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Glossary of OSA attributes
This Glossary alphabetically lists all attributes used in the OSAv20230621 database(s) held in the OSA. If you would like to have more information about the schema tables please use the OSAv20230621 Schema Browser (other Browser versions).

A

B

C

D

E

F

G

H

I

J

K

L

M

N

O

P

Q

R

S

T

U

V

W

X

Y

Z

H
Name	Schema Table	Database	Description	Type	Length	Unit	Default Value	Unified Content Descriptor
h_2mrat	twomass_scn	TWOMASS	H-band 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 5-sigma isophote.	real	4			phys.size.axisRatio
h_5sig_phi	twomass_xsc	TWOMASS	H angle to 5-sigma 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 3-sigma 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 bi-symmetric cross-correlation chi.	real	4			stat.fit.param
h_bisym_rat	twomass_xsc	TWOMASS	H bi-symmetric 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 H-band magnitude.	real	4	mag	H-band	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 5-sigma to 3-sigma 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 H-Ks color, computed from the H-band and Ks-band 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 H-band 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 H-band 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 H-band magnitude entry is "null".	float	8	mag
h_m_2mass	wise_allskysc	WISE	2MASS H-band 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 H-band magnitude entry is default.	real	4	mag	-0.9999995e9
h_m_2mass	wise_prelimsc	WISE	2MASS H-band 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 H-band 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	H-band "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 half-light 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 1-sigma uncertainty in 10 arcsec circular ap. mag.	real	4	mag		stat.error
h_msig_15	twomass_xsc	TWOMASS	H 1-sigma uncertainty in 15 arcsec circular ap. mag.	real	4	mag		stat.error
h_msig_20	twomass_xsc	TWOMASS	H 1-sigma uncertainty in 20 arcsec circular ap. mag.	real	4	mag		stat.error
h_msig_25	twomass_xsc	TWOMASS	H 1-sigma uncertainty in 25 arcsec circular ap. mag.	real	4	mag		stat.error
h_msig_2mass	allwise_sc	WISE	2MASS H-band corrected photometric uncertainty of the associated 2MASS PSC source. This column is "null" if there is no associated 2MASS PSC source or if the 2MASS PSC H-band uncertainty entry is "null".	float	8	mag
h_msig_2mass	wise_allskysc	WISE	2MASS H-band 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 H-band uncertainty entry is default.	real	4	mag	-0.9999995e9
h_msig_2mass	wise_prelimsc	WISE	2MASS H-band 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 H-band uncertainty entry is default	real	4	mag	-0.9999995e9
h_msig_30	twomass_xsc	TWOMASS	H 1-sigma uncertainty in 30 arcsec circular ap. mag.	real	4	mag		stat.error
h_msig_40	twomass_xsc	TWOMASS	H 1-sigma uncertainty in 40 arcsec circular ap. mag.	real	4	mag		stat.error
h_msig_5	twomass_xsc	TWOMASS	H 1-sigma uncertainty in 5 arcsec circular ap. mag.	real	4	mag		stat.error
h_msig_50	twomass_xsc	TWOMASS	H 1-sigma uncertainty in 50 arcsec circular ap. mag.	real	4	mag		stat.error
h_msig_60	twomass_xsc	TWOMASS	H 1-sigma uncertainty in 60 arcsec circular ap. mag.	real	4	mag		stat.error
h_msig_7	twomass_sixx2_xsc	TWOMASS	H 1-sigma uncertainty in 7 arcsec circular ap. mag	real	4	mag
h_msig_7	twomass_xsc	TWOMASS	H 1-sigma uncertainty in 7 arcsec circular ap. mag.	real	4	mag		stat.error
h_msig_70	twomass_xsc	TWOMASS	H 1-sigma uncertainty in 70 arcsec circular ap. mag.	real	4	mag		stat.error
h_msig_c	twomass_xsc	TWOMASS	H 1-sigma uncertainty in Kron circular mag.	real	4	mag		stat.error
h_msig_e	twomass_xsc	TWOMASS	H 1-sigma uncertainty in Kron elliptical mag.	real	4	mag		stat.error
h_msig_ext	twomass_sixx2_xsc	TWOMASS	H 1-sigma uncertainty in mag from fit extrapolation	real	4	mag
h_msig_ext	twomass_xsc	TWOMASS	H 1-sigma uncertainty in mag from fit extrapolation.	real	4	mag		stat.error
h_msig_fc	twomass_xsc	TWOMASS	H 1-sigma uncertainty in fiducial Kron circ. mag.	real	4	mag		stat.error
h_msig_fe	twomass_xsc	TWOMASS	H 1-sigma uncertainty in fiducial Kron ell. mag.	real	4	mag		stat.error
h_msig_i20c	twomass_xsc	TWOMASS	H 1-sigma uncertainty in 20mag/sq." iso. circ. mag.	real	4	mag		stat.error
h_msig_i20e	twomass_xsc	TWOMASS	H 1-sigma uncertainty in 20mag/sq." iso. ell. mag.	real	4	mag		stat.error
h_msig_i21c	twomass_xsc	TWOMASS	H 1-sigma uncertainty in 21mag/sq." iso. circ. mag.	real	4	mag		stat.error
h_msig_i21e	twomass_xsc	TWOMASS	H 1-sigma uncertainty in 21mag/sq." iso. ell. mag.	real	4	mag		stat.error
h_msig_j21fc	twomass_xsc	TWOMASS	H 1-sigma uncertainty in 21mag/sq." iso.fid.circ.mag.	real	4	mag		stat.error
h_msig_j21fe	twomass_xsc	TWOMASS	H 1-sigma uncertainty in 21mag/sq." iso.fid.ell.mag.	real	4	mag		stat.error
h_msig_k20fc	twomass_xsc	TWOMASS	H 1-sigma uncertainty in 20mag/sq." iso.fid.circ. mag.	real	4	mag		stat.error
h_msig_k20fe	twomass_sixx2_xsc	TWOMASS	H 1-sigma uncertainty in 20mag/sq.″ iso.fid.ell.mag	real	4	mag
h_msig_k20fe	twomass_xsc	TWOMASS	H 1-sigma uncertainty in 20mag/sq." iso.fid.ell.mag.	real	4	mag		stat.error
h_msig_stdap	twomass_psc	TWOMASS	Uncertainty in the H-band standard aperture magnitude.	real	4	mag		phot.flux
h_msig_sys	twomass_xsc	TWOMASS	H 1-sigma uncertainty in system photometry mag.	real	4	mag		stat.error
h_msigcom	twomass_psc	TWOMASS	Combined, or total photometric uncertainty for the default H-band magnitude.	real	4	mag	H-band	phot.flux
h_msigcom	twomass_sixx2_psc	TWOMASS	combined (total) H band photometric uncertainty	real	4	mag
h_msnr10	twomass_scn	TWOMASS	The estimated H-band 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 H-band 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 5-sigma to 3-sigma percent area change.	smallint	2			FIT_PARAM
h_phi	twomass_xsc	TWOMASS	H angle to 3-sigma major axis (E of N).	smallint	2	degrees		pos.posAng
h_psfchi	twomass_psc	TWOMASS	Reduced chi-squared goodness-of-fit value for the H-band profile-fit photometry made on the 1.3 s "Read_2" exposures.	real	4			stat.fit.param
h_psp	twomass_scn	TWOMASS	H-band 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	Base-10 logarithm of the mode of the noise distribution for all point source detections in the scan, where the noise is estimated from the measured H-band 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 semi-major axis.	real	4	arcsec		phys.angSize;src
h_r_eff	twomass_xsc	TWOMASS	H half-light (integrated half-flux 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. semi-major 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. semi-major 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	H-band 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	RMS-error of H-band 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	H-band "scan" signal-to-noise ratio.	real	4	mag		instr.det.noise
h_snr	twomass_sixx2_psc	TWOMASS	H band "scan" signal-to-noise ratio	real	4
h_subst2	twomass_xsc	TWOMASS	H residual background #2 (score).	real	4			meta.code
h_zp_ap	twomass_scn	TWOMASS	Photometric zero-point for H-band aperture photometry.	real	4	mag		phot.mag;arith.zp
h_zp_ap	twomass_sixx2_scn	TWOMASS	H band ap. calibration photometric zero-point for scan	real	4	mag
h_zperr_ap	twomass_scn	TWOMASS	RMS-error of zero-point for H-band aperture photometry	real	4	mag		stat.error
h_zperr_ap	twomass_sixx2_scn	TWOMASS	H band ap. calibration rms error of zero-point 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 half-light 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 half-light 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 half-light 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 half-light 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 half-light 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 half-light 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 half-light 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 half-light 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 half-light 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 half-light 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 half-light 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) stellarness-of-profile statistic in Havphas	real	4		-0.9999995e9	stat;em.line.Halpha
havphasClassStat	vphasSource	VPHASv20160112	N(0,1) stellarness-of-profile statistic in Havphas	real	4		-0.9999995e9	stat;em.opt.R;em.line.Halpha
havphasClassStat	vphasSource	VPHASv20170222	N(0,1) stellarness-of-profile statistic in Havphas	real	4		-0.9999995e9	stat;em.opt.R;em.line.Halpha
havphasEll	vphasSource	VPHASDR3	1-b/a, where a/b=semi-major/minor axes in Havphas	real	4		-0.9999995e9	src.ellipticity;em.line.Halpha
havphasEll	vphasSource	VPHASv20160112	1-b/a, where a/b=semi-major/minor axes in Havphas	real	4		-0.9999995e9	src.ellipticity;em.opt.R;em.line.Halpha
havphasEll	vphasSource	VPHASv20170222	1-b/a, where a/b=semi-major/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 post-processing error bits in Havphas	int	4		0	meta.code;em.line.Halpha
			Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte 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 post-processing error bits in Havphas	int	4		0	meta.code;em.opt.R;em.line.Halpha
			Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte 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 post-processing error bits in Havphas	int	4		0	meta.code;em.opt.R;em.line.Halpha
			Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte 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 profile-fitted Havphas mag	real	4	mag	-0.9999995e9	phot.mag;em.line.Halpha
havphasPsfMag	vphasSource	VPHASv20160112	Point source profile-fitted Havphas mag	real	4	mag	-0.9999995e9	phot.mag;em.opt.R;em.line.Halpha
havphasPsfMag	vphasSource	VPHASv20170222	Point source profile-fitted Havphas mag	real	4	mag	-0.9999995e9	phot.mag;em.opt.R;em.line.Halpha
havphasPsfMagErr	vphasSource	VPHASDR3	Error in point source profile-fitted Havphas mag	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.line.Halpha
havphasPsfMagErr	vphasSource	VPHASv20160112	Error in point source profile-fitted Havphas mag	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.R;em.line.Halpha
havphasPsfMagErr	vphasSource	VPHASv20170222	Error in point source profile-fitted 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 (profile-fitted)	real	4	mag	-0.9999995e9	phot.mag;em.line.Halpha
havphasSerMag2D	vphasSource	VPHASv20160112	Extended source Havphas mag (profile-fitted)	real	4	mag	-0.9999995e9	phot.mag;em.opt.R;em.line.Halpha
havphasSerMag2D	vphasSource	VPHASv20170222	Extended source Havphas mag (profile-fitted)	real	4	mag	-0.9999995e9	phot.mag;em.opt.R;em.line.Halpha
havphasSerMag2DErr	vphasSource	VPHASDR3	Error in extended source Havphas mag (profile-fitted)	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.line.Halpha
havphasSerMag2DErr	vphasSource	VPHASv20160112	Error in extended source Havphas mag (profile-fitted)	real	4	mag	-0.9999995e9	stat.error;phot.mag;em.opt.R;em.line.Halpha
havphasSerMag2DErr	vphasSource	VPHASv20170222	Error in extended source Havphas mag (profile-fitted)	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 1-sigma uncertainty in 20mag/sq." aperture {image primary HDU keyword: h_msig_k20fe}	real	4	mag	-0.9999995e9
HEALPix	ravedr5Source	RAVE	Hierarchical Equal-Area iso-Latitude 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 single-frame H-band electronic glitch.	smallint	2			meta.code
hgl	twomass_sixx2_scn	TWOMASS	single-frame H-band glitch flag (0:not found|1: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 half-light 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 half-light 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 half-light 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 half-light 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 half-light 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 half-light 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 half-light 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 half-light 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 half-light 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 half-light 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 half-light 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 Half-light semi-major axis	real	4	arcsec	-0.9999995e9
hlCorSMjRadAs	atlasDetection	ATLASDR3	Seeing corrected Half-light semi-major axis	real	4	arcsec	-0.9999995e9
hlCorSMjRadAs	atlasDetection	ATLASDR4	Seeing corrected Half-light semi-major axis	real	4	arcsec	-0.9999995e9
hlCorSMjRadAs	atlasDetection	ATLASDR5	Seeing corrected Half-light semi-major axis	real	4	arcsec	-0.9999995e9
hlCorSMjRadAs	atlasDetection	ATLASv20131127	Seeing corrected Half-light semi-major axis	real	4	arcsec	-0.9999995e9
hlCorSMjRadAs	atlasDetection	ATLASv20160425	Seeing corrected Half-light semi-major axis	real	4	arcsec	-0.9999995e9
hlCorSMjRadAs	atlasDetection	ATLASv20180209	Seeing corrected Half-light semi-major axis	real	4	arcsec	-0.9999995e9
hlCorSMjRadAs	atlasDetection, atlasDetectionUncorr	ATLASDR2	Seeing corrected Half-light semi-major axis	real	4	arcsec	-0.9999995e9
hlCorSMjRadAs	vphasDetection	VPHASv20160112	Seeing corrected Half-light semi-major axis	real	4	arcsec	-0.9999995e9
hlCorSMjRadAs	vphasDetection	VPHASv20170222	Seeing corrected Half-light semi-major axis	real	4	arcsec	-0.9999995e9
hlCorSMjRadAs	vphasDetection, vphasDetectionUncorr	VPHASDR3	Seeing corrected Half-light semi-major axis	real	4	arcsec	-0.9999995e9
hlCorSMnRadAs	atlasDetection	ATLASDR1	Seeing corrected Half-light semi-minor 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 Half-light semi-minor 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 Half-light semi-minor 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 Half-light semi-minor 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 Half-light semi-minor 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 Half-light semi-minor 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 Half-light semi-minor 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 Half-light semi-minor 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 Half-light semi-minor 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 Half-light semi-minor 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 Half-light semi-minor 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 half-light 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 half-light 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 half-light 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 half-light 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 half-light 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 half-light 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 half-light 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 half-light 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 half-light 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 half-light 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 half-light 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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	Semi-major axis of half-light ellipse	real	4	pixel
hlSMjRadAs	atlasDetection	ATLASDR1	Half-light semi-major 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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	Half-light semi-major 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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	Half-light semi-major 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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	Half-light semi-major 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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	Half-light semi-major 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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	Half-light semi-major 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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	Half-light semi-major 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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	Half-light semi-major 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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	Half-light semi-major 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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	Half-light semi-major 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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	Half-light semi-major 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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	Half-light semi-minor 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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	Half-light semi-minor 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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	Half-light semi-minor 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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	Half-light semi-minor 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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	Half-light semi-minor 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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	Half-light semi-minor 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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	Half-light semi-minor 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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	Half-light semi-minor 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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	Half-light semi-minor 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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	Half-light semi-minor 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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	Half-light semi-minor 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 semi-major axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1-ellipticity. 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 (1-ellipticity)*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 H-band array configuration for the camera.	smallint	2			meta.code
hry	twomass_sixx2_scn	TWOMASS	H-band 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 co-ordinates	bigint	8			pos.eq
htmID	CurrentAstrometry	ATLASDR1	Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre	bigint	8		-99999999	pos.eq
htmID	CurrentAstrometry	ATLASDR2	Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre	bigint	8		-99999999	pos.eq
htmID	CurrentAstrometry	ATLASDR3	Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre	bigint	8		-99999999	pos.eq
htmID	CurrentAstrometry	ATLASDR4	Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre	bigint	8		-99999999	pos.eq
htmID	CurrentAstrometry	ATLASDR5	Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre	bigint	8		-99999999	pos.eq
htmID	CurrentAstrometry	ATLASv20131127	Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre	bigint	8		-99999999	pos.eq
htmID	CurrentAstrometry	ATLASv20160425	Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre	bigint	8		-99999999	pos.eq
htmID	CurrentAstrometry	ATLASv20180209	Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre	bigint	8		-99999999	pos.eq
htmID	CurrentAstrometry	VPHASDR3	Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre	bigint	8		-99999999	pos.eq
htmID	CurrentAstrometry	VPHASv20160112	Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre	bigint	8		-99999999	pos.eq
htmID	CurrentAstrometry	VPHASv20170222	Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre	bigint	8		-99999999	pos.eq
htmID	atlasDetection	ATLASDR3	Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates	bigint	8			pos.eq
htmID	atlasDetection	ATLASDR4	Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates	bigint	8			pos.eq
htmID	atlasDetection	ATLASDR5	Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates	bigint	8			pos.eq
htmID	atlasDetection	ATLASv20131127	Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates	bigint	8			pos.eq
htmID	atlasDetection	ATLASv20160425	Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates	bigint	8			pos.eq
htmID	atlasDetection	ATLASv20180209	Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates	bigint	8			pos.eq
htmID	atlasDetection, atlasDetectionUncorr	ATLASDR2	Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates	bigint	8			pos.eq
htmID	atlasDetection, atlasMergeLog, atlasSource	ATLASDR1	Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates	bigint	8			pos.eq
htmID	catwise_2020, catwise_prelim	WISE	Level 20 Hierarchical Triangular Mesh (HTM) index for equatorial co-ordinates	bigint	8			pos.eq
htmID	denisDR3Source	DENIS	Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates	bigint	8			pos.eq
htmID	first08Jul16Source, firstSource, firstSource12Feb16	FIRST	Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates	bigint	8			pos.eq
htmID	gaia_source	GAIADR2	Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates	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 co-ordinates	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 co-ordinates	bigint	8			pos.eq
htmID	iras_psc	IRAS	Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates	bigint	8			pos.eq
htmID	mgcDetection	MGC	Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates	bigint	8			pos.eq
htmID	nvssSource	NVSS	Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates	bigint	8			pos.eq
htmID	ravedr5Source	RAVE	Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates	bigint	8			pos.general
htmID	rosat_bsc, rosat_fsc	ROSAT	Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates	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 co-ordinates	bigint	8			pos.eq
htmID	twompzPhotoz	TWOMPZ	Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates	bigint	8			pos
htmID	vphasDetection	VPHASv20160112	Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates	bigint	8			pos.eq
htmID	vphasDetection	VPHASv20170222	Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates	bigint	8			pos.eq
htmID	vphasDetection, vphasDetectionUncorr	VPHASDR3	Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates	bigint	8			pos.eq
htmID	vphasMergeLog	VPHASv20160112	Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates	bigint	8			pos
htmID	vphasMergeLog	VPHASv20170222	Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates	bigint	8			pos
htmID	vphasMergeLog, vphasSource	VPHASDR3	Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates	bigint	8			pos
htmID	wise_allskysc, wise_prelimsc	WISE	Hierarchical Triangular Mesh (HTM) index for equatorial co-ordinates (similar to spt_ind in IPAC IRSA schema, but recomputed to level 20)	bigint	8			pos.eq