuming Kron flux is total flux {catalogue TType keyword: Half_radius} 
real 
4 
pixels 

phys.angSize 
halfRad 
videoDetection 
VIDEODR4 
SExtractor halflight radius (FRAC_RADIUS), calcuated assuming Kron flux is total flux {catalogue TType keyword: Half_radius} 
real 
4 
pixels 

phys.angSize 
halfRad 
videoDetection 
VIDEOv20100513 
SExtractor halflight radius (FRAC_RADIUS), calcuated assuming Kron flux is total flux {catalogue TType keyword: Half_radius} 
real 
4 
pixels 

phys.angSize;src 
halfRad 
videoDetection 
VIDEOv20111208 
SExtractor halflight radius (FRAC_RADIUS), calcuated assuming Kron flux is total flux {catalogue TType keyword: Half_radius} 
real 
4 
pixels 

phys.angSize;src 
halfRad 
vikingDetection 
VIKINGDR2 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize;src 
halfRad 
vikingDetection 
VIKINGDR3 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vikingDetection 
VIKINGDR4 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vikingDetection 
VIKINGv20110714 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize;src 
halfRad 
vikingDetection 
VIKINGv20111019 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize;src 
halfRad 
vikingDetection 
VIKINGv20130417 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vikingDetection 
VIKINGv20140402 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vikingDetection 
VIKINGv20150421 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vmcDetection 
VMCDR1 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize;src 
halfRad 
vmcDetection 
VMCDR2 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vmcDetection 
VMCDR3 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vmcDetection 
VMCv20110816 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize;src 
halfRad 
vmcDetection 
VMCv20110909 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize;src 
halfRad 
vmcDetection 
VMCv20120126 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize;src 
halfRad 
vmcDetection 
VMCv20121128 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vmcDetection 
VMCv20130304 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vmcDetection 
VMCv20130805 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vmcDetection 
VMCv20140428 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vmcDetection 
VMCv20140903 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vmcDetection 
VMCv20150309 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vvvDetection 
VVVDR1 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vvvDetection 
VVVDR2 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vvvDetection, vvvListRemeasurement 
VVVv20100531 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize;src 
halfRad 
vvvListRemeasurement 
VVVv20110718 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize;src 
hAperMag1 
vvvSource 
VVVDR1 
Extended source H aperture corrected mag (0.7 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag1 
vvvSource 
VVVv20100531 
Extended source H aperture corrected mag (0.7 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag1 
vvvSource 
VVVv20110718 
Extended source H aperture corrected mag (0.7 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag1 
vvvSource, vvvSynopticSource 
VVVDR2 
Extended source H aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag1Err 
vvvSource 
VVVDR1 
Error in extended source H mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag1Err 
vvvSource 
VVVv20100531 
Error in extended source H mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag1Err 
vvvSource 
VVVv20110718 
Error in extended source H mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag1Err 
vvvSource, vvvSynopticSource 
VVVDR2 
Error in extended source H mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag2 
vvvSynopticSource 
VVVDR1 
Extended source H aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag2 
vvvSynopticSource 
VVVDR2 
Extended source H aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag2Err 
vvvSynopticSource 
VVVDR1 
Error in extended source H mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag2Err 
vvvSynopticSource 
VVVDR2 
Error in extended source H mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3 
svNgc253Source 
SVNGC253v20100429 
Default point/extended source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
svOrionSource 
SVORIONv20100429 
Default point/extended source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
ultravistaSource 
ULTRAVISTAv20100429 
Default point/extended source H mag, no aperture correction applied If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
vhsSource 
VHSDR1 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
vhsSource 
VHSDR2 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
vhsSource 
VHSDR3 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag3 
vhsSource 
VHSv20120926 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
vhsSource 
VHSv20130417 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
vhsSource 
VHSv20140409 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag3 
vhsSource 
VHSv20150108 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag3 
videoSource 
VIDEODR2 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
videoSource 
VIDEODR3 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
videoSource 
VIDEODR4 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag3 
videoSource 
VIDEOv20100513 
Default point/extended source H mag, no aperture correction applied If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
videoSource 
VIDEOv20111208 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
vikingSource 
VIKINGDR2 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
vikingSource 
VIKINGDR3 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
vikingSource 
VIKINGDR4 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag3 
vikingSource 
VIKINGv20110714 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
vikingSource 
VIKINGv20111019 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
vikingSource 
VIKINGv20130417 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
vikingSource 
VIKINGv20140402 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag3 
vikingSource 
VIKINGv20150421 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag3 
vvvSource 
VVVDR1 
Default point/extended source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
vvvSource 
VVVDR2 
Default point/extended source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag3 
vvvSource 
VVVv20100531 
Default point/extended source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
vvvSource 
VVVv20110718 
Default point/extended source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
vvvSynopticSource 
VVVDR1 
Default point/extended source H aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
vvvSynopticSource 
VVVDR2 
Default point/extended source H aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag3Err 
svNgc253Source 
SVNGC253v20100429 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
svOrionSource 
SVORIONv20100429 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
ultravistaSource 
ULTRAVISTAv20100429 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
vhsSource 
VHSDR1 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
vhsSource 
VHSDR2 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
vhsSource 
VHSDR3 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
hAperMag3Err 
vhsSource 
VHSv20120926 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
vhsSource 
VHSv20130417 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
vhsSource 
VHSv20140409 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
hAperMag3Err 
vhsSource 
VHSv20150108 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;phot.mag 
hAperMag3Err 
videoSource 
VIDEODR2 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
videoSource 
VIDEODR3 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
videoSource 
VIDEODR4 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;phot.mag 
hAperMag3Err 
videoSource 
VIDEOv20100513 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
videoSource 
VIDEOv20111208 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
vikingSource 
VIKINGDR2 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
vikingSource 
VIKINGDR3 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
vikingSource 
VIKINGDR4 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
hAperMag3Err 
vikingSource 
VIKINGv20110714 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
vikingSource 
VIKINGv20111019 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
vikingSource 
VIKINGv20130417 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
vikingSource 
VIKINGv20140402 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
vikingSource 
VIKINGv20150421 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;phot.mag 
hAperMag3Err 
vvvSource 
VVVDR2 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
vvvSource 
VVVv20100531 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
vvvSource 
VVVv20110718 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
vvvSource, vvvSynopticSource 
VVVDR1 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4 
svNgc253Source 
SVNGC253v20100429 
Extended source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
svOrionSource 
SVORIONv20100429 
Extended source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
ultravistaSource 
ULTRAVISTAv20100429 
Extended source H mag, no aperture correction applied 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
vhsSource 
VHSDR1 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
vhsSource 
VHSDR2 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
vhsSource 
VHSDR3 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag4 
vhsSource 
VHSv20120926 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
vhsSource 
VHSv20130417 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
vhsSource 
VHSv20140409 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag4 
vhsSource 
VHSv20150108 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag4 
videoSource 
VIDEODR2 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
videoSource 
VIDEODR3 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
videoSource 
VIDEODR4 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag4 
videoSource 
VIDEOv20100513 
Extended source H mag, no aperture correction applied 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
videoSource 
VIDEOv20111208 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
vikingSource 
VIKINGDR2 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
vikingSource 
VIKINGDR3 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
vikingSource 
VIKINGDR4 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag4 
vikingSource 
VIKINGv20110714 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
vikingSource 
VIKINGv20111019 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
vikingSource 
VIKINGv20130417 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
vikingSource 
VIKINGv20140402 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag4 
vikingSource 
VIKINGv20150421 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag4 
vvvSource 
VVVDR2 
Extended source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag4 
vvvSource 
VVVv20100531 
Extended source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
vvvSource 
VVVv20110718 
Extended source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
vvvSource, vvvSynopticSource 
VVVDR1 
Extended source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4Err 
svNgc253Source 
SVNGC253v20100429 
Error in extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
svOrionSource 
SVORIONv20100429 
Error in extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
ultravistaSource 
ULTRAVISTAv20100429 
Error in extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
vhsSource 
VHSDR1 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
vhsSource 
VHSDR2 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
vhsSource 
VHSDR3 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
hAperMag4Err 
vhsSource 
VHSv20120926 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
vhsSource 
VHSv20130417 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
vhsSource 
VHSv20140409 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
hAperMag4Err 
vhsSource 
VHSv20150108 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;phot.mag 
hAperMag4Err 
videoSource 
VIDEODR2 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
videoSource 
VIDEODR3 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
videoSource 
VIDEODR4 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;phot.mag 
hAperMag4Err 
videoSource 
VIDEOv20100513 
Error in extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
videoSource 
VIDEOv20111208 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
vikingSource 
VIKINGDR2 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
vikingSource 
VIKINGDR3 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
vikingSource 
VIKINGDR4 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
hAperMag4Err 
vikingSource 
VIKINGv20110714 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
vikingSource 
VIKINGv20111019 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
vikingSource 
VIKINGv20130417 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
vikingSource 
VIKINGv20140402 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
vikingSource 
VIKINGv20150421 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;phot.mag 
hAperMag4Err 
vvvSource 
VVVDR2 
Error in extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
vvvSource 
VVVv20100531 
Error in extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
vvvSource 
VVVv20110718 
Error in extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
vvvSource, vvvSynopticSource 
VVVDR1 
Error in extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag5 
vvvSynopticSource 
VVVDR1 
Extended source H aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag5 
vvvSynopticSource 
VVVDR2 
Extended source H aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag5Err 
vvvSynopticSource 
VVVDR1 
Error in extended source H mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag5Err 
vvvSynopticSource 
VVVDR2 
Error in extended source H mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6 
svNgc253Source 
SVNGC253v20100429 
Extended source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag6 
svOrionSource 
SVORIONv20100429 
Extended source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag6 
ultravistaSource 
ULTRAVISTAv20100429 
Extended source H mag, no aperture correction applied 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag6 
vhsSource 
VHSDR1 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag6 
vhsSource 
VHSDR2 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag6 
vhsSource 
VHSDR3 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag6 
vhsSource 
VHSv20120926 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag6 
vhsSource 
VHSv20130417 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag6 
vhsSource 
VHSv20140409 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag6 
vhsSource 
VHSv20150108 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag6 
videoSource 
VIDEODR2 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag6 
videoSource 
VIDEODR3 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag6 
videoSource 
VIDEODR4 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag6 
videoSource 
VIDEOv20100513 
Extended source H mag, no aperture correction applied 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag6 
videoSource 
VIDEOv20111208 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag6 
vikingSource 
VIKINGDR2 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag6 
vikingSource 
VIKINGDR3 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag6 
vikingSource 
VIKINGDR4 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag6 
vikingSource 
VIKINGv20110714 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag6 
vikingSource 
VIKINGv20111019 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag6 
vikingSource 
VIKINGv20130417 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag6 
vikingSource 
VIKINGv20140402 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag6 
vikingSource 
VIKINGv20150421 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag6Err 
svNgc253Source 
SVNGC253v20100429 
Error in extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6Err 
svOrionSource 
SVORIONv20100429 
Error in extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6Err 
ultravistaSource 
ULTRAVISTAv20100429 
Error in extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6Err 
vhsSource 
VHSDR1 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6Err 
vhsSource 
VHSDR2 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6Err 
vhsSource 
VHSDR3 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
hAperMag6Err 
vhsSource 
VHSv20120926 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6Err 
vhsSource 
VHSv20130417 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6Err 
vhsSource 
VHSv20140409 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
hAperMag6Err 
vhsSource 
VHSv20150108 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;phot.mag 
hAperMag6Err 
videoSource 
VIDEODR2 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6Err 
videoSource 
VIDEODR3 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6Err 
videoSource 
VIDEODR4 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;phot.mag 
hAperMag6Err 
videoSource 
VIDEOv20100513 
Error in extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6Err 
videoSource 
VIDEOv20111208 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6Err 
vikingSource 
VIKINGDR2 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6Err 
vikingSource 
VIKINGDR3 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6Err 
vikingSource 
VIKINGDR4 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
hAperMag6Err 
vikingSource 
VIKINGv20110714 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6Err 
vikingSource 
VIKINGv20111019 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6Err 
vikingSource 
VIKINGv20130417 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6Err 
vikingSource 
VIKINGv20140402 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6Err 
vikingSource 
VIKINGv20150421 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;phot.mag 
hAperMagNoAperCorr3 
vhsSource 
VHSDR1 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr3 
vhsSource 
VHSDR2 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr3 
vhsSource 
VHSDR3 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr3 
vhsSource 
VHSv20120926 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr3 
vhsSource 
VHSv20130417 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr3 
vhsSource 
VHSv20140409 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr3 
vhsSource 
VHSv20150108 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr3 
videoSource 
VIDEODR2 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr3 
videoSource 
VIDEODR3 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr3 
videoSource 
VIDEODR4 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr3 
videoSource 
VIDEOv20111208 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr3 
vikingSource 
VIKINGDR2 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr3 
vikingSource 
VIKINGDR3 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr3 
vikingSource 
VIKINGDR4 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr3 
vikingSource 
VIKINGv20110714 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr3 
vikingSource 
VIKINGv20111019 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr3 
vikingSource 
VIKINGv20130417 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr3 
vikingSource 
VIKINGv20140402 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr3 
vikingSource 
VIKINGv20150421 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr4 
vhsSource 
VHSDR1 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr4 
vhsSource 
VHSDR2 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr4 
vhsSource 
VHSDR3 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr4 
vhsSource 
VHSv20120926 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr4 
vhsSource 
VHSv20130417 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr4 
vhsSource 
VHSv20140409 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr4 
vhsSource 
VHSv20150108 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr4 
videoSource 
VIDEODR2 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr4 
videoSource 
VIDEODR3 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr4 
videoSource 
VIDEODR4 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr4 
videoSource 
VIDEOv20111208 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr4 
vikingSource 
VIKINGDR2 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr4 
vikingSource 
VIKINGDR3 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr4 
vikingSource 
VIKINGDR4 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr4 
vikingSource 
VIKINGv20110714 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr4 
vikingSource 
VIKINGv20111019 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr4 
vikingSource 
VIKINGv20130417 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr4 
vikingSource 
VIKINGv20140402 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr4 
vikingSource 
VIKINGv20150421 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr6 
vhsSource 
VHSDR1 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr6 
vhsSource 
VHSDR2 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr6 
vhsSource 
VHSDR3 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr6 
vhsSource 
VHSv20120926 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr6 
vhsSource 
VHSv20130417 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr6 
vhsSource 
VHSv20140409 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr6 
vhsSource 
VHSv20150108 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr6 
videoSource 
VIDEODR2 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr6 
videoSource 
VIDEODR3 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr6 
videoSource 
VIDEODR4 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr6 
videoSource 
VIDEOv20111208 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr6 
vikingSource 
VIKINGDR2 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr6 
vikingSource 
VIKINGDR3 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr6 
vikingSource 
VIKINGDR4 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr6 
vikingSource 
VIKINGv20110714 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr6 
vikingSource 
VIKINGv20111019 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr6 
vikingSource 
VIKINGv20130417 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr6 
vikingSource 
VIKINGv20140402 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr6 
vikingSource 
VIKINGv20150421 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
haStratAst 
videoVarFrameSetInfo 
VIDEODR2 
Strateva parameter, a, in fit to astrometric rms vs magnitude in H 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. 
haStratAst 
videoVarFrameSetInfo 
VIDEODR3 
Strateva parameter, a, in fit to astrometric rms vs magnitude in H 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. 
haStratAst 
videoVarFrameSetInfo 
VIDEODR4 
Strateva parameter, a, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
haStratAst 
videoVarFrameSetInfo 
VIDEOv20100513 
Strateva parameter, a, in fit to astrometric rms vs magnitude in H 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. 
haStratAst 
videoVarFrameSetInfo 
VIDEOv20111208 
Strateva parameter, a, in fit to astrometric rms vs magnitude in H 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. 
haStratAst 
vikingVarFrameSetInfo 
VIKINGDR2 
Strateva parameter, a, in fit to astrometric rms vs magnitude in H 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. 
haStratAst 
vikingVarFrameSetInfo 
VIKINGv20110714 
Strateva parameter, a, in fit to astrometric rms vs magnitude in H 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. 
haStratAst 
vikingVarFrameSetInfo 
VIKINGv20111019 
Strateva parameter, a, in fit to astrometric rms vs magnitude in H 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. 
haStratAst 
vvvVarFrameSetInfo 
VVVv20100531 
Strateva parameter, a, in fit to astrometric rms vs magnitude in H 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. 
haStratPht 
videoVarFrameSetInfo 
VIDEODR2 
Strateva parameter, a, in fit to photometric rms vs magnitude in H 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. 
haStratPht 
videoVarFrameSetInfo 
VIDEODR3 
Strateva parameter, a, in fit to photometric rms vs magnitude in H 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. 
haStratPht 
videoVarFrameSetInfo 
VIDEODR4 
Strateva parameter, a, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
haStratPht 
videoVarFrameSetInfo 
VIDEOv20100513 
Strateva parameter, a, in fit to photometric rms vs magnitude in H 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. 
haStratPht 
videoVarFrameSetInfo 
VIDEOv20111208 
Strateva parameter, a, in fit to photometric rms vs magnitude in H 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. 
haStratPht 
vikingVarFrameSetInfo 
VIKINGDR2 
Strateva parameter, a, in fit to photometric rms vs magnitude in H 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. 
haStratPht 
vikingVarFrameSetInfo 
VIKINGv20110714 
Strateva parameter, a, in fit to photometric rms vs magnitude in H 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. 
haStratPht 
vikingVarFrameSetInfo 
VIKINGv20111019 
Strateva parameter, a, in fit to photometric rms vs magnitude in H 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. 
haStratPht 
vvvVarFrameSetInfo 
VVVv20100531 
Strateva parameter, a, in fit to photometric rms vs magnitude in H 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. 
hAverageConf 
svNgc253Source 
SVNGC253v20100429 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

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

99999999 
meta.code 
hAverageConf 
vhsSource 
VHSDR1 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

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

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

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

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

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

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

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

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

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

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

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

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

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

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

0.9999995e9 
stat.likelihood;em.IR.H 
hAverageConf 
vvvSource 
VVVDR2 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

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

99999999 
stat.likelihood;em.IR.NIR 
hbestAper 
videoVariability 
VIDEODR2 
Best aperture (16) for photometric statistics in the H 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) 
hbestAper 
videoVariability 
VIDEODR3 
Best aperture (16) for photometric statistics in the H 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) 
hbestAper 
videoVariability 
VIDEODR4 
Best aperture (16) for photometric statistics in the H band 
int 
4 

9999 
meta.code.class;em.IR.H 
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) 
hbestAper 
videoVariability 
VIDEOv20100513 
Best aperture (16) for photometric statistics in the H 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) 
hbestAper 
videoVariability 
VIDEOv20111208 
Best aperture (16) for photometric statistics in the H 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) 
hbestAper 
vikingVariability 
VIKINGDR2 
Best aperture (16) for photometric statistics in the H 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) 
hbestAper 
vikingVariability 
VIKINGv20110714 
Best aperture (16) for photometric statistics in the H 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) 
hbestAper 
vikingVariability 
VIKINGv20111019 
Best aperture (16) for photometric statistics in the H 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) 
hbestAper 
vvvVariability 
VVVv20100531 
Best aperture (16) for photometric statistics in the H 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) 
hbStratAst 
videoVarFrameSetInfo 
VIDEODR2 
Strateva parameter, b, in fit to astrometric rms vs magnitude in H 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. 
hbStratAst 
videoVarFrameSetInfo 
VIDEODR3 
Strateva parameter, b, in fit to astrometric rms vs magnitude in H 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. 
hbStratAst 
videoVarFrameSetInfo 
VIDEODR4 
Strateva parameter, b, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hbStratAst 
videoVarFrameSetInfo 
VIDEOv20100513 
Strateva parameter, b, in fit to astrometric rms vs magnitude in H 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. 
hbStratAst 
videoVarFrameSetInfo 
VIDEOv20111208 
Strateva parameter, b, in fit to astrometric rms vs magnitude in H 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. 
hbStratAst 
vikingVarFrameSetInfo 
VIKINGDR2 
Strateva parameter, b, in fit to astrometric rms vs magnitude in H 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. 
hbStratAst 
vikingVarFrameSetInfo 
VIKINGv20110714 
Strateva parameter, b, in fit to astrometric rms vs magnitude in H 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. 
hbStratAst 
vikingVarFrameSetInfo 
VIKINGv20111019 
Strateva parameter, b, in fit to astrometric rms vs magnitude in H 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. 
hbStratAst 
vvvVarFrameSetInfo 
VVVv20100531 
Strateva parameter, b, in fit to astrometric rms vs magnitude in H 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. 
hbStratPht 
videoVarFrameSetInfo 
VIDEODR2 
Strateva parameter, b, in fit to photometric rms vs magnitude in H 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. 
hbStratPht 
videoVarFrameSetInfo 
VIDEODR3 
Strateva parameter, b, in fit to photometric rms vs magnitude in H 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. 
hbStratPht 
videoVarFrameSetInfo 
VIDEODR4 
Strateva parameter, b, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hbStratPht 
videoVarFrameSetInfo 
VIDEOv20100513 
Strateva parameter, b, in fit to photometric rms vs magnitude in H 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. 
hbStratPht 
videoVarFrameSetInfo 
VIDEOv20111208 
Strateva parameter, b, in fit to photometric rms vs magnitude in H 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. 
hbStratPht 
vikingVarFrameSetInfo 
VIKINGDR2 
Strateva parameter, b, in fit to photometric rms vs magnitude in H 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. 
hbStratPht 
vikingVarFrameSetInfo 
VIKINGv20110714 
Strateva parameter, b, in fit to photometric rms vs magnitude in H 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. 
hbStratPht 
vikingVarFrameSetInfo 
VIKINGv20111019 
Strateva parameter, b, in fit to photometric rms vs magnitude in H 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. 
hbStratPht 
vvvVarFrameSetInfo 
VVVv20100531 
Strateva parameter, b, in fit to photometric rms vs magnitude in H 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. 
hchiSqAst 
videoVarFrameSetInfo 
VIDEODR2 
Goodness of fit of Strateva function to astrometric data in H 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. 
hchiSqAst 
videoVarFrameSetInfo 
VIDEODR3 
Goodness of fit of Strateva function to astrometric data in H 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. 
hchiSqAst 
videoVarFrameSetInfo 
VIDEODR4 
Goodness of fit of Strateva function to astrometric data in H band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.H 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hchiSqAst 
videoVarFrameSetInfo 
VIDEOv20100513 
Goodness of fit of Strateva function to astrometric data in H 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. 
hchiSqAst 
videoVarFrameSetInfo 
VIDEOv20111208 
Goodness of fit of Strateva function to astrometric data in H 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. 
hchiSqAst 
vikingVarFrameSetInfo 
VIKINGDR2 
Goodness of fit of Strateva function to astrometric data in H 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. 
hchiSqAst 
vikingVarFrameSetInfo 
VIKINGv20110714 
Goodness of fit of Strateva function to astrometric data in H 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. 
hchiSqAst 
vikingVarFrameSetInfo 
VIKINGv20111019 
Goodness of fit of Strateva function to astrometric data in H 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. 
hchiSqAst 
vvvVarFrameSetInfo 
VVVv20100531 
Goodness of fit of Strateva function to astrometric data in H 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. 
hchiSqpd 
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. 
hchiSqpd 
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. 
hchiSqpd 
videoVariability 
VIDEODR4 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2;em.IR.H 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hchiSqpd 
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. 
hchiSqpd 
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. 
hchiSqpd 
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. 
hchiSqpd 
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. 
hchiSqpd 
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. 
hchiSqpd 
vvvVariability 
VVVv20100531 
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. 
hchiSqPht 
videoVarFrameSetInfo 
VIDEODR2 
Goodness of fit of Strateva function to photometric data in H 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. 
hchiSqPht 
videoVarFrameSetInfo 
VIDEODR3 
Goodness of fit of Strateva function to photometric data in H 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. 
hchiSqPht 
videoVarFrameSetInfo 
VIDEODR4 
Goodness of fit of Strateva function to photometric data in H band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.H 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hchiSqPht 
videoVarFrameSetInfo 
VIDEOv20100513 
Goodness of fit of Strateva function to photometric data in H 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. 
hchiSqPht 
videoVarFrameSetInfo 
VIDEOv20111208 
Goodness of fit of Strateva function to photometric data in H 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. 
hchiSqPht 
vikingVarFrameSetInfo 
VIKINGDR2 
Goodness of fit of Strateva function to photometric data in H 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. 
hchiSqPht 
vikingVarFrameSetInfo 
VIKINGv20110714 
Goodness of fit of Strateva function to photometric data in H 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. 
hchiSqPht 
vikingVarFrameSetInfo 
VIKINGv20111019 
Goodness of fit of Strateva function to photometric data in H 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. 
hchiSqPht 
vvvVarFrameSetInfo 
VVVv20100531 
Goodness of fit of Strateva function to photometric data in H 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. 
hClass 
svNgc253Source 
SVNGC253v20100429 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
svOrionSource 
SVORIONv20100429 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
ultravistaSource, ultravistaSourceRemeasurement 
ULTRAVISTAv20100429 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
vhsSource 
VHSDR2 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
vhsSource 
VHSDR3 
discrete image classification flag in H 
smallint 
2 

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

9999 
src.class 
hClass 
vhsSource 
VHSv20130417 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
vhsSource 
VHSv20140409 
discrete image classification flag in H 
smallint 
2 

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

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

9999 
src.class 
hClass 
videoSource 
VIDEODR2 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
videoSource 
VIDEODR3 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
videoSource 
VIDEODR4 
discrete image classification flag in H 
smallint 
2 

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

9999 
src.class 
hClass 
videoSource, videoSourceRemeasurement 
VIDEOv20100513 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
vikingSource 
VIKINGDR2 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
vikingSource 
VIKINGDR3 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
vikingSource 
VIKINGDR4 
discrete image classification flag in H 
smallint 
2 

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

9999 
src.class 
hClass 
vikingSource 
VIKINGv20130417 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
vikingSource 
VIKINGv20140402 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
vikingSource 
VIKINGv20150421 
discrete image classification flag in H 
smallint 
2 

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

9999 
src.class 
hClass 
vvvSource 
VVVDR2 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
vvvSource 
VVVv20110718 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
vvvSource, vvvSourceRemeasurement 
VVVv20100531 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
vvvSource, vvvSynopticSource 
VVVDR1 
discrete image classification flag in H 
smallint 
2 

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

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

0.9999995e9 
stat 
hClassStat 
ultravistaSource 
ULTRAVISTAv20100429 
SExtractor classification statistic in H 
real 
4 

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

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

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

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

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

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

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

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

0.9999995e9 
stat 
hClassStat 
videoSource 
VIDEODR2 
SExtractor classification statistic in H 
real 
4 

0.9999995e9 
stat 
hClassStat 
videoSource 
VIDEODR3 
SExtractor classification statistic in H 
real 
4 

0.9999995e9 
stat 
hClassStat 
videoSource 
VIDEODR4 
SExtractor classification statistic in H 
real 
4 

0.9999995e9 
stat;em.IR.H 
hClassStat 
videoSource 
VIDEOv20100513 
SExtractor classification statistic in H 
real 
4 

0.9999995e9 
stat 
hClassStat 
videoSource 
VIDEOv20111208 
SExtractor classification statistic in H 
real 
4 

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

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

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

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

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

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

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

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

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

0.9999995e9 
stat 
hClassStat 
vvvSource 
VVVDR1 
SExtractor classification statistic in H 
real 
4 

0.9999995e9 
stat 
hClassStat 
vvvSource 
VVVDR2 
SExtractor classification statistic in H 
real 
4 

0.9999995e9 
stat 
hClassStat 
vvvSource 
VVVv20100531 
SExtractor classification statistic in H 
real 
4 

0.9999995e9 
stat 
hClassStat 
vvvSource 
VVVv20110718 
SExtractor classification statistic in H 
real 
4 

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

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

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

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

0.9999995e9 
stat 
hcStratAst 
videoVarFrameSetInfo 
VIDEODR2 
Strateva parameter, c, in fit to astrometric rms vs magnitude in H 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. 
hcStratAst 
videoVarFrameSetInfo 
VIDEODR3 
Strateva parameter, c, in fit to astrometric rms vs magnitude in H 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. 
hcStratAst 
videoVarFrameSetInfo 
VIDEODR4 
Strateva parameter, c, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hcStratAst 
videoVarFrameSetInfo 
VIDEOv20100513 
Strateva parameter, c, in fit to astrometric rms vs magnitude in H 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. 
hcStratAst 
videoVarFrameSetInfo 
VIDEOv20111208 
Strateva parameter, c, in fit to astrometric rms vs magnitude in H 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. 
hcStratAst 
vikingVarFrameSetInfo 
VIKINGDR2 
Strateva parameter, c, in fit to astrometric rms vs magnitude in H 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. 
hcStratAst 
vikingVarFrameSetInfo 
VIKINGv20110714 
Strateva parameter, c, in fit to astrometric rms vs magnitude in H 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. 
hcStratAst 
vikingVarFrameSetInfo 
VIKINGv20111019 
Strateva parameter, c, in fit to astrometric rms vs magnitude in H 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. 
hcStratAst 
vvvVarFrameSetInfo 
VVVv20100531 
Strateva parameter, c, in fit to astrometric rms vs magnitude in H 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. 
hcStratPht 
videoVarFrameSetInfo 
VIDEODR2 
Strateva parameter, c, in fit to photometric rms vs magnitude in H 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. 
hcStratPht 
videoVarFrameSetInfo 
VIDEODR3 
Strateva parameter, c, in fit to photometric rms vs magnitude in H 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. 
hcStratPht 
videoVarFrameSetInfo 
VIDEODR4 
Strateva parameter, c, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hcStratPht 
videoVarFrameSetInfo 
VIDEOv20100513 
Strateva parameter, c, in fit to photometric rms vs magnitude in H 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. 
hcStratPht 
videoVarFrameSetInfo 
VIDEOv20111208 
Strateva parameter, c, in fit to photometric rms vs magnitude in H 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. 
hcStratPht 
vikingVarFrameSetInfo 
VIKINGDR2 
Strateva parameter, c, in fit to photometric rms vs magnitude in H 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. 
hcStratPht 
vikingVarFrameSetInfo 
VIKINGv20110714 
Strateva parameter, c, in fit to photometric rms vs magnitude in H 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. 
hcStratPht 
vikingVarFrameSetInfo 
VIKINGv20111019 
Strateva parameter, c, in fit to photometric rms vs magnitude in H 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. 
hcStratPht 
vvvVarFrameSetInfo 
VVVv20100531 
Strateva parameter, c, in fit to photometric rms vs magnitude in H 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. 
hDeblend 
ultravistaSource, ultravistaSourceRemeasurement 
ULTRAVISTAv20100429 
placeholder flag indicating parent/child relation in H 
int 
4 

99999999 
meta.code 
hDeblend 
vhsSourceRemeasurement 
VHSDR1 
placeholder flag indicating parent/child relation in H 
int 
4 

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

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

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

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

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

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

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

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

0.9999995e9 
src.ellipticity 
hEll 
vhsSource 
VHSDR2 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

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

0.9999995e9 
src.ellipticity;em.IR.H 
hEll 
vhsSource 
VHSv20120926 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity 
hEll 
vhsSource 
VHSv20130417 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity 
hEll 
vhsSource 
VHSv20140409 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.H 
hEll 
vhsSource 
VHSv20150108 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.H 
hEll 
vhsSource, vhsSourceRemeasurement 
VHSDR1 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

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

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

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

0.9999995e9 
src.ellipticity;em.IR.H 
hEll 
videoSource 
VIDEOv20111208 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

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

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

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

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

0.9999995e9 
src.ellipticity;em.IR.H 
hEll 
vikingSource 
VIKINGv20111019 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

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

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

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

0.9999995e9 
src.ellipticity;em.IR.H 
hEll 
vikingSource, vikingSourceRemeasurement 
VIKINGv20110714 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

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

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

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

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

0.9999995e9 
src.ellipticity 
hemis 
twomass_psc 
2MASS 
Hemisphere code for the TWOMASS Observatory from which this source was observed. 
varchar 
1 


meta.code;obs 
hemis 
twomass_scn 
2MASS 
Observatory from which data were obtained: "n" = north = Mt. Hopkins, "s" = south = Cerro Tololo. 
varchar 
1 


meta.code;obs 
hemis 
twomass_sixx2_scn 
2MASS 
hemisphere (N/S) of observation 
varchar 
1 



hemis 
twomass_xsc 
2MASS 
hemisphere (N/S) of observation. "n" = North/Mt. Hopkins; "s" = South/CTIO. 
varchar 
1 


meta.code;obs 
heNum 
svNgc253MergeLog 
SVNGC253v20100429 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
svOrionMergeLog 
SVORIONv20100429 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
ultravistaMergeLog 
ULTRAVISTAv20100429 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
vhsMergeLog 
VHSDR1 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
vhsMergeLog 
VHSDR2 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
vhsMergeLog 
VHSDR3 
the extension number of this H frame 
tinyint 
1 


meta.number;em.IR.H 
heNum 
vhsMergeLog 
VHSv20120926 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
vhsMergeLog 
VHSv20130417 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
vhsMergeLog 
VHSv20140409 
the extension number of this H frame 
tinyint 
1 


meta.number;em.IR.H 
heNum 
vhsMergeLog 
VHSv20150108 
the extension number of this H frame 
tinyint 
1 


meta.number;em.IR.H 
heNum 
videoMergeLog 
VIDEODR2 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
videoMergeLog 
VIDEODR3 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
videoMergeLog 
VIDEODR4 
the extension number of this H frame 
tinyint 
1 


meta.number;em.IR.H 
heNum 
videoMergeLog 
VIDEOv20100513 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
videoMergeLog 
VIDEOv20111208 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
vikingMergeLog 
VIKINGDR2 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
vikingMergeLog 
VIKINGDR3 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
vikingMergeLog 
VIKINGDR4 
the extension number of this H frame 
tinyint 
1 


meta.number;em.IR.H 
heNum 
vikingMergeLog 
VIKINGv20110714 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
vikingMergeLog 
VIKINGv20111019 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
vikingMergeLog 
VIKINGv20130417 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
vikingMergeLog 
VIKINGv20140402 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
vikingMergeLog 
VIKINGv20150421 
the extension number of this H frame 
tinyint 
1 


meta.number;em.IR.H 
heNum 
vvvMergeLog 
VVVDR2 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
vvvMergeLog 
VVVv20100531 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
vvvMergeLog 
VVVv20110718 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
vvvMergeLog, vvvSynopticMergeLog 
VVVDR1 
the extension number of this H frame 
tinyint 
1 


meta.number 
hErrBits 
svNgc253Source 
SVNGC253v20100429 
processing warning/error bitwise flags in H 
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. 
hErrBits 
svOrionSource 
SVORIONv20100429 
processing warning/error bitwise flags in H 
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. 
hErrBits 
ultravistaSource 
ULTRAVISTAv20100429 
processing warning/error bitwise flags in H 
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  

hErrBits 
ultravistaSourceRemeasurement 
ULTRAVISTAv20100429 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code 
hErrBits 
vhsSource 
VHSDR1 
processing warning/error bitwise flags in H 
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. 
hErrBits 
vhsSource 
VHSDR2 
processing warning/error bitwise flags in H 
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. 
hErrBits 
vhsSource 
VHSDR3 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code;em.IR.H 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vhsSource 
VHSv20120926 
processing warning/error bitwise flags in H 
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. 
hErrBits 
vhsSource 
VHSv20130417 
processing warning/error bitwise flags in H 
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. 
hErrBits 
vhsSource 
VHSv20140409 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code;em.IR.H 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vhsSource 
VHSv20150108 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code;em.IR.H 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vhsSourceRemeasurement 
VHSDR1 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code 
hErrBits 
videoSource 
VIDEODR2 
processing warning/error bitwise flags in H 
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  

hErrBits 
videoSource 
VIDEODR3 
processing warning/error bitwise flags in H 
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  

hErrBits 
videoSource 
VIDEODR4 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code;em.IR.H 
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  

hErrBits 
videoSource 
VIDEOv20100513 
processing warning/error bitwise flags in H 
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  

hErrBits 
videoSource 
VIDEOv20111208 
processing warning/error bitwise flags in H 
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  

hErrBits 
videoSourceRemeasurement 
VIDEOv20100513 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code 
hErrBits 
vikingSource 
VIKINGDR2 
processing warning/error bitwise flags in H 
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. 
hErrBits 
vikingSource 
VIKINGDR3 
processing warning/error bitwise flags in H 
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. 
hErrBits 
vikingSource 
VIKINGDR4 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code;em.IR.H 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vikingSource 
VIKINGv20110714 
processing warning/error bitwise flags in H 
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. 
hErrBits 
vikingSource 
VIKINGv20111019 
processing warning/error bitwise flags in H 
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. 
hErrBits 
vikingSource 
VIKINGv20130417 
processing warning/error bitwise flags in H 
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. 
hErrBits 
vikingSource 
VIKINGv20140402 
processing warning/error bitwise flags in H 
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. 
hErrBits 
vikingSource 
VIKINGv20150421 
processing warning/error bitwise flags in H 
int 
4 

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

99999999 
meta.code 
hErrBits 
vikingSourceRemeasurement 
VIKINGv20111019 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code 
hErrBits 
vvvSource 
VVVDR2 
processing warning/error bitwise flags in H 
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. 
hErrBits 
vvvSource 
VVVv20100531 
processing warning/error bitwise flags in H 
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. 
hErrBits 
vvvSource 
VVVv20110718 
processing warning/error bitwise flags in H 
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. 
hErrBits 
vvvSource, vvvSynopticSource 
VVVDR1 
processing warning/error bitwise flags in H 
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. 
hErrBits 
vvvSourceRemeasurement 
VVVv20100531 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code 
hErrBits 
vvvSourceRemeasurement 
VVVv20110718 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code 
hEta 
svNgc253Source 
SVNGC253v20100429 
Offset of H 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. 
hEta 
svOrionSource 
SVORIONv20100429 
Offset of H 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. 
hEta 
ultravistaSource 
ULTRAVISTAv20100429 
Offset of H 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. 
hEta 
vhsSource 
VHSDR1 
Offset of H 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. 
hEta 
vhsSource 
VHSDR2 
Offset of H 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. 
hEta 
vhsSource 
VHSDR3 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.H 
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. 
hEta 
vhsSource 
VHSv20120926 
Offset of H 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. 
hEta 
vhsSource 
VHSv20130417 
Offset of H 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. 
hEta 
vhsSource 
VHSv20140409 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.H 
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. 
hEta 
vhsSource 
VHSv20150108 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.H 
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. 
hEta 
videoSource 
VIDEODR2 
Offset of H 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. 
hEta 
videoSource 
VIDEODR3 
Offset of H 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. 
hEta 
videoSource 
VIDEODR4 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.H 
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. 
hEta 
videoSource 
VIDEOv20100513 
Offset of H 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. 
hEta 
videoSource 
VIDEOv20111208 
Offset of H 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. 
hEta 
vikingSource 
VIKINGDR2 
Offset of H 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. 
hEta 
vikingSource 
VIKINGDR3 
Offset of H 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. 
hEta 
vikingSource 
VIKINGDR4 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.H 
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. 
hEta 
vikingSource 
VIKINGv20110714 
Offset of H 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. 
hEta 
vikingSource 
VIKINGv20111019 
Offset of H 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. 
hEta 
vikingSource 
VIKINGv20130417 
Offset of H 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. 
hEta 
vikingSource 
VIKINGv20140402 
Offset of H 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. 
hEta 
vikingSource 
VIKINGv20150421 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.H 
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. 
hEta 
vvvSource 
VVVDR2 
Offset of H 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. 
hEta 
vvvSource 
VVVv20100531 
Offset of H 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. 
hEta 
vvvSource 
VVVv20110718 
Offset of H 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. 
hEta 
vvvSource, vvvSynopticSource 
VVVDR1 
Offset of H 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. 
hexpML 
videoVarFrameSetInfo 
VIDEODR2 
Expected magnitude limit of frameSet in this in H band. 
real 
4 

0.9999995e9 

hexpML 
videoVarFrameSetInfo 
VIDEODR3 
Expected magnitude limit of frameSet in this in H band. 
real 
4 

0.9999995e9 
phot.mag;stat.max;em.IR.NIR 
hexpML 
videoVarFrameSetInfo 
VIDEODR4 
Expected magnitude limit of frameSet in this in H band. 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H;stat.max 
hexpML 
videoVarFrameSetInfo 
VIDEOv20100513 
Expected magnitude limit of frameSet in this in H band. 
real 
4 

0.9999995e9 

hexpML 
videoVarFrameSetInfo 
VIDEOv20111208 
Expected magnitude limit of frameSet in this in H band. 
real 
4 

0.9999995e9 

hexpML 
vikingVarFrameSetInfo 
VIKINGDR2 
Expected magnitude limit of frameSet in this in H band. 
real 
4 

0.9999995e9 

hexpML 
vikingVarFrameSetInfo 
VIKINGv20110714 
Expected magnitude limit of frameSet in this in H band. 
real 
4 

0.9999995e9 

hexpML 
vikingVarFrameSetInfo 
VIKINGv20111019 
Expected magnitude limit of frameSet in this in H band. 
real 
4 

0.9999995e9 

hexpML 
vvvVarFrameSetInfo 
VVVv20100531 
Expected magnitude limit of frameSet in this in H band. 
real 
4 

0.9999995e9 

hExpRms 
videoVariability 
VIDEODR2 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in H 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. 
hExpRms 
videoVariability 
VIDEODR3 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in H 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. 
hExpRms 
videoVariability 
VIDEODR4 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in H band 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hExpRms 
videoVariability 
VIDEOv20100513 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in H 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. 
hExpRms 
videoVariability 
VIDEOv20111208 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in H 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. 
hExpRms 
vikingVariability 
VIKINGDR2 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in H 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. 
hExpRms 
vikingVariability 
VIKINGv20110714 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in H 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. 
hExpRms 
vikingVariability 
VIKINGv20111019 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in H 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. 
hExpRms 
vvvVariability 
VVVv20100531 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in H 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. 
hGausig 
svNgc253Source 
SVNGC253v20100429 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
svOrionSource 
SVORIONv20100429 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
ultravistaSource, ultravistaSourceRemeasurement 
ULTRAVISTAv20100429 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
vhsSource 
VHSDR2 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
vhsSource 
VHSDR3 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.IR.H 
hGausig 
vhsSource 
VHSv20120926 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
vhsSource 
VHSv20130417 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
vhsSource 
VHSv20140409 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.IR.H 
hGausig 
vhsSource 
VHSv20150108 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.IR.H 
hGausig 
vhsSource, vhsSourceRemeasurement 
VHSDR1 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
videoSource 
VIDEODR2 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
videoSource 
VIDEODR3 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
videoSource 
VIDEODR4 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.IR.H 
hGausig 
videoSource 
VIDEOv20111208 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
videoSource, videoSourceRemeasurement 
VIDEOv20100513 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
vikingSource 
VIKINGDR2 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
vikingSource 
VIKINGDR3 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
vikingSource 
VIKINGDR4 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.IR.H 
hGausig 
vikingSource 
VIKINGv20111019 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
vikingSource 
VIKINGv20130417 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
vikingSource 
VIKINGv20140402 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
vikingSource 
VIKINGv20150421 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.IR.H 
hGausig 
vikingSource, vikingSourceRemeasurement 
VIKINGv20110714 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
vvvSource 
VVVDR2 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
vvvSource 
VVVv20110718 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
vvvSource, vvvSourceRemeasurement 
VVVv20100531 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
vvvSource, vvvSynopticSource 
VVVDR1 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hgl 
twomass_scn 
2MASS 
Special flag indicating whether or not this scan has a singleframe Hband electronic glitch. 
smallint 
2 


meta.code 
hgl 
twomass_sixx2_scn 
2MASS 
singleframe Hband glitch flag (0:not found1:found) 
smallint 
2 



hHalfRad 
videoSource 
VIDEODR4 
SExtractor halflight radius in H band 
real 
4 
pixels 
0.9999995e9 
phys.angSize;em.IR.H 
hHlCorSMjRadAs 
svNgc253Source 
SVNGC253v20100429 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hHlCorSMjRadAs 
ultravistaSource 
ULTRAVISTAv20100429 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hHlCorSMjRadAs 
vhsSource 
VHSDR1 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hHlCorSMjRadAs 
vhsSource 
VHSDR2 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hHlCorSMjRadAs 
vhsSource 
VHSDR3 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.IR.H 
hHlCorSMjRadAs 
vhsSource 
VHSv20120926 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hHlCorSMjRadAs 
vhsSource 
VHSv20130417 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hHlCorSMjRadAs 
vhsSource 
VHSv20140409 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.IR.H 
hHlCorSMjRadAs 
vhsSource 
VHSv20150108 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.IR.H 
hHlCorSMjRadAs 
videoSource 
VIDEODR2 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hHlCorSMjRadAs 
videoSource 
VIDEODR3 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hHlCorSMjRadAs 
videoSource 
VIDEODR4 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.IR.H 
hHlCorSMjRadAs 
videoSource 
VIDEOv20100513 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hHlCorSMjRadAs 
videoSource 
VIDEOv20111208 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hHlCorSMjRadAs 
vikingSource 
VIKINGDR2 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hHlCorSMjRadAs 
vikingSource 
VIKINGDR3 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hHlCorSMjRadAs 
vikingSource 
VIKINGDR4 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.IR.H 
hHlCorSMjRadAs 
vikingSource 
VIKINGv20110714 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hHlCorSMjRadAs 
vikingSource 
VIKINGv20111019 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hHlCorSMjRadAs 
vikingSource 
VIKINGv20130417 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hHlCorSMjRadAs 
vikingSource 
VIKINGv20140402 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hHlCorSMjRadAs 
vikingSource 
VIKINGv20150421 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.IR.H 
HIGH_BACKGROUND 
xmm3dr4 
XMM 
The flag is set to 1 (= True) if this detection comes from a field which, during manual screening, was considered to have a high background level which notably impacted on source detection. 
bit 
1 



hIntRms 
videoVariability 
VIDEODR2 
Intrinsic rms in Hband 
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. 
hIntRms 
videoVariability 
VIDEODR3 
Intrinsic rms in Hband 
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. 
hIntRms 
videoVariability 
VIDEODR4 
Intrinsic rms in Hband 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hIntRms 
videoVariability 
VIDEOv20100513 
Intrinsic rms in Hband 
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. 
hIntRms 
videoVariability 
VIDEOv20111208 
Intrinsic rms in Hband 
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. 
hIntRms 
vikingVariability 
VIKINGDR2 
Intrinsic rms in Hband 
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. 
hIntRms 
vikingVariability 
VIKINGv20110714 
Intrinsic rms in Hband 
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. 
hIntRms 
vikingVariability 
VIKINGv20111019 
Intrinsic rms in Hband 
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. 
hIntRms 
vvvVariability 
VVVv20100531 
Intrinsic rms in Hband 
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. 
hisDefAst 
videoVarFrameSetInfo 
VIDEODR2 
Use a default model for the astrometric noise in H band. 
tinyint 
1 

0 

hisDefAst 
videoVarFrameSetInfo 
VIDEODR3 
Use a default model for the astrometric noise in H band. 
tinyint 
1 

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

0 
meta.code;em.IR.H 
hisDefAst 
videoVarFrameSetInfo 
VIDEOv20111208 
Use a default model for the astrometric noise in H band. 
tinyint 
1 

0 

hisDefAst 
vikingVarFrameSetInfo 
VIKINGDR2 
Use a default model for the astrometric noise in H band. 
tinyint 
1 

0 

hisDefAst 
vikingVarFrameSetInfo 
VIKINGv20111019 
Use a default model for the astrometric noise in H band. 
tinyint 
1 

0 

hisDefPht 
videoVarFrameSetInfo 
VIDEODR2 
Use a default model for the photometric noise in H band. 
tinyint 
1 

0 

hisDefPht 
videoVarFrameSetInfo 
VIDEODR3 
Use a default model for the photometric noise in H band. 
tinyint 
1 

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

0 
meta.code;em.IR.H 
hisDefPht 
videoVarFrameSetInfo 
VIDEOv20111208 
Use a default model for the photometric noise in H band. 
tinyint 
1 

0 

hisDefPht 
vikingVarFrameSetInfo 
VIKINGDR2 
Use a default model for the photometric noise in H band. 
tinyint 
1 

0 

hisDefPht 
vikingVarFrameSetInfo 
VIKINGv20111019 
Use a default model for the photometric noise in H band. 
tinyint 
1 

0 

hKronMag 
videoSource 
VIDEODR4 
Extended source H mag (Kron  SExtractor MAG_AUTO) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hKronMagErr 
videoSource 
VIDEODR4 
Extended source H mag error (Kron  SExtractor MAG_AUTO) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;phot.mag 
hlCircRadAs 
svNgc253Detection 
SVNGC253v20100429 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
svOrionDetection 
SVORIONv20100429 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
ultravistaDetection 
ULTRAVISTAv20100429 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vhsDetection 
VHSDR1 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vhsDetection 
VHSDR2 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vhsDetection 
VHSDR3 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vhsDetection 
VHSv20120926 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vhsDetection 
VHSv20130417 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vhsDetection 
VHSv20140409 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vhsDetection 
VHSv20150108 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
videoDetection 
VIDEODR2 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
videoDetection 
VIDEODR3 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
videoDetection 
VIDEODR4 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
videoDetection 
VIDEOv20100513 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
videoDetection 
VIDEOv20111208 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vikingDetection 
VIKINGDR2 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vikingDetection 
VIKINGDR3 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vikingDetection 
VIKINGDR4 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vikingDetection 
VIKINGv20110714 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vikingDetection 
VIKINGv20111019 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vikingDetection 
VIKINGv20130417 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vikingDetection 
VIKINGv20140402 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vikingDetection 
VIKINGv20150421 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
svNgc253Detection 
SVNGC253v20100429 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
svOrionDetection 
SVORIONv20100429 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
ultravistaDetection 
ULTRAVISTAv20100429 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vhsDetection 
VHSDR1 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vhsDetection 
VHSDR2 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vhsDetection 
VHSDR3 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vhsDetection 
VHSv20120926 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vhsDetection 
VHSv20130417 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vhsDetection 
VHSv20140409 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vhsDetection 
VHSv20150108 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
videoDetection 
VIDEODR2 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
videoDetection 
VIDEODR3 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
videoDetection 
VIDEODR4 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
videoDetection 
VIDEOv20100513 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
videoDetection 
VIDEOv20111208 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vikingDetection 
VIKINGDR2 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vikingDetection 
VIKINGDR3 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vikingDetection 
VIKINGDR4 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vikingDetection 
VIKINGv20110714 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vikingDetection 
VIKINGv20111019 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vikingDetection 
VIKINGv20130417 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vikingDetection 
VIKINGv20140402 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vikingDetection 
VIKINGv20150421 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMjRadAs 
svNgc253Detection 
SVNGC253v20100429 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCorSMjRadAs 
svOrionDetection 
SVORIONv20100429 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCorSMjRadAs 
ultravistaDetection 
ULTRAVISTAv20100429 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCorSMjRadAs 
vhsDetection 
VHSDR1 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCorSMjRadAs 
vhsDetection 
VHSDR2 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCorSMjRadAs 
vhsDetection 
VHSDR3 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
vhsDetection 
VHSv20120926 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
vhsDetection 
VHSv20130417 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
vhsDetection 
VHSv20140409 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
vhsDetection 
VHSv20150108 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
videoDetection 
VIDEODR2 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCorSMjRadAs 
videoDetection 
VIDEODR3 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
videoDetection 
VIDEODR4 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
videoDetection 
VIDEOv20100513 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCorSMjRadAs 
videoDetection 
VIDEOv20111208 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCorSMjRadAs 
vikingDetection 
VIKINGDR2 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCorSMjRadAs 
vikingDetection 
VIKINGDR3 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
vikingDetection 
VIKINGDR4 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
vikingDetection 
VIKINGv20110714 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCorSMjRadAs 
vikingDetection 
VIKINGv20111019 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCorSMjRadAs 
vikingDetection 
VIKINGv20130417 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
vikingDetection 
VIKINGv20140402 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
vikingDetection 
VIKINGv20150421 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMnRadAs 
svNgc253Detection 
SVNGC253v20100429 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
svOrionDetection 
SVORIONv20100429 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
ultravistaDetection 
ULTRAVISTAv20100429 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vhsDetection 
VHSDR1 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vhsDetection 
VHSDR2 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vhsDetection 
VHSDR3 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vhsDetection 
VHSv20120926 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vhsDetection 
VHSv20130417 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vhsDetection 
VHSv20140409 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vhsDetection 
VHSv20150108 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
videoDetection 
VIDEODR2 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
videoDetection 
VIDEODR3 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
videoDetection 
VIDEODR4 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
videoDetection 
VIDEOv20100513 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
videoDetection 
VIDEOv20111208 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vikingDetection 
VIKINGDR2 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vikingDetection 
VIKINGDR3 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vikingDetection 
VIKINGDR4 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vikingDetection 
VIKINGv20110714 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vikingDetection 
VIKINGv20111019 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vikingDetection 
VIKINGv20130417 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vikingDetection 
VIKINGv20140402 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vikingDetection 
VIKINGv20150421 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
svNgc253Detection 
SVNGC253v20100429 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
svOrionDetection 
SVORIONv20100429 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
ultravistaDetection 
ULTRAVISTAv20100429 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
vhsDetection 
VHSDR1 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
vhsDetection 
VHSDR2 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
vhsDetection 
VHSDR3 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
vhsDetection 
VHSv20120926 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
vhsDetection 
VHSv20130417 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
vhsDetection 
VHSv20140409 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
vhsDetection 
VHSv20150108 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
videoDetection 
VIDEODR2 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
videoDetection 
VIDEODR3 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
videoDetection 
VIDEODR4 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
videoDetection 
VIDEOv20100513 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
videoDetection 
VIDEOv20111208 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
vikingDetection 
VIKINGDR2 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
vikingDetection 
VIKINGDR3 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
vikingDetection 
VIKINGDR4 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
vikingDetection 
VIKINGv20110714 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
vikingDetection 
VIKINGv20111019 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
vikingDetection 
VIKINGv20130417 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
vikingDetection 
VIKINGv20140402 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
vikingDetection 
VIKINGv20150421 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
HLRADIUS 
mgcBrightSpec 
MGC 
Semimajor axis of halflight ellipse 
real 
4 
pixel 


hlSMjRadAs 
svNgc253Detection 
SVNGC253v20100429 
Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMjRadAs 
svOrionDetection 
SVORIONv20100429 
Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMjRadAs 
ultravistaDetection 
ULTRAVISTAv20100429 
Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMjRadAs 
vhsDetection 
VHSDR1 
Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMjRadAs 
vhsDetection 
VHSDR2 
Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMjRadAs 
vhsDetection 
VHSDR3 
Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMjRadAs 
vhsDetection 
VHSv20120926 
Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMjRadAs 
vhsDetection 
VHSv20130417 
Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMjRadAs 
vhsDetection 
VHSv20140409 
Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMjRadAs 
vhsDetection 
VHSv20150108 
Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMjRadAs 
videoDetection 
VIDEODR2 
Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMjRadAs 
videoDetection 
VIDEODR3 
Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMjRadAs 
videoDetection 
VIDEODR4 
Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMjRadAs 
videoDetection 
VIDEOv20100513 
Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMjRadAs 
videoDetection 
VIDEOv20111208 
Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMjRadAs 
vikingDetection 
VIKINGDR2 
Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMjRadAs 
vikingDetection 
VIKINGDR3 
Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMjRadAs 
vikingDetection 
VIKINGDR4 
Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMjRadAs 
vikingDetection 
VIKINGv20110714 
Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMjRadAs 
vikingDetection 
VIKINGv20111019 
Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMjRadAs 
vikingDetection 
VIKINGv20130417 
Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMjRadAs 
vikingDetection 
VIKINGv20140402 
Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMjRadAs 
vikingDetection 
VIKINGv20150421 
Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMnRadAs 
svNgc253Detection 
SVNGC253v20100429 
Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMnRadAs 
svOrionDetection 
SVORIONv20100429 
Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMnRadAs 
ultravistaDetection 
ULTRAVISTAv20100429 
Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMnRadAs 
vhsDetection 
VHSDR1 
Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMnRadAs 
vhsDetection 
VHSDR2 
Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMnRadAs 
vhsDetection 
VHSDR3 
Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMnRadAs 
vhsDetection 
VHSv20120926 
Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMnRadAs 
vhsDetection 
VHSv20130417 
Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMnRadAs 
vhsDetection 
VHSv20140409 
Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMnRadAs 
vhsDetection 
VHSv20150108 
Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMnRadAs 
videoDetection 
VIDEODR2 
Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMnRadAs 
videoDetection 
VIDEODR3 
Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMnRadAs 
videoDetection 
VIDEODR4 
Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMnRadAs 
videoDetection 
VIDEOv20100513 
Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMnRadAs 
videoDetection 
VIDEOv20111208 
Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMnRadAs 
vikingDetection 
VIKINGDR2 
Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMnRadAs 
vikingDetection 
VIKINGDR3 
Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMnRadAs 
vikingDetection 
VIKINGDR4 
Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMnRadAs 
vikingDetection 
VIKINGv20110714 
Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMnRadAs 
vikingDetection 
VIKINGv20111019 
Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMnRadAs 
vikingDetection 
VIKINGv20130417 
Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMnRadAs 
vikingDetection 
VIKINGv20140402 
Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMnRadAs 
vikingDetection 
VIKINGv20150421 
Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
Hmag 
mcps_lmcSource, mcps_smcSource 
MCPS 
The H band magnitude (from 2MASS) (0.00 if star not detected.) 
real 
4 
mag 


hMag 
ukirtFSstars 
SVNGC253v20100429 
H band total magnitude on the MKO(UFTI) system 
real 
4 
mag 

phot.mag 
hMag 
ukirtFSstars 
SVORIONv20100429 
H band total magnitude on the MKO(UFTI) system 
real 
4 
mag 

phot.mag 
hMag 
ukirtFSstars 
ULTRAVISTAv20100429 
H band total magnitude on the MKO(UFTI) system 
real 
4 
mag 

phot.mag 
hMag 
ukirtFSstars 
VIDEOv20100513 
H band total magnitude on the MKO(UFTI) system 
real 
4 
mag 

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

phot.mag 
hMag 
ukirtFSstars 
VVVv20100531 
H band total magnitude on the MKO(UFTI) system 
real 
4 
mag 

phot.mag 
hMag 
ultravistaSourceRemeasurement 
ULTRAVISTAv20100429 
H mag (as appropriate for this merged source) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hMag 
vhsSourceRemeasurement 
VHSDR1 
H mag (as appropriate for this merged source) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hMag 
videoSourceRemeasurement 
VIDEOv20100513 
H mag (as appropriate for this merged source) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hMag 
vikingSourceRemeasurement 
VIKINGv20110714 
H mag (as appropriate for this merged source) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hMag 
vikingSourceRemeasurement 
VIKINGv20111019 
H mag (as appropriate for this merged source) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hMag 
vvvSourceRemeasurement 
VVVv20100531 
H mag (as appropriate for this merged source) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hMag 
vvvSourceRemeasurement 
VVVv20110718 
H mag (as appropriate for this merged source) 
real 
4 
mag 
0.9999995e9 
phot.mag 
Hmag2MASS 
spitzer_smcSource 
SPITZER 
The 2MASS H band magnitude. 
real 
4 
mag 


hMagErr 
ukirtFSstars 
SVNGC253v20100429 
H band magnitude error 
real 
4 
mag 

stat.error 
hMagErr 
ukirtFSstars 
SVORIONv20100429 
H band magnitude error 
real 
4 
mag 

stat.error 
hMagErr 
ukirtFSstars 
ULTRAVISTAv20100429 
H band magnitude error 
real 
4 
mag 

stat.error 
hMagErr 
ukirtFSstars 
VIDEOv20100513 
H band magnitude error 
real 
4 
mag 

stat.error 
hMagErr 
ukirtFSstars 
VIKINGv20110714 
H band magnitude error 
real 
4 
mag 

stat.error 
hMagErr 
ukirtFSstars 
VVVv20100531 
H band magnitude error 
real 
4 
mag 

stat.error 
hMagErr 
ultravistaSourceRemeasurement 
ULTRAVISTAv20100429 
Error in H mag 
real 
4 
mag 
0.9999995e9 
stat.error 
hMagErr 
vhsSourceRemeasurement 
VHSDR1 
Error in H mag 
real 
4 
mag 
0.9999995e9 
stat.error 
hMagErr 
videoSourceRemeasurement 
VIDEOv20100513 
Error in H mag 
real 
4 
mag 
0.9999995e9 
stat.error 
hMagErr 
vikingSourceRemeasurement 
VIKINGv20110714 
Error in H mag 
real 
4 
mag 
0.9999995e9 
stat.error 
hMagErr 
vikingSourceRemeasurement 
VIKINGv20111019 
Error in H mag 
real 
4 
mag 
0.9999995e9 
stat.error 
hMagErr 
vvvSourceRemeasurement 
VVVv20100531 
Error in H mag 
real 
4 
mag 
0.9999995e9 
stat.error 
hMagErr 
vvvSourceRemeasurement 
VVVv20110718 
Error in H mag 
real 
4 
mag 
0.9999995e9 
stat.error 
hMagMAD 
videoVariability 
VIDEODR2 
Median Absolute Deviation of H magnitude 
real 
4 
mag 
0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hMagMAD 
videoVariability 
VIDEODR3 
Median Absolute Deviation of H magnitude 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.NIR 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hMagMAD 
videoVariability 
VIDEODR4 
Median Absolute Deviation of H magnitude 
real 
4 
mag 
0.9999995e9 
stat.err;em.IR.H;phot.mag 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hMagMAD 
videoVariability 
VIDEOv20100513 
Median Absolute Deviation of H magnitude 
real 
4 
mag 
0.9999995e9 

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

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hMagMAD 
vikingVariability 
VIKINGDR2 
Median Absolute Deviation of H magnitude 
real 
4 
mag 
0.9999995e9 

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

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hMagMAD 
vikingVariability 
VIKINGv20111019 
Median Absolute Deviation of H magnitude 
real 
4 
mag 
0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hMagMAD 
vvvVariability 
VVVv20100531 
Median Absolute Deviation of H magnitude 
real 
4 
mag 
0.9999995e9 

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

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hMagRms 
videoVariability 
VIDEODR3 
rms of H magnitude 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.NIR 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hMagRms 
videoVariability 
VIDEODR4 
rms of H magnitude 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;phot.mag 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hMagRms 
videoVariability 
VIDEOv20100513 
rms of H magnitude 
real 
4 
mag 
0.9999995e9 

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

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hMagRms 
vikingVariability 
VIKINGDR2 
rms of H magnitude 
real 
4 
mag 
0.9999995e9 

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

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hMagRms 
vikingVariability 
VIKINGv20111019 
rms of H magnitude 
real 
4 
mag 
0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hMagRms 
vvvVariability 
VVVv20100531 
rms of H magnitude 
real 
4 
mag 
0.9999995e9 

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

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
hmaxCadence 
videoVariability 
VIDEODR3 
maximum gap between observations 
real 
4 
days 
0.9999995e9 
time.interval;obs;stat.max 
The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
hmaxCadence 
videoVariability 
VIDEODR4 
maximum gap between observations 
real 
4 
days 
0.9999995e9 
time.interval;obs;stat.max 
The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
hmaxCadence 
videoVariability 
VIDEOv20100513 
maximum gap between observations 
real 
4 
days 
0.9999995e9 

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

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
hmaxCadence 
vikingVariability 
VIKINGDR2 
maximum gap between observations 
real 
4 
days 
0.9999995e9 

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

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
hmaxCadence 
vikingVariability 
VIKINGv20111019 
maximum gap between observations 
real 
4 
days 
0.9999995e9 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
hmaxCadence 
vvvVariability 
VVVv20100531 
maximum gap between observations 
real 
4 
days 
0.9999995e9 

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

0.9999995e9 

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

0.9999995e9 
phot.mag;stat.max;em.IR.NIR 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hMaxMag 
videoVariability 
VIDEODR4 
Maximum magnitude in H band, of good detections 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H;stat.max 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hMaxMag 
videoVariability 
VIDEOv20100513 
Maximum magnitude in H band, of good detections 
real 
4 

0.9999995e9 

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

0.9999995e9 

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

0.9999995e9 

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

0.9999995e9 

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

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hMaxMag 
vvvVariability 
VVVv20100531 
Maximum magnitude in H band, of good detections 
real 
4 

0.9999995e9 

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

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hmeanMag 
videoVariability 
VIDEODR3 
Mean H magnitude 
real 
4 
mag 
0.9999995e9 
phot.mag;stat.mean;em.IR.NIR 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hmeanMag 
videoVariability 
VIDEODR4 
Mean H magnitude 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H;stat.mean;em.IR.H 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hmeanMag 
videoVariability 
VIDEOv20100513 
Mean H magnitude 
real 
4 
mag 
0.9999995e9 

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

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hmeanMag 
vikingVariability 
VIKINGDR2 
Mean H magnitude 
real 
4 
mag 
0.9999995e9 

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

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hmeanMag 
vikingVariability 
VIKINGv20111019 
Mean H magnitude 
real 
4 
mag 
0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hmeanMag 
vvvVariability 
VVVv20100531 
Mean H magnitude 
real 
4 
mag 
0.9999995e9 

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

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
hmedCadence 
videoVariability 
VIDEODR3 
median gap between observations 
real 
4 
days 
0.9999995e9 
time.interval;obs;stat.median 
The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
hmedCadence 
videoVariability 
VIDEODR4 
median gap between observations 
real 
4 
days 
0.9999995e9 
time.interval;obs;stat.median 
The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
hmedCadence 
videoVariability 
VIDEOv20100513 
median gap between observations 
real 
4 
days 
0.9999995e9 

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

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
hmedCadence 
vikingVariability 
VIKINGDR2 
median gap between observations 
real 
4 
days 
0.9999995e9 

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

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
hmedCadence 
vikingVariability 
VIKINGv20111019 
median gap between observations 
real 
4 
days 
0.9999995e9 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
hmedCadence 
vvvVariability 
VVVv20100531 
median gap between observations 
real 
4 
days 
0.9999995e9 

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

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hmedianMag 
videoVariability 
VIDEODR3 
Median H magnitude 
real 
4 
mag 
0.9999995e9 
phot.mag;stat.median;em.IR.NIR 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hmedianMag 
videoVariability 
VIDEODR4 
Median H magnitude 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H;stat.median;em.IR.H 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hmedianMag 
videoVariability 
VIDEOv20100513 
Median H magnitude 
real 
4 
mag 
0.9999995e9 

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

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hmedianMag 
vikingVariability 
VIKINGDR2 
Median H magnitude 
real 
4 
mag 
0.9999995e9 

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

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hmedianMag 
vikingVariability 
VIKINGv20111019 
Median H magnitude 
real 
4 
mag 
0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hmedianMag 
vvvVariability 
VVVv20100531 
Median H magnitude 
real 
4 
mag 
0.9999995e9 

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


obs.field 
hmfID 
svOrionMergeLog 
SVORIONv20100429 
the UID of the relevant H multiframe 
bigint 
8 


obs.field 
hmfID 
ultravistaMergeLog 
ULTRAVISTAv20100429 
the UID of the relevant H multiframe 
bigint 
8 


obs.field 
hmfID 
vhsMergeLog 
VHSDR1 
the UID of the relevant H multiframe 
bigint 
8 


obs.field 
hmfID 
vhsMergeLog 
VHSDR2 
the UID of the relevant H multiframe 
bigint 
8 


obs.field 
hmfID 
vhsMergeLog 
VHSDR3 
the UID of the relevant H multiframe 
bigint 
8 


meta.id;obs.field;em.IR.H 
hmfID 
vhsMergeLog 
VHSv20120926 
the UID of the relevant H multiframe 
bigint 
8 


meta.id;obs.field 
hmfID 
vhsMergeLog 
VHSv20130417 
the UID of the relevant H multiframe 
bigint 
8 


meta.id;obs.field 
hmfID 
vhsMergeLog 
VHSv20140409 
the UID of the relevant H multiframe 
bigint 
8 


meta.id;obs.field;em.IR.H 
hmfID 
vhsMergeLog 
VHSv20150108 
the UID of the relevant H multiframe 
bigint 
8 


meta.id;obs.field;em.IR.H 
hmfID 
videoMergeLog 
VIDEODR2 
the UID of the relevant H multiframe 
bigint 
8 


obs.field 
hmfID 
videoMergeLog 
VIDEODR3 
the UID of the relevant H multiframe 
bigint 
8 


meta.id;obs.field 
hmfID 
videoMergeLog 
VIDEODR4 
the UID of the relevant H multiframe 
bigint 
8 


meta.id;obs.field;em.IR.H 
hmfID 
videoMergeLog 
VIDEOv20100513 
the UID of the relevant H multiframe 
bigint 
8 


obs.field 
hmfID 
videoMergeLog 
VIDEOv20111208 
the UID of the relevant H multiframe 
bigint 
8 


obs.field 
hmfID 
vikingMergeLog 
VIKINGDR2 
the UID of the relevant H multiframe 
bigint 
8 


obs.field 
hmfID 
vikingMergeLog 
VIKINGDR3 
the UID of the relevant H multiframe 
bigint 
8 


meta.id;obs.field 
hmfID 
vikingMergeLog 
VIKINGDR4 
the UID of the relevant H multiframe 
bigint 
8 


meta.id;obs.field;em.IR.H 
hmfID 
vikingMergeLog 
VIKINGv20110714 
the UID of the relevant H multiframe 
bigint 
8 


obs.field 
hmfID 
vikingMergeLog 
VIKINGv20111019 
the UID of the relevant H multiframe 
bigint 
8 


obs.field 
hmfID 
vikingMergeLog 
VIKINGv20130417 
the UID of the relevant H multiframe 
bigint 
8 


meta.id;obs.field 
hmfID 
vikingMergeLog 
VIKINGv20140402 
the UID of the relevant H multiframe 
bigint 
8 


meta.id;obs.field 
hmfID 
vikingMergeLog 
VIKINGv20150421 
the UID of the relevant H multiframe 
bigint 
8 


meta.id;obs.field;em.IR.H 
hmfID 
vvvMergeLog 
VVVDR2 
the UID of the relevant H multiframe 
bigint 
8 


meta.id;obs.field 
hmfID 
vvvMergeLog 
VVVv20100531 
the UID of the relevant H multiframe 
bigint 
8 


obs.field 
hmfID 
vvvMergeLog 
VVVv20110718 
the UID of the relevant H multiframe 
bigint 
8 


obs.field 
hmfID 
vvvMergeLog, vvvSynopticMergeLog 
VVVDR1 
the UID of the relevant H multiframe 
bigint 
8 


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

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
hminCadence 
videoVariability 
VIDEODR3 
minimum gap between observations 
real 
4 
days 
0.9999995e9 
time.interval;obs;stat.min 
The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
hminCadence 
videoVariability 
VIDEODR4 
minimum gap between observations 
real 
4 
days 
0.9999995e9 
time.interval;obs;stat.min 
The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
hminCadence 
videoVariability 
VIDEOv20100513 
minimum gap between observations 
real 
4 
days 
0.9999995e9 

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

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
hminCadence 
vikingVariability 
VIKINGDR2 
minimum gap between observations 
real 
4 
days 
0.9999995e9 

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

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
hminCadence 
vikingVariability 
VIKINGv20111019 
minimum gap between observations 
real 
4 
days 
0.9999995e9 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
hminCadence 
vvvVariability 
VVVv20100531 
minimum gap between observations 
real 
4 
days 
0.9999995e9 

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

0.9999995e9 

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

0.9999995e9 
phot.mag;stat.min;em.IR.NIR 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hMinMag 
videoVariability 
VIDEODR4 
Minimum magnitude in H band, of good detections 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H;stat.min 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hMinMag 
videoVariability 
VIDEOv20100513 
Minimum magnitude in H band, of good detections 
real 
4 

0.9999995e9 

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

0.9999995e9 

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

0.9999995e9 

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

0.9999995e9 

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

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hMinMag 
vvvVariability 
VVVv20100531 
Minimum magnitude in H band, of good detections 
real 
4 

0.9999995e9 

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

PHOT_COLOR 
hmks 
vhsSourceRemeasurement 
VHSDR1 
Default colour HKs (using appropriate mags) 
real 
4 
mag 

PHOT_COLOR 
hmks 
videoSourceRemeasurement 
VIDEOv20100513 
Default colour HKs (using appropriate mags) 
real 
4 
mag 

PHOT_COLOR 
hmks 
vikingSourceRemeasurement 
VIKINGv20110714 
Default colour HKs (using appropriate mags) 
real 
4 
mag 

PHOT_COLOR 
hmks 
vikingSourceRemeasurement 
VIKINGv20111019 
Default colour HKs (using appropriate mags) 
real 
4 
mag 

PHOT_COLOR 
hmks 
vvvSourceRemeasurement 
VVVv20100531 
Default colour HKs (using appropriate mags) 
real 
4 
mag 

PHOT_COLOR 
hmks 
vvvSourceRemeasurement 
VVVv20110718 
Default colour HKs (using appropriate mags) 
real 
4 
mag 

PHOT_COLOR 
hmksErr 
ultravistaSourceRemeasurement 
ULTRAVISTAv20100429 
Error on colour HKs 
real 
4 
mag 

stat.error 
hmksErr 
vhsSourceRemeasurement 
VHSDR1 
Error on colour HKs 
real 
4 
mag 

stat.error 
hmksErr 
videoSourceRemeasurement 
VIDEOv20100513 
Error on colour HKs 
real 
4 
mag 

stat.error 
hmksErr 
vikingSourceRemeasurement 
VIKINGv20110714 
Error on colour HKs 
real 
4 
mag 

stat.error 
hmksErr 
vikingSourceRemeasurement 
VIKINGv20111019 
Error on colour HKs 
real 
4 
mag 

stat.error 
hmksErr 
vvvSourceRemeasurement 
VVVv20100531 
Error on colour HKs 
real 
4 
mag 

stat.error 
hmksErr 
vvvSourceRemeasurement 
VVVv20110718 
Error on colour HKs 
real 
4 
mag 

stat.error 
hmksExt 
svNgc253Source 
SVNGC253v20100429 
Extended source colour HKs (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExt 
svOrionSource 
SVORIONv20100429 
Extended source colour HKs (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExt 
ultravistaSource 
ULTRAVISTAv20100429 
Extended source colour HKs (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExt 
vhsSource 
VHSDR1 
Extended source colour HKs (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExt 
vhsSource 
VHSDR2 
Extended source colour HKs (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExt 
vhsSource 
VHSDR3 
Extended source colour HKs (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.IR.H;em.IR.K 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExt 
vhsSource 
VHSv20120926 
Extended source colour HKs (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExt 
vhsSource 
VHSv20130417 
Extended source colour HKs (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExt 
vhsSource 
VHSv20140409 
Extended source colour HKs (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.IR.H;em.IR.K 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExt 
vhsSource 
VHSv20150108 
Extended source colour HKs (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.IR.H;em.IR.K 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExt 
videoSource 
VIDEODR2 
Extended source colour HKs (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExt 
videoSource 
VIDEODR3 
Extended source colour HKs (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExt 
videoSource 
VIDEODR4 
Extended source colour HKs (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.IR.H;em.IR.K 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExt 
videoSource 
VIDEOv20100513 
Extended source colour HKs (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExt 
videoSource 
VIDEOv20111208 
Extended source colour HKs (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExt 
vikingSource 
VIKINGDR2 
Extended source colour HKs (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExt 
vikingSource 
VIKINGDR3 
Extended source colour HKs (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExt 
vikingSource 
VIKINGDR4 
Extended source colour HKs (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.IR.H;em.IR.K 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExt 
vikingSource 
VIKINGv20110714 
Extended source colour HKs (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExt 
vikingSource 
VIKINGv20111019 
Extended source colour HKs (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExt 
vikingSource 
VIKINGv20130417 
Extended source colour HKs (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExt 
vikingSource 
VIKINGv20140402 
Extended source colour HKs (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.IR.H;em.IR.K 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExt 
vikingSource 
VIKINGv20150421 
Extended source colour HKs (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.IR.H;em.IR.K 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExt 
vvvSource 
VVVv20100531 
Extended source colour HKs (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExtErr 
svNgc253Source 
SVNGC253v20100429 
Error on extended source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExtErr 
svOrionSource 
SVORIONv20100429 
Error on extended source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExtErr 
ultravistaSource 
ULTRAVISTAv20100429 
Error on extended source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExtErr 
vhsSource 
VHSDR1 
Error on extended source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExtErr 
vhsSource 
VHSDR2 
Error on extended source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExtErr 
vhsSource 
VHSDR3 
Error on extended source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;em.IR.K 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExtErr 
vhsSource 
VHSv20120926 
Error on extended source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExtErr 
vhsSource 
VHSv20130417 
Error on extended source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExtErr 
vhsSource 
VHSv20140409 
Error on extended source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;em.IR.K 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExtErr 
vhsSource 
VHSv20150108 
Error on extended source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;em.IR.K 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExtErr 
videoSource 
VIDEODR2 
Error on extended source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExtErr 
videoSource 
VIDEODR3 
Error on extended source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExtErr 
videoSource 
VIDEODR4 
Error on extended source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;em.IR.K 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExtErr 
videoSource 
VIDEOv20100513 
Error on extended source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExtErr 
videoSource 
VIDEOv20111208 
Error on extended source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExtErr 
vikingSource 
VIKINGDR2 
Error on extended source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExtErr 
vikingSource 
VIKINGDR3 
Error on extended source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExtErr 
vikingSource 
VIKINGDR4 
Error on extended source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;em.IR.K 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExtErr 
vikingSource 
VIKINGv20110714 
Error on extended source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExtErr 
vikingSource 
VIKINGv20111019 
Error on extended source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExtErr 
vikingSource 
VIKINGv20130417 
Error on extended source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExtErr 
vikingSource 
VIKINGv20140402 
Error on extended source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExtErr 
vikingSource 
VIKINGv20150421 
Error on extended source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;em.IR.K 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksExtErr 
vvvSource 
VVVv20100531 
Error on extended source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPnt 
svNgc253Source 
SVNGC253v20100429 
Point source colour HKs (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPnt 
svOrionSource 
SVORIONv20100429 
Point source colour HKs (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPnt 
ultravistaSource 
ULTRAVISTAv20100429 
Point source colour HKs (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPnt 
vhsSource 
VHSDR1 
Point source colour HKs (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPnt 
vhsSource 
VHSDR2 
Point source colour HKs (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPnt 
vhsSource 
VHSDR3 
Point source colour HKs (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.IR.H;em.IR.K 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPnt 
vhsSource 
VHSv20120926 
Point source colour HKs (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPnt 
vhsSource 
VHSv20130417 
Point source colour HKs (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPnt 
vhsSource 
VHSv20140409 
Point source colour HKs (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.IR.H;em.IR.K 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPnt 
vhsSource 
VHSv20150108 
Point source colour HKs (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.IR.H;em.IR.K 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPnt 
videoSource 
VIDEODR2 
Point source colour HKs (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPnt 
videoSource 
VIDEODR3 
Point source colour HKs (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPnt 
videoSource 
VIDEODR4 
Point source colour HKs (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.IR.H;em.IR.K 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPnt 
videoSource 
VIDEOv20100513 
Point source colour HKs (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPnt 
videoSource 
VIDEOv20111208 
Point source colour HKs (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPnt 
vikingSource 
VIKINGDR2 
Point source colour HKs (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPnt 
vikingSource 
VIKINGDR3 
Point source colour HKs (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPnt 
vikingSource 
VIKINGDR4 
Point source colour HKs (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.IR.H;em.IR.K 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPnt 
vikingSource 
VIKINGv20110714 
Point source colour HKs (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPnt 
vikingSource 
VIKINGv20111019 
Point source colour HKs (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPnt 
vikingSource 
VIKINGv20130417 
Point source colour HKs (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPnt 
vikingSource 
VIKINGv20140402 
Point source colour HKs (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.IR.H;em.IR.K 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPnt 
vikingSource 
VIKINGv20150421 
Point source colour HKs (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.IR.H;em.IR.K 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPnt 
vvvSource 
VVVDR2 
Point source colour HKs (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.IR.H;em.IR.K 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPnt 
vvvSource 
VVVv20100531 
Point source colour HKs (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPnt 
vvvSource 
VVVv20110718 
Point source colour HKs (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPnt 
vvvSource, vvvSynopticSource 
VVVDR1 
Point source colour HKs (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPntErr 
svNgc253Source 
SVNGC253v20100429 
Error on point source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPntErr 
svOrionSource 
SVORIONv20100429 
Error on point source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPntErr 
ultravistaSource 
ULTRAVISTAv20100429 
Error on point source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPntErr 
vhsSource 
VHSDR1 
Error on point source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPntErr 
vhsSource 
VHSDR2 
Error on point source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPntErr 
vhsSource 
VHSDR3 
Error on point source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;em.IR.K 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPntErr 
vhsSource 
VHSv20120926 
Error on point source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPntErr 
vhsSource 
VHSv20130417 
Error on point source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPntErr 
vhsSource 
VHSv20140409 
Error on point source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;em.IR.K 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPntErr 
vhsSource 
VHSv20150108 
Error on point source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;em.IR.K 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPntErr 
videoSource 
VIDEODR2 
Error on point source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPntErr 
videoSource 
VIDEODR3 
Error on point source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPntErr 
videoSource 
VIDEODR4 
Error on point source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;em.IR.K 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPntErr 
videoSource 
VIDEOv20100513 
Error on point source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPntErr 
videoSource 
VIDEOv20111208 
Error on point source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPntErr 
vikingSource 
VIKINGDR2 
Error on point source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPntErr 
vikingSource 
VIKINGDR3 
Error on point source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPntErr 
vikingSource 
VIKINGDR4 
Error on point source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;em.IR.K 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPntErr 
vikingSource 
VIKINGv20110714 
Error on point source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPntErr 
vikingSource 
VIKINGv20111019 
Error on point source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPntErr 
vikingSource 
VIKINGv20130417 
Error on point source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPntErr 
vikingSource 
VIKINGv20140402 
Error on point source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPntErr 
vikingSource 
VIKINGv20150421 
Error on point source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;em.IR.K 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPntErr 
vvvSource 
VVVDR2 
Error on point source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPntErr 
vvvSource 
VVVv20100531 
Error on point source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPntErr 
vvvSource 
VVVv20110718 
Error on point source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmksPntErr 
vvvSource, vvvSynopticSource 
VVVDR1 
Error on point source colour HKs 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hndof 
videoVariability 
VIDEODR2 
Number of degrees of freedom for chisquare 
smallint 
2 

9999 

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

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

9999 
stat.fit.dof;em.IR.H 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hndof 
videoVariability 
VIDEOv20100513 
Number of degrees of freedom for chisquare 
smallint 
2 

9999 

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

9999 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hndof 
vikingVariability 
VIKINGDR2 
Number of degrees of freedom for chisquare 
smallint 
2 

9999 

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

9999 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hndof 
vikingVariability 
VIKINGv20111019 
Number of degrees of freedom for chisquare 
smallint 
2 

9999 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hndof 
vvvVariability 
VVVv20100531 
Number of degrees of freedom for chisquare 
smallint 
2 

9999 

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

9999 

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

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

9999 
stat.fit.dof;stat.param;em.IR.H 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hnDofAst 
videoVarFrameSetInfo 
VIDEOv20100513 
Number of degrees of freedom of astrometric fit in H band. 
smallint 
2 

9999 

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

9999 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hnDofAst 
vikingVarFrameSetInfo 
VIKINGDR2 
Number of degrees of freedom of astrometric fit in H band. 
smallint 
2 

9999 

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

9999 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hnDofAst 
vikingVarFrameSetInfo 
VIKINGv20111019 
Number of degrees of freedom of astrometric fit in H band. 
smallint 
2 

9999 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hnDofAst 
vvvVarFrameSetInfo 
VVVv20100531 
Number of degrees of freedom of astrometric fit in H band. 
smallint 
2 

9999 

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

9999 

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

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

9999 
stat.fit.dof;stat.param;em.IR.H 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hnDofPht 
videoVarFrameSetInfo 
VIDEOv20100513 
Number of degrees of freedom of photometric fit in H band. 
smallint 
2 

9999 

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

9999 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hnDofPht 
vikingVarFrameSetInfo 
VIKINGDR2 
Number of degrees of freedom of photometric fit in H band. 
smallint 
2 

9999 

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

9999 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hnDofPht 
vikingVarFrameSetInfo 
VIKINGv20111019 
Number of degrees of freedom of photometric fit in H band. 
smallint 
2 

9999 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hnDofPht 
vvvVarFrameSetInfo 
VVVv20100531 
Number of degrees of freedom of photometric fit in H band. 
smallint 
2 

9999 

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

0 

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

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

0 
meta.number;em.IR.H 
The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
hnFlaggedObs 
videoVariability 
VIDEOv20100513 
Number of detections in H band flagged as potentially spurious by videoDetection.ppErrBits 
int 
4 

0 

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

0 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
hnFlaggedObs 
vikingVariability 
VIKINGDR2 
Number of detections in H band flagged as potentially spurious by vikingDetection.ppErrBits 
int 
4 

0 

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

0 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
hnFlaggedObs 
vikingVariability 
VIKINGv20111019 
Number of detections in H band flagged as potentially spurious by vikingDetection.ppErrBits 
int 
4 

0 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
hnFlaggedObs 
vvvVariability 
VVVv20100531 
Number of detections in H band flagged as potentially spurious by vvvDetection.ppErrBits 
int 
4 

0 

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

0 

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

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

0 
meta.number;em.IR.H 
The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
hnGoodObs 
videoVariability 
VIDEOv20100513 
Number of good detections in H band 
int 
4 

0 

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

0 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
hnGoodObs 
vikingVariability 
VIKINGDR2 
Number of good detections in H band 
int 
4 

0 

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

0 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
hnGoodObs 
vikingVariability 
VIKINGv20111019 
Number of good detections in H band 
int 
4 

0 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
hnGoodObs 
vvvVariability 
VVVv20100531 
Number of good detections in H band 
int 
4 

0 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
hNgt3sig 
videoVariability 
VIDEODR2 
Number of good detections in Hband that are more than 3 sigma deviations 
smallint 
2 

9999 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hNgt3sig 
videoVariability 
VIDEODR3 
Number of good detections in Hband that are more than 3 sigma deviations 
smallint 
2 

9999 
meta.number;em.IR.NIR 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hNgt3sig 
videoVariability 
VIDEODR4 
Number of good detections in Hband that are more than 3 sigma deviations 
smallint 
2 

9999 
meta.number;em.IR.H 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hNgt3sig 
videoVariability 
VIDEOv20100513 
Number of good detections in Hband that are more than 3 sigma deviations 
smallint 
2 

9999 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hNgt3sig 
videoVariability 
VIDEOv20111208 
Number of good detections in Hband that are more than 3 sigma deviations 
smallint 
2 

9999 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hNgt3sig 
vikingVariability 
VIKINGDR2 
Number of good detections in Hband that are more than 3 sigma deviations 
smallint 
2 

9999 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hNgt3sig 
vikingVariability 
VIKINGv20110714 
Number of good detections in Hband that are more than 3 sigma deviations 
smallint 
2 

9999 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hNgt3sig 
vikingVariability 
VIKINGv20111019 
Number of good detections in Hband that are more than 3 sigma deviations 
smallint 
2 

9999 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hNgt3sig 
vvvVariability 
VVVv20100531 
Number of good detections in Hband that are more than 3 sigma deviations 
smallint 
2 

9999 

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

0 

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

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

0 
meta.number;em.IR.H 
The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
hnMissingObs 
videoVariability 
VIDEOv20100513 
Number of H band frames that this object should have been detected on and was not 
int 
4 

0 

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

0 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
hnMissingObs 
vikingVariability 
VIKINGDR2 
Number of H band frames that this object should have been detected on and was not 
int 
4 

0 

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

0 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
hnMissingObs 
vikingVariability 
VIKINGv20111019 
Number of H band frames that this object should have been detected on and was not 
int 
4 

0 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
hnMissingObs 
vvvVariability 
VVVv20100531 
Number of H band frames that this object should have been detected on and was not 
int 
4 

0 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
hPA 
svNgc253Source 
SVNGC253v20100429 
ellipse fit celestial orientation in H 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
hPA 
svOrionSource 
SVORIONv20100429 
ellipse fit celestial orientation in H 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
hPA 
ultravistaSource, ultravistaSourceRemeasurement 
ULTRAVISTAv20100429 
ellipse fit celestial orientation in H 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
hPA 
vhsSource 
VHSDR2 
ellipse fit celestial orientation in H 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
hPA 
vhsSource 
VHSDR3 
ellipse fit celestial orientation in H 
real 
4 
Degrees 
0.9999995e9 
pos.posAng;em.IR.H 
hPA 
vhsSource 
VHSv20120926 
ellipse fit celestial orientation in H 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
hPA 
vhsSource 
VHSv20130417 
ellipse fit celestial orientation in H 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
hPA 
vhsSource 
VHSv20140409 
ellipse fit celestial orientation in H 
real 
4 
Degrees 
0.9999995e9 
pos.posAng;em.IR.H 
hPA 
vhsSource 
VHSv20150108 
ellipse fit celestial orientation in H 
real 
4 
Degrees 
0.9999995e9 
pos.posAng;em.IR.H 
hPA 
vhsSource, vhsSourceRemeasurement 
VHSDR1 
ellipse fit celestial orientation in H 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
hPA 
videoSource 
VIDEODR2 
ellipse fit celestial orientation in H 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
hPA 
videoSource 
VIDEODR3 
ellipse fit celestial orientation in H 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
hPA 
videoSource 
VIDEODR4 
ellipse fit celestial orientation in H 
real 
4 
Degrees 
0.9999995e9 
pos.posAng;em.IR.H 
hPA 
videoSource 
VIDEOv20111208 
ellipse fit celestial orientation in H 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
hPA 
videoSource, videoSourceRemeasurement 
VIDEOv20100513 
ellipse fit celestial orientation in H 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
hPA 
vikingSource 
VIKINGDR2 
ellipse fit celestial orientation in H 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
hPA 
vikingSource 
VIKINGDR3 
ellipse fit celestial orientation in H 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
hPA 
vikingSource 
VIKINGDR4 
ellipse fit celestial orientation in H 
real 
4 
Degrees 
0.9999995e9 
pos.posAng;em.IR.H 
hPA 
vikingSource 
VIKINGv20111019 
ellipse fit celestial orientation in H 
real 
4 
Degrees 
0.9999995e9 