H 
Name  Schema Table  Database  Description  Type  Length  Unit  Default Value  Unified Content Descriptor 
h_2mrat 
twomass_scn 
TWOMASS 
Hband average 2nd image moment ratio. 
real 
4 


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



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


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

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

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


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


meta.code 
h_bisym_chi 
twomass_xsc 
TWOMASS 
H bisymmetric crosscorrelation chi. 
real 
4 


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


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

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

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


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


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


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


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


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


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


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


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


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


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


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



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


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


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


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


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


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


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


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


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


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


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


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


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


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



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


meta.code 
h_k 
twomass_sixx2_psc 
TWOMASS 
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 
TWOMASS 
Default Hband magnitude 
real 
4 
mag 

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


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

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

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

phot.flux 
h_m_25 
twomass_xsc 
TWOMASS 
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 
TWOMASS 
H 30 arcsec radius circular aperture magnitude. 
real 
4 
mag 

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

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

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

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

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


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

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

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

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

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


h_m_ext 
twomass_xsc 
TWOMASS 
H mag from fit extrapolation. 
real 
4 
mag 

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

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

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

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

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

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

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

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

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

phot.flux 
h_m_k20fe 
twomass_sixx2_xsc 
TWOMASS 
H 20mag/sq.″ isophotal fiducial ell. ap. magnitude 
real 
4 
mag 


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

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

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

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

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


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

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

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

stat.error 
h_msig_25 
twomass_xsc 
TWOMASS 
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 
TWOMASS 
H 1sigma uncertainty in 30 arcsec circular ap. mag. 
real 
4 
mag 

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

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

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

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

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


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

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

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

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

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


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

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

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

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

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

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

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

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

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

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

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


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

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

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

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


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

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


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


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



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


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

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


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

pos.posAng 
h_psfchi 
twomass_psc 
TWOMASS 
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 
TWOMASS 
Hband photometric sensitivity paramater (PSP). 
real 
4 


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



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


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


h_r_c 
twomass_xsc 
TWOMASS 
H Kron circular aperture radius. 
real 
4 
arcsec 

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

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

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

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

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

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

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

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


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


meta.code 
h_sc_msh 
twomass_xsc 
TWOMASS 
H median shape score. 
real 
4 


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


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


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


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


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


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


meta.code 
h_seetrack 
twomass_xsc 
TWOMASS 
H band seetracking score. 
real 
4 


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


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


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



h_shape_rms 
twomass_scn 
TWOMASS 
RMSerror of Hband average seeing shape. 
real 
4 


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



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


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

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



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


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

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


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

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


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

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


halfFlux 
atlasDetection 
ATLASDR1 
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 
atlasDetection 
ATLASDR3 
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 
atlasDetection 
ATLASDR4 
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 
atlasDetection 
ATLASDR5 
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 
atlasDetection 
ATLASv20131127 
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 
atlasDetection 
ATLASv20160425 
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 
atlasDetection 
ATLASv20180209 
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 
atlasDetection, atlasDetectionUncorr 
ATLASDR2 
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 
vphasDetection 
VPHASv20160112 
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 
vphasDetection 
VPHASv20170222 
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 
vphasDetection, vphasDetectionUncorr 
VPHASDR3 
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 
atlasDetection 
ATLASDR1 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
atlasDetection 
ATLASDR3 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
atlasDetection 
ATLASDR4 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
atlasDetection 
ATLASDR5 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
atlasDetection 
ATLASv20131127 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
atlasDetection 
ATLASv20160425 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
atlasDetection 
ATLASv20180209 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
atlasDetection, atlasDetectionUncorr 
ATLASDR2 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vphasDetection 
VPHASv20160112 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vphasDetection 
VPHASv20170222 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vphasDetection, vphasDetectionUncorr 
VPHASDR3 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfMag 
atlasDetection 
ATLASDR1 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
atlasDetection 
ATLASDR3 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
atlasDetection 
ATLASDR4 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
atlasDetection 
ATLASDR5 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
atlasDetection 
ATLASv20131127 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
atlasDetection 
ATLASv20160425 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
atlasDetection 
ATLASv20180209 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
atlasDetection, atlasDetectionUncorr 
ATLASDR2 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vphasDetection 
VPHASv20160112 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vphasDetection 
VPHASv20170222 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vphasDetection, vphasDetectionUncorr 
VPHASDR3 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMagErr 
atlasDetection 
ATLASDR1 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
atlasDetection 
ATLASDR3 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
atlasDetection 
ATLASDR4 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
atlasDetection 
ATLASDR5 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
atlasDetection 
ATLASv20131127 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
atlasDetection 
ATLASv20160425 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
atlasDetection 
ATLASv20180209 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
atlasDetection, atlasDetectionUncorr 
ATLASDR2 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vphasDetection 
VPHASv20160112 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vphasDetection 
VPHASv20170222 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vphasDetection, vphasDetectionUncorr 
VPHASDR3 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfRad 
atlasDetection 
ATLASDR1 
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 
atlasDetection 
ATLASDR3 
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 
atlasDetection 
ATLASDR4 
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 
atlasDetection 
ATLASDR5 
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 
atlasDetection 
ATLASv20131127 
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 
atlasDetection 
ATLASv20160425 
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 
atlasDetection 
ATLASv20180209 
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 
atlasDetection, atlasDetectionUncorr 
ATLASDR2 
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 
vphasDetection 
VPHASv20160112 
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 
vphasDetection 
VPHASv20170222 
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 
vphasDetection, vphasDetectionUncorr 
VPHASDR3 
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 
havphasAperMag3 
vphasSource 
VPHASDR3 
Default point source Havphas aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.line.Halpha 
havphasAperMag3 
vphasSource 
VPHASv20160112 
Default point source Havphas aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.R;em.line.Halpha 
havphasAperMag3 
vphasSource 
VPHASv20170222 
Default point source Havphas aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.R;em.line.Halpha 
havphasAperMag3Err 
vphasSource 
VPHASDR3 
Error in default point/extended source Havphas mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.line.Halpha 
havphasAperMag3Err 
vphasSource 
VPHASv20160112 
Error in default point/extended source Havphas mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.opt.R;em.line.Halpha 
havphasAperMag3Err 
vphasSource 
VPHASv20170222 
Error in default point/extended source Havphas mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.opt.R;em.line.Halpha 
havphasAperMag4 
vphasSource 
VPHASDR3 
Point source Havphas aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.line.Halpha 
havphasAperMag4 
vphasSource 
VPHASv20160112 
Point source Havphas aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.R;em.line.Halpha 
havphasAperMag4 
vphasSource 
VPHASv20170222 
Point source Havphas aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.R;em.line.Halpha 
havphasAperMag4Err 
vphasSource 
VPHASDR3 
Error in point/extended source Havphas mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.line.Halpha 
havphasAperMag4Err 
vphasSource 
VPHASv20160112 
Error in point/extended source Havphas mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.opt.R;em.line.Halpha 
havphasAperMag4Err 
vphasSource 
VPHASv20170222 
Error in point/extended source Havphas mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.opt.R;em.line.Halpha 
havphasAperMag6 
vphasSource 
VPHASDR3 
Point source Havphas aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.line.Halpha 
havphasAperMag6 
vphasSource 
VPHASv20160112 
Point source Havphas aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.R;em.line.Halpha 
havphasAperMag6 
vphasSource 
VPHASv20170222 
Point source Havphas aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.R;em.line.Halpha 
havphasAperMag6Err 
vphasSource 
VPHASDR3 
Error in point/extended source Havphas mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.line.Halpha 
havphasAperMag6Err 
vphasSource 
VPHASv20160112 
Error in point/extended source Havphas mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.opt.R;em.line.Halpha 
havphasAperMag6Err 
vphasSource 
VPHASv20170222 
Error in point/extended source Havphas mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.opt.R;em.line.Halpha 
havphasAperMagNoAperCorr3 
vphasSource 
VPHASDR3 
Default extended source Havphas aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.line.Halpha 
havphasAperMagNoAperCorr3 
vphasSource 
VPHASv20160112 
Default extended source Havphas aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.R;em.line.Halpha 
havphasAperMagNoAperCorr3 
vphasSource 
VPHASv20170222 
Default extended source Havphas aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.R;em.line.Halpha 
havphasAperMagNoAperCorr4 
vphasSource 
VPHASDR3 
Extended source Havphas aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.line.Halpha 
havphasAperMagNoAperCorr4 
vphasSource 
VPHASv20160112 
Extended source Havphas aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.R;em.line.Halpha 
havphasAperMagNoAperCorr4 
vphasSource 
VPHASv20170222 
Extended source Havphas aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.R;em.line.Halpha 
havphasAperMagNoAperCorr6 
vphasSource 
VPHASDR3 
Extended source Havphas aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.line.Halpha 
havphasAperMagNoAperCorr6 
vphasSource 
VPHASv20160112 
Extended source Havphas aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.R;em.line.Halpha 
havphasAperMagNoAperCorr6 
vphasSource 
VPHASv20170222 
Extended source Havphas aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.R;em.line.Halpha 
havphasAverageConf 
vphasSource 
VPHASDR3 
average confidence in 2 arcsec diameter default aperture (aper3) Havphas 
real 
4 

99999999 
stat.likelihood;em.line.Halpha 
havphasAverageConf 
vphasSource 
VPHASv20160112 
average confidence in 2 arcsec diameter default aperture (aper3) Havphas 
real 
4 

99999999 
stat.likelihood;em.opt.R;em.line.Halpha 
havphasAverageConf 
vphasSource 
VPHASv20170222 
average confidence in 2 arcsec diameter default aperture (aper3) Havphas 
real 
4 

99999999 
stat.likelihood;em.opt.R;em.line.Halpha 
havphasClass 
vphasSource 
VPHASDR3 
discrete image classification flag in Havphas 
smallint 
2 

9999 
src.class;em.line.Halpha 
havphasClass 
vphasSource 
VPHASv20160112 
discrete image classification flag in Havphas 
smallint 
2 

9999 
src.class;em.opt.R;em.line.Halpha 
havphasClass 
vphasSource 
VPHASv20170222 
discrete image classification flag in Havphas 
smallint 
2 

9999 
src.class;em.opt.R;em.line.Halpha 
havphasClassStat 
vphasSource 
VPHASDR3 
N(0,1) stellarnessofprofile statistic in Havphas 
real 
4 

0.9999995e9 
stat;em.line.Halpha 
havphasClassStat 
vphasSource 
VPHASv20160112 
N(0,1) stellarnessofprofile statistic in Havphas 
real 
4 

0.9999995e9 
stat;em.opt.R;em.line.Halpha 
havphasClassStat 
vphasSource 
VPHASv20170222 
N(0,1) stellarnessofprofile statistic in Havphas 
real 
4 

0.9999995e9 
stat;em.opt.R;em.line.Halpha 
havphasEll 
vphasSource 
VPHASDR3 
1b/a, where a/b=semimajor/minor axes in Havphas 
real 
4 

0.9999995e9 
src.ellipticity;em.line.Halpha 
havphasEll 
vphasSource 
VPHASv20160112 
1b/a, where a/b=semimajor/minor axes in Havphas 
real 
4 

0.9999995e9 
src.ellipticity;em.opt.R;em.line.Halpha 
havphasEll 
vphasSource 
VPHASv20170222 
1b/a, where a/b=semimajor/minor axes in Havphas 
real 
4 

0.9999995e9 
src.ellipticity;em.opt.R;em.line.Halpha 
havphaseNum 
vphasMergeLog 
VPHASDR3 
the extension number of this Havphas frame 
tinyint 
1 


meta.number;em.line.Halpha 
havphaseNum 
vphasMergeLog 
VPHASv20160112 
the extension number of this Havphas frame 
tinyint 
1 


meta.number;em.opt.R;em.line.Halpha 
havphaseNum 
vphasMergeLog 
VPHASv20170222 
the extension number of this Havphas frame 
tinyint 
1 


meta.number;em.opt.R;em.line.Halpha 
havphasErrBits 
vphasSource 
VPHASDR3 
processing warning/error bitwise flags in Havphas 
int 
4 

99999999 
meta.code;em.line.Halpha 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
havphasErrBits 
vphasSource 
VPHASv20160112 
processing warning/error bitwise flags in Havphas 
int 
4 

99999999 
meta.code;em.opt.R;em.line.Halpha 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
havphasErrBits 
vphasSource 
VPHASv20170222 
processing warning/error bitwise flags in Havphas 
int 
4 

99999999 
meta.code;em.opt.R;em.line.Halpha 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
havphasEta 
vphasSource 
VPHASDR3 
Offset of Havphas detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.line.Halpha 
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. 
havphasEta 
vphasSource 
VPHASv20160112 
Offset of Havphas detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.opt.R;em.line.Halpha 
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. 
havphasEta 
vphasSource 
VPHASv20170222 
Offset of Havphas detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.opt.R;em.line.Halpha 
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. 
havphasGausig 
vphasSource 
VPHASDR3 
RMS of axes of ellipse fit in Havphas 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.line.Halpha 
havphasGausig 
vphasSource 
VPHASv20160112 
RMS of axes of ellipse fit in Havphas 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.opt.R;em.line.Halpha 
havphasGausig 
vphasSource 
VPHASv20170222 
RMS of axes of ellipse fit in Havphas 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.opt.R;em.line.Halpha 
havphasmfID 
vphasMergeLog 
VPHASDR3 
the UID of the relevant Havphas multiframe 
bigint 
8 


meta.id;obs.field;em.line.Halpha 
havphasmfID 
vphasMergeLog 
VPHASv20160112 
the UID of the relevant Havphas multiframe 
bigint 
8 


meta.id;obs.field;em.opt.R;em.line.Halpha 
havphasmfID 
vphasMergeLog 
VPHASv20170222 
the UID of the relevant Havphas multiframe 
bigint 
8 


meta.id;obs.field;em.opt.R;em.line.Halpha 
havphasMjd 
vphasSource 
VPHASDR3 
The mean Modified Julian Day of each detection 
float 
8 
day 
0.9999995e9 
time.epoch;em.line.Halpha 
havphasMjd 
vphasSource 
VPHASv20160112 
The mean Modified Julian Day of each detection 
float 
8 
day 
0.9999995e9 
time.epoch 
havphasMjd 
vphasSource 
VPHASv20170222 
The mean Modified Julian Day of each detection 
float 
8 
day 
0.9999995e9 
time.epoch 
havphasPA 
vphasSource 
VPHASDR3 
ellipse fit celestial orientation in Havphas 
real 
4 
Degrees 
0.9999995e9 
pos.posAng;em.line.Halpha 
havphasPA 
vphasSource 
VPHASv20160112 
ellipse fit celestial orientation in Havphas 
real 
4 
Degrees 
0.9999995e9 
pos.posAng;em.opt.R;em.line.Halpha 
havphasPA 
vphasSource 
VPHASv20170222 
ellipse fit celestial orientation in Havphas 
real 
4 
Degrees 
0.9999995e9 
pos.posAng;em.opt.R;em.line.Halpha 
havphasPetroMag 
vphasSource 
VPHASDR3 
Extended source Havphas mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.line.Halpha 
havphasPetroMag 
vphasSource 
VPHASv20160112 
Extended source Havphas mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.R;em.line.Halpha 
havphasPetroMag 
vphasSource 
VPHASv20170222 
Extended source Havphas mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.R;em.line.Halpha 
havphasPetroMagErr 
vphasSource 
VPHASDR3 
Error in extended source Havphas mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.line.Halpha 
havphasPetroMagErr 
vphasSource 
VPHASv20160112 
Error in extended source Havphas mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.opt.R;em.line.Halpha 
havphasPetroMagErr 
vphasSource 
VPHASv20170222 
Error in extended source Havphas mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.opt.R;em.line.Halpha 
havphasppErrBits 
vphasSource 
VPHASDR3 
additional WFAU postprocessing error bits in Havphas 
int 
4 

0 
meta.code;em.line.Halpha 
Postprocessing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings: Byte  Bit  Detection quality issue  Threshold or bit mask  Applies to     Decimal  Hexadecimal   0  4  Deblended  16  0x00000010  All VDFS catalogues  0  6  Bad pixel(s) in default aperture  64  0x00000040  All VDFS catalogues  0  7  Low confidence in default aperture  128  0x00000080  All VDFS catalogues  1  12  Lies within detector 16 region of a tile  4096  0x00001000  All catalogues from tiles  2  16  Close to saturated  65536  0x00010000  All VDFS catalogues  2  17  Photometric calibration probably subject to systematic error  131072  0x00020000  VVV only  2  22  Lies within a dither offset of the stacked frame boundary  4194304  0x00400000  All catalogues  2  23  Lies within the underexposed strip (or "ear") of a tile  8388608  0x00800000  All catalogues from tiles  3  24  Lies within an underexposed region of a tile due to missing detector  16777216  0x01000000  All catalogues from tiles  In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information. 
havphasppErrBits 
vphasSource 
VPHASv20160112 
additional WFAU postprocessing error bits in Havphas 
int 
4 

0 
meta.code;em.opt.R;em.line.Halpha 
Postprocessing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings: Byte  Bit  Detection quality issue  Threshold or bit mask  Applies to     Decimal  Hexadecimal   0  4  Deblended  16  0x00000010  All VDFS catalogues  0  6  Bad pixel(s) in default aperture  64  0x00000040  All VDFS catalogues  0  7  Low confidence in default aperture  128  0x00000080  All VDFS catalogues  1  12  Lies within detector 16 region of a tile  4096  0x00001000  All catalogues from tiles  2  16  Close to saturated  65536  0x00010000  All VDFS catalogues  2  17  Photometric calibration probably subject to systematic error  131072  0x00020000  VVV only  2  22  Lies within a dither offset of the stacked frame boundary  4194304  0x00400000  All catalogues  2  23  Lies within the underexposed strip (or "ear") of a tile  8388608  0x00800000  All catalogues from tiles  3  24  Lies within an underexposed region of a tile due to missing detector  16777216  0x01000000  All catalogues from tiles  In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information. 
havphasppErrBits 
vphasSource 
VPHASv20170222 
additional WFAU postprocessing error bits in Havphas 
int 
4 

0 
meta.code;em.opt.R;em.line.Halpha 
Postprocessing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings: Byte  Bit  Detection quality issue  Threshold or bit mask  Applies to     Decimal  Hexadecimal   0  4  Deblended  16  0x00000010  All VDFS catalogues  0  6  Bad pixel(s) in default aperture  64  0x00000040  All VDFS catalogues  0  7  Low confidence in default aperture  128  0x00000080  All VDFS catalogues  1  12  Lies within detector 16 region of a tile  4096  0x00001000  All catalogues from tiles  2  16  Close to saturated  65536  0x00010000  All VDFS catalogues  2  17  Photometric calibration probably subject to systematic error  131072  0x00020000  VVV only  2  22  Lies within a dither offset of the stacked frame boundary  4194304  0x00400000  All catalogues  2  23  Lies within the underexposed strip (or "ear") of a tile  8388608  0x00800000  All catalogues from tiles  3  24  Lies within an underexposed region of a tile due to missing detector  16777216  0x01000000  All catalogues from tiles  In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information. 
havphasPsfMag 
vphasSource 
VPHASDR3 
Point source profilefitted Havphas mag 
real 
4 
mag 
0.9999995e9 
phot.mag;em.line.Halpha 
havphasPsfMag 
vphasSource 
VPHASv20160112 
Point source profilefitted Havphas mag 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.R;em.line.Halpha 
havphasPsfMag 
vphasSource 
VPHASv20170222 
Point source profilefitted Havphas mag 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.R;em.line.Halpha 
havphasPsfMagErr 
vphasSource 
VPHASDR3 
Error in point source profilefitted Havphas mag 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.line.Halpha 
havphasPsfMagErr 
vphasSource 
VPHASv20160112 
Error in point source profilefitted Havphas mag 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.opt.R;em.line.Halpha 
havphasPsfMagErr 
vphasSource 
VPHASv20170222 
Error in point source profilefitted Havphas mag 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.opt.R;em.line.Halpha 
havphasSeqNum 
vphasSource 
VPHASDR3 
the running number of the Havphas detection 
int 
4 

99999999 
meta.number;em.line.Halpha 
havphasSeqNum 
vphasSource 
VPHASv20160112 
the running number of the Havphas detection 
int 
4 

99999999 
meta.number;em.opt.R;em.line.Halpha 
havphasSeqNum 
vphasSource 
VPHASv20170222 
the running number of the Havphas detection 
int 
4 

99999999 
meta.number;em.opt.R;em.line.Halpha 
havphasSerMag2D 
vphasSource 
VPHASDR3 
Extended source Havphas mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.line.Halpha 
havphasSerMag2D 
vphasSource 
VPHASv20160112 
Extended source Havphas mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.R;em.line.Halpha 
havphasSerMag2D 
vphasSource 
VPHASv20170222 
Extended source Havphas mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.opt.R;em.line.Halpha 
havphasSerMag2DErr 
vphasSource 
VPHASDR3 
Error in extended source Havphas mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.line.Halpha 
havphasSerMag2DErr 
vphasSource 
VPHASv20160112 
Error in extended source Havphas mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.opt.R;em.line.Halpha 
havphasSerMag2DErr 
vphasSource 
VPHASv20170222 
Error in extended source Havphas mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.opt.R;em.line.Halpha 
havphasXi 
vphasSource 
VPHASDR3 
Offset of Havphas detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff;em.line.Halpha 
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. 
havphasXi 
vphasSource 
VPHASv20160112 
Offset of Havphas detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff;em.opt.R;em.line.Halpha 
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. 
havphasXi 
vphasSource 
VPHASv20170222 
Offset of Havphas detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff;em.opt.R;em.line.Halpha 
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. 
hCorr 
twompzPhotoz 
TWOMPZ 
H 20mag/sq." isophotal fiducial ell. ap. magnitude with Galactic dust correction {image primary HDU keyword: Hcorr} 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hCorrErr 
twompzPhotoz 
TWOMPZ 
H 1sigma uncertainty in 20mag/sq." aperture {image primary HDU keyword: h_msig_k20fe} 
real 
4 
mag 
0.9999995e9 

HEALPix 
ravedr5Source 
RAVE 
Hierarchical EqualArea isoLatitude Pixelisation value (N_side = 4096) 
bigint 
8 


meta.code 
hemis 
twomass_psc 
TWOMASS 
Hemisphere code for the TWOMASS Observatory from which this source was observed. 
varchar 
1 


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


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



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


meta.code;obs 
hgl 
twomass_scn 
TWOMASS 
Special flag indicating whether or not this scan has a singleframe Hband electronic glitch. 
smallint 
2 


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



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 



hip 
hipparcos_new_reduction 
GAIADR1 
Hipparcos identifier 
int 
4 


meta.main;meta.id 
hip 
tgas_source 
GAIADR1 
Hipparcos identifier 
int 
4 


id.cross 
hip 
tycho2 
GAIADR1 
Hipparcos number 
varchar 
16 


meta.id.cross 
hip_tyc_oid 
gaia_hip_tycho2_match 
GAIADR1 
Initial Gaia Source List identifier for Hipparcos/Tycho2 
bigint 
8 


id.cross 
hlCircRadAs 
atlasDetection 
ATLASDR1 
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 
atlasDetection 
ATLASDR3 
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 
atlasDetection 
ATLASDR4 
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 
atlasDetection 
ATLASDR5 
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 
atlasDetection 
ATLASv20131127 
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 
atlasDetection 
ATLASv20160425 
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 
atlasDetection 
ATLASv20180209 
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 
atlasDetection, atlasDetectionUncorr 
ATLASDR2 
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 
vphasDetection 
VPHASv20160112 
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 
vphasDetection 
VPHASv20170222 
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 
vphasDetection, vphasDetectionUncorr 
VPHASDR3 
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. 
hlCircRadErrAs 
atlasDetection 
ATLASDR1 
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 
atlasDetection 
ATLASDR3 
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 
atlasDetection 
ATLASDR4 
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 
atlasDetection 
ATLASDR5 
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 
atlasDetection 
ATLASv20131127 
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 
atlasDetection 
ATLASv20160425 
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 
atlasDetection 
ATLASv20180209 
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 
atlasDetection, atlasDetectionUncorr 
ATLASDR2 
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 
vphasDetection 
VPHASv20160112 
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 
vphasDetection 
VPHASv20170222 
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 
vphasDetection, vphasDetectionUncorr 
VPHASDR3 
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. 
hlCorSMjRadAs 
atlasDetection 
ATLASDR1 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCorSMjRadAs 
atlasDetection 
ATLASDR3 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCorSMjRadAs 
atlasDetection 
ATLASDR4 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCorSMjRadAs 
atlasDetection 
ATLASDR5 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCorSMjRadAs 
atlasDetection 
ATLASv20131127 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCorSMjRadAs 
atlasDetection 
ATLASv20160425 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCorSMjRadAs 
atlasDetection 
ATLASv20180209 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCorSMjRadAs 
atlasDetection, atlasDetectionUncorr 
ATLASDR2 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCorSMjRadAs 
vphasDetection 
VPHASv20160112 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCorSMjRadAs 
vphasDetection 
VPHASv20170222 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCorSMjRadAs 
vphasDetection, vphasDetectionUncorr 
VPHASDR3 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCorSMnRadAs 
atlasDetection 
ATLASDR1 
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 
atlasDetection 
ATLASDR3 
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 
atlasDetection 
ATLASDR4 
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 
atlasDetection 
ATLASDR5 
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 
atlasDetection 
ATLASv20131127 
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 
atlasDetection 
ATLASv20160425 
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 
atlasDetection 
ATLASv20180209 
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 
atlasDetection, atlasDetectionUncorr 
ATLASDR2 
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 
vphasDetection 
VPHASv20160112 
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 
vphasDetection 
VPHASv20170222 
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 
vphasDetection, vphasDetectionUncorr 
VPHASDR3 
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. 
hlGeoRadAs 
atlasDetection 
ATLASDR1 
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 
atlasDetection 
ATLASDR3 
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 
atlasDetection 
ATLASDR4 
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 
atlasDetection 
ATLASDR5 
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 
atlasDetection 
ATLASv20131127 
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 
atlasDetection 
ATLASv20160425 
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 
atlasDetection 
ATLASv20180209 
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 
atlasDetection, atlasDetectionUncorr 
ATLASDR2 
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 
vphasDetection 
VPHASv20160112 
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 
vphasDetection 
VPHASv20170222 
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 
vphasDetection, vphasDetectionUncorr 
VPHASDR3 
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. 
HLRADIUS 
mgcBrightSpec 
MGC 
Semimajor axis of halflight ellipse 
real 
4 
pixel 


hlSMjRadAs 
atlasDetection 
ATLASDR1 
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 
atlasDetection 
ATLASDR3 
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 
atlasDetection 
ATLASDR4 
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 
atlasDetection 
ATLASDR5 
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 
atlasDetection 
ATLASv20131127 
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 
atlasDetection 
ATLASv20160425 
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 
atlasDetection 
ATLASv20180209 
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 
atlasDetection, atlasDetectionUncorr 
ATLASDR2 
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 
vphasDetection 
VPHASv20160112 
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 
vphasDetection 
VPHASv20170222 
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 
vphasDetection, vphasDetectionUncorr 
VPHASDR3 
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. 
hlSMnRadAs 
atlasDetection 
ATLASDR1 
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 
atlasDetection 
ATLASDR3 
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 
atlasDetection 
ATLASDR4 
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 
atlasDetection 
ATLASDR5 
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 
atlasDetection 
ATLASv20131127 
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 
atlasDetection 
ATLASv20160425 
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 
atlasDetection 
ATLASv20180209 
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 
atlasDetection, atlasDetectionUncorr 
ATLASDR2 
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 
vphasDetection 
VPHASv20160112 
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 
vphasDetection 
VPHASv20170222 
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 
vphasDetection, vphasDetectionUncorr 
VPHASDR3 
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. 
hMag 
ukirtFSstars 
ATLASDR1 
H band total magnitude on the MKO(UFTI) system 
real 
4 
mag 

phot.mag 
hMag 
ukirtFSstars 
ATLASDR2 
H band total magnitude on the MKO(UFTI) system 
real 
4 
mag 

phot.mag 
hMag 
ukirtFSstars 
ATLASDR3 
H band total magnitude on the MKO(UFTI) system 
real 
4 
mag 

phot.mag 
hMag 
ukirtFSstars 
ATLASDR4 
H band total magnitude on the MKO(UFTI) system 
real 
4 
mag 

phot.mag 
hMag 
ukirtFSstars 
ATLASDR5 
H band total magnitude on the MKO(UFTI) system 
real 
4 
mag 

phot.mag 
hMag 
ukirtFSstars 
ATLASv20131127 
H band total magnitude on the MKO(UFTI) system 
real 
4 
mag 

phot.mag 
hMag 
ukirtFSstars 
ATLASv20160425 
H band total magnitude on the MKO(UFTI) system 
real 
4 
mag 

phot.mag 
hMag 
ukirtFSstars 
ATLASv20180209 
H band total magnitude on the MKO(UFTI) system 
real 
4 
mag 

phot.mag 
hMag 
ukirtFSstars 
VPHASDR3 
H band total magnitude on the MKO(UFTI) system 
real 
4 
mag 

phot.mag 
hMag 
ukirtFSstars 
VPHASv20160112 
H band total magnitude on the MKO(UFTI) system 
real 
4 
mag 

phot.mag 
hMag 
ukirtFSstars 
VPHASv20170222 
H band total magnitude on the MKO(UFTI) system 
real 
4 
mag 

phot.mag 
Hmag_2MASS 
ravedr5Source 
RAVE 
H selected default magnitude from 2MASS 
real 
4 
mag 
magnitude 
phot.mag;em.IR.H 
hMagErr 
ukirtFSstars 
ATLASDR1 
H band magnitude error 
real 
4 
mag 

stat.error 
hMagErr 
ukirtFSstars 
ATLASDR2 
H band magnitude error 
real 
4 
mag 

stat.error 
hMagErr 
ukirtFSstars 
ATLASDR3 
H band magnitude error 
real 
4 
mag 

stat.error 
hMagErr 
ukirtFSstars 
ATLASDR4 
H band magnitude error 
real 
4 
mag 

stat.error 
hMagErr 
ukirtFSstars 
ATLASDR5 
H band magnitude error 
real 
4 
mag 

stat.error 
hMagErr 
ukirtFSstars 
ATLASv20131127 
H band magnitude error 
real 
4 
mag 

stat.error 
hMagErr 
ukirtFSstars 
ATLASv20160425 
H band magnitude error 
real 
4 
mag 

stat.error 
hMagErr 
ukirtFSstars 
ATLASv20180209 
H band magnitude error 
real 
4 
mag 

stat.error 
hMagErr 
ukirtFSstars 
VPHASDR3 
H band magnitude error 
real 
4 
mag 

stat.error 
hMagErr 
ukirtFSstars 
VPHASv20160112 
H band magnitude error 
real 
4 
mag 

stat.error 
hMagErr 
ukirtFSstars 
VPHASv20170222 
H band magnitude error 
real 
4 
mag 

stat.error 
hp_mag 
hipparcos_new_reduction 
GAIADR1 
Hipparcos magnitude 
float 
8 
mag 

em.opt;phot.mag 
hr1 
rosat_bsc, rosat_fsc 
ROSAT 
hardness ratio 1 
float 
8 


phot.flux;arith.ratio 
hr2 
rosat_bsc, rosat_fsc 
ROSAT 
hardness ratio 2 
float 
8 


phot.flux;arith.ratio 
HRV 
ravedr5Source 
RAVE 
Heliocentric radial velocity 
real 
4 
km/s 

spect.dopplerVeloc;pos.heliocentric 
hry 
twomass_scn 
TWOMASS 
Flag indicating the Hband array configuration for the camera. 
smallint 
2 


meta.code 
hry 
twomass_sixx2_scn 
TWOMASS 
Hband detector array switched, north only (0=old, 1=new) 
smallint 
2 



hsdFlag_100 
iras_psc 
IRAS 
Source is located in high source density bin (100 micron). 
tinyint 
1 


meta.note 
hsdFlag_12 
iras_psc 
IRAS 
Source is located in high source density bin (12 micron). 
tinyint 
1 


meta.note 
hsdFlag_25 
iras_psc 
IRAS 
Source is located in high source density bin (25 micron). 
tinyint 
1 


meta.note 
hsdFlag_60 
iras_psc 
IRAS 
Source is located in high source density bin (60 micron). 
tinyint 
1 


meta.note 
htm20 
allwise_sc 
WISE 
Level 20 HTM spatial index key 
bigint 
8 



HTMID 
twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0, xmm3dr4 
XMM 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


pos.eq 
htmID 
CurrentAstrometry 
ATLASDR1 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates of device centre 
bigint 
8 

99999999 
pos.eq 
htmID 
CurrentAstrometry 
ATLASDR2 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates of device centre 
bigint 
8 

99999999 
pos.eq 
htmID 
CurrentAstrometry 
ATLASDR3 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates of device centre 
bigint 
8 

99999999 
pos.eq 
htmID 
CurrentAstrometry 
ATLASDR4 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates of device centre 
bigint 
8 

99999999 
pos.eq 
htmID 
CurrentAstrometry 
ATLASDR5 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates of device centre 
bigint 
8 

99999999 
pos.eq 
htmID 
CurrentAstrometry 
ATLASv20131127 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates of device centre 
bigint 
8 

99999999 
pos.eq 
htmID 
CurrentAstrometry 
ATLASv20160425 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates of device centre 
bigint 
8 

99999999 
pos.eq 
htmID 
CurrentAstrometry 
ATLASv20180209 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates of device centre 
bigint 
8 

99999999 
pos.eq 
htmID 
CurrentAstrometry 
VPHASDR3 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates of device centre 
bigint 
8 

99999999 
pos.eq 
htmID 
CurrentAstrometry 
VPHASv20160112 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates of device centre 
bigint 
8 

99999999 
pos.eq 
htmID 
CurrentAstrometry 
VPHASv20170222 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates of device centre 
bigint 
8 

99999999 
pos.eq 
htmID 
atlasDetection 
ATLASDR3 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


pos.eq 
htmID 
atlasDetection 
ATLASDR4 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


pos.eq 
htmID 
atlasDetection 
ATLASDR5 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


pos.eq 
htmID 
atlasDetection 
ATLASv20131127 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


pos.eq 
htmID 
atlasDetection 
ATLASv20160425 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


pos.eq 
htmID 
atlasDetection 
ATLASv20180209 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


pos.eq 
htmID 
atlasDetection, atlasDetectionUncorr 
ATLASDR2 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


pos.eq 
htmID 
atlasDetection, atlasMergeLog, atlasSource 
ATLASDR1 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


pos.eq 
htmID 
catwise_2020, catwise_prelim 
WISE 
Level 20 Hierarchical Triangular Mesh (HTM) index for equatorial coordinates 
bigint 
8 


pos.eq 
htmID 
denisDR3Source 
DENIS 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


pos.eq 
htmID 
first08Jul16Source, firstSource, firstSource12Feb16 
FIRST 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


pos.eq 
htmID 
gaia_source 
GAIADR2 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


pos.eq 
htmID 
gaia_source, hipparcos_new_reduction, igsl_source, tgas_source, tycho2 
GAIADR1 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


pos.eq 
htmID 
glimpse1_hrc, glimpse1_mca, glimpse2_hrc, glimpse2_mca, glimpse_hrc_inter, glimpse_mca_inter 
GLIMPSE 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


pos.eq 
htmID 
iras_psc 
IRAS 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


pos.eq 
htmID 
mgcDetection 
MGC 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


pos.eq 
htmID 
nvssSource 
NVSS 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


pos.eq 
htmID 
ravedr5Source 
RAVE 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


pos.general 
htmID 
rosat_bsc, rosat_fsc 
ROSAT 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


pos.eq 
htmID 
twomass_psc, twomass_scn, twomass_sixx2_psc, twomass_sixx2_scn, twomass_sixx2_xsc, twomass_xsc 
TWOMASS 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


pos.eq 
htmID 
twompzPhotoz 
TWOMPZ 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


pos 
htmID 
vphasDetection 
VPHASv20160112 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


pos.eq 
htmID 
vphasDetection 
VPHASv20170222 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


pos.eq 
htmID 
vphasDetection, vphasDetectionUncorr 
VPHASDR3 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


pos.eq 
htmID 
vphasMergeLog 
VPHASv20160112 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


pos 
htmID 
vphasMergeLog 
VPHASv20170222 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


pos 
htmID 
vphasMergeLog, vphasSource 
VPHASDR3 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


pos 
htmID 
wise_allskysc, wise_prelimsc 
WISE 
Hierarchical Triangular Mesh (HTM) index for equatorial coordinates (similar to spt_ind in IPAC IRSA schema, but recomputed to level 20) 
bigint 
8 


pos.eq 