VSA Browser

Glossary of VSA attributes

This Glossary alphabetically lists all attributes used in the VSAv20110218 database(s) held in the VSA. If you would like to have more information about the schema tables please use the VSAv20110218 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 twomass SIXDF H magnitude (HEXT) used for H selection real 4 mag

h_2mrat twomass_scn 2MASS H-band average 2nd image moment ratio. real 4 FIT_PARAM_VALUE

h_2mrat twomass_sixx2_scn 2MASS H band average 2nd image moment ratio for scan real 4

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

h_5sig_phi twomass_xsc 2MASS H angle to 5-sigma major axis (E of N). smallint 2 degrees ERROR

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

h_ba twomass_xsc 2MASS H minor/major axis ratio fit to the 3-sigma isophote. real 4 PHYS_AXIS-RATIO

h_back twomass_xsc 2MASS H coadd median background. real 4 CODE_MISC

h_bisym_chi twomass_xsc 2MASS H bi-symmetric cross-correlation chi. real 4 FIT_PARAM_VALUE

h_bisym_rat twomass_xsc 2MASS H bi-symmetric flux ratio. real 4 PHOT_FLUX_RATIO

h_bndg_amp twomass_xsc 2MASS H banding maximum FT amplitude on this side of coadd. real 4 DN FIT_PARAM_VALUE

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

h_cmsig twomass_psc 2MASS Corrected photometric uncertainty for the default H-band magnitude. real 4 mag SPECT_FLUX_VALUE

h_con_indx twomass_xsc 2MASS H concentration index r_75%/r_25%. real 4 PHYS_CONCENT_INDEX

h_d_area twomass_xsc 2MASS H 5-sigma to 3-sigma differential area. smallint 2 FIT_RESIDUAL

h_flg_10 twomass_xsc 2MASS H confusion flag for 10 arcsec circular ap. mag. smallint 2 CODE_MISC

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

h_k twomass_sixx2_psc 2MASS 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 2MASS Default H-band magnitude real 4 mag SPECT_FLUX_VALUE

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

h_m_ext twomass_sixx2_xsc 2MASS H mag from fit extrapolation real 4 mag

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

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

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

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

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

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

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

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

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

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

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

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

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

h_m_stdap twomass_psc 2MASS H-band "standard" aperture magnitude. real 4 mag SPECT_FLUX_VALUE

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

h_mnsurfb_eff twomass_xsc 2MASS H mean surface brightness at the half-light radius. real 4 mag PHOT_SB_GENERAL

h_msig twomass_sixx2_psc 2MASS H "default" mag uncertainty real 4 mag

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

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

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

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

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

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

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

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

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

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

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

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

h_msig_c twomass_xsc 2MASS H 1-sigma uncertainty in Kron circular mag. real 4 mag ERROR

h_msig_e twomass_xsc 2MASS H 1-sigma uncertainty in Kron elliptical mag. real 4 mag ERROR

h_msig_ext twomass_sixx2_xsc 2MASS H 1-sigma uncertainty in mag from fit extrapolation real 4 mag

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

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

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

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

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

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

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

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

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

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

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

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

h_msig_stdap twomass_psc 2MASS Uncertainty in the H-band standard aperture magnitude. real 4 mag SPECT_FLUX_VALUE

h_msig_sys twomass_xsc 2MASS H 1-sigma uncertainty in system photometry mag. real 4 mag ERROR

h_msigcom twomass_psc 2MASS Combined, or total photometric uncertainty for the default H-band magnitude. real 4 mag SPECT_FLUX_VALUE

h_msigcom twomass_sixx2_psc 2MASS combined (total) H band photometric uncertainty real 4 mag

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

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

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

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

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

h_peak twomass_xsc 2MASS H peak pixel brightness. real 4 mag PHOT_SB_GENERAL

h_perc_darea twomass_xsc 2MASS H 5-sigma to 3-sigma percent area change. smallint 2 FIT_PARAM

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

h_psfchi twomass_psc 2MASS 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 FIT_PARAM_VALUE

h_psp twomass_scn 2MASS H-band photometric sensitivity paramater (PSP). real 4 INST_SENSITIVITY

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

h_pts_noise twomass_scn 2MASS 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 INST_NOISE

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

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

h_r_e twomass_xsc 2MASS H Kron elliptical aperture semi-major axis. real 4 arcsec EXTENSION_RAD

h_r_eff twomass_xsc 2MASS H half-light (integrated half-flux point) radius. real 4 arcsec EXTENSION_RAD

h_r_i20c twomass_xsc 2MASS H 20mag/sq." isophotal circular aperture radius. real 4 arcsec EXTENSION_RAD

h_r_i20e twomass_xsc 2MASS H 20mag/sq." isophotal elliptical ap. semi-major axis. real 4 arcsec EXTENSION_RAD

h_r_i21c twomass_xsc 2MASS H 21mag/sq." isophotal circular aperture radius. real 4 arcsec EXTENSION_RAD

h_r_i21e twomass_xsc 2MASS H 21mag/sq." isophotal elliptical ap. semi-major axis. real 4 arcsec EXTENSION_RAD

h_resid_ann twomass_xsc 2MASS H residual annulus background median. real 4 DN CODE_MISC

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

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

h_sc_msh twomass_xsc 2MASS H median shape score. real 4 CODE_MISC

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

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

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

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

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

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

h_seetrack twomass_xsc 2MASS H band seetracking score. real 4 CODE_MISC

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

h_shape_avg twomass_scn 2MASS H-band average seeing shape for scan. real 4 INST_SEEING

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

h_shape_rms twomass_scn 2MASS RMS-error of H-band average seeing shape. real 4 INST_SEEING

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

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

h_snr twomass_psc 2MASS H-band "scan" signal-to-noise ratio. real 4 mag INST_NOISE

h_snr twomass_sixx2_psc 2MASS H band "scan" signal-to-noise ratio real 4

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

h_zp_ap twomass_scn 2MASS Photometric zero-point for H-band aperture photometry. real 4 mag PHOT_ZP

h_zp_ap twomass_sixx2_scn 2MASS H band ap. calibration photometric zero-point for scan real 4 mag

h_zperr_ap twomass_scn 2MASS RMS-error of zero-point for H-band aperture photometry real 4 mag FIT_ERROR

h_zperr_ap twomass_sixx2_scn 2MASS H band ap. calibration rms error of zero-point for scan real 4 mag

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

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

halfFlux svNgc253Detection VSASVNGC253 Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 PHOT_INTENSITY_ADU

halfFlux svOrionDetection VSASVORION Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 PHOT_INTENSITY_ADU

halfFlux ultravistaDetection VSAUltraVISTA Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation, not available in SE output {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 PHOT_INTENSITY_ADU

halfFlux ultravistaDetection, videoDetection VSAQC Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation, not available in SE output {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 PHOT_INTENSITY_ADU

halfFlux ultravistaListRemeasurement VSAUltraVISTA Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 PHOT_INTENSITY_ADU

halfFlux ultravistaListRemeasurement, vhsDetection, vhsListRemeasurement, videoListRemeasurement, vikingDetection, vikingListRemeasurement, vmcDetection, vmcListRemeasurement, vvvDetection, vvvListRemeasurement VSAQC Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} real 4 ADU -0.9999995e9 PHOT_INTENSITY_ADU

halfFluxErr svNgc253Detection VSASVNGC253 error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 ERROR

halfFluxErr svOrionDetection VSASVORION error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 ERROR

halfFluxErr ultravistaDetection VSAUltraVISTA error on Half flux, not available in SE output {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 ERROR

halfFluxErr ultravistaDetection, videoDetection VSAQC error on Half flux, not available in SE output {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 ERROR

halfFluxErr ultravistaListRemeasurement VSAUltraVISTA error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 ERROR

halfFluxErr ultravistaListRemeasurement, vhsDetection, vhsListRemeasurement, videoListRemeasurement, vikingDetection, vikingListRemeasurement, vmcDetection, vmcListRemeasurement, vvvDetection, vvvListRemeasurement VSAQC error on Half flux {catalogue TType keyword: Half_flux_err} real 4 ADU -0.9999995e9 ERROR

halfMag svNgc253Detection VSASVNGC253 Calibrated magnitude within circular aperture halfRad real 4 mag PHOT_INT-MAG

halfMag svOrionDetection VSASVORION Calibrated magnitude within circular aperture halfRad real 4 mag PHOT_INT-MAG

halfMag ultravistaDetection VSAUltraVISTA Calibrated magnitude within circular aperture halfRad, not available in SE output real 4 mag PHOT_INT-MAG

halfMag ultravistaDetection, videoDetection VSAQC Calibrated magnitude within circular aperture halfRad, not available in SE output real 4 mag PHOT_INT-MAG

halfMag ultravistaListRemeasurement VSAUltraVISTA Calibrated magnitude within circular aperture halfRad real 4 mag PHOT_INT-MAG

halfMag ultravistaListRemeasurement, vhsDetection, vhsListRemeasurement, videoListRemeasurement, vikingDetection, vikingListRemeasurement, vmcDetection, vmcListRemeasurement, vvvDetection, vvvListRemeasurement VSAQC Calibrated magnitude within circular aperture halfRad real 4 mag PHOT_INT-MAG

halfMagErr svNgc253Detection VSASVNGC253 Calibrated error on Half magnitude real 4 mag ERROR

halfMagErr svOrionDetection VSASVORION Calibrated error on Half magnitude real 4 mag ERROR

halfMagErr ultravistaDetection VSAUltraVISTA Calibrated error on Half magnitude, not available in SE output real 4 mag ERROR

halfMagErr ultravistaDetection, videoDetection VSAQC Calibrated error on Half magnitude, not available in SE output real 4 mag ERROR

halfMagErr ultravistaListRemeasurement VSAUltraVISTA Calibrated error on Half magnitude real 4 mag ERROR

halfMagErr ultravistaListRemeasurement, vhsDetection, vhsListRemeasurement, videoListRemeasurement, vikingDetection, vikingListRemeasurement, vmcDetection, vmcListRemeasurement, vvvDetection, vvvListRemeasurement VSAQC Calibrated error on Half magnitude real 4 mag ERROR

halfRad svNgc253Detection VSASVNGC253 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 EXTENSION_RAD

halfRad svOrionDetection VSASVORION 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 EXTENSION_RAD

halfRad ultravistaDetection VSAUltraVISTA SExtractor half-light radius (FRAC_RADIUS), calcuated assuming Kron flux is total flux {catalogue TType keyword: Half_radius} real 4 pixels EXTENSION_RAD

halfRad ultravistaDetection, videoDetection VSAQC SExtractor half-light radius (FRAC_RADIUS), calcuated assuming Kron flux is total flux {catalogue TType keyword: Half_radius} real 4 pixels EXTENSION_RAD

halfRad ultravistaListRemeasurement VSAUltraVISTA 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 EXTENSION_RAD

halfRad ultravistaListRemeasurement, vhsDetection, vhsListRemeasurement, videoListRemeasurement, vikingDetection, vikingListRemeasurement, vmcDetection, vmcListRemeasurement, vvvDetection, vvvListRemeasurement VSAQC 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 EXTENSION_RAD

hAperMag1 vvvSource VSAQC Extended source H aperture corrected mag (0.7 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

hAperMag1 vvvSource VSAVVV Extended source H aperture corrected mag (0.7 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

hAperMag1Err vvvSource VSAQC Error in extended source H mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

hAperMag1Err vvvSource VSAVVV Error in extended source H mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

hAperMag3 svNgc253Source VSASVNGC253 Default point/extended source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

hAperMag3 svOrionSource VSASVORION Default point/extended source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

hAperMag3 ultravistaSource VSAUltraVISTA Default point/extended source H mag, no aperture correction applied
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

hAperMag3 ultravistaSource, videoSource VSAQC Default point/extended source H mag, no aperture correction applied
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

hAperMag3 vhsSource VSAVHS Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

hAperMag3 vhsSource, vikingSource VSAQC Default point source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

hAperMag3 vvvSource VSAQC Default point/extended source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

hAperMag3 vvvSource VSAVVV Default point/extended source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

hAperMag3Err svNgc253Source VSASVNGC253 Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

hAperMag3Err svOrionSource VSASVORION Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

hAperMag3Err ultravistaSource VSAUltraVISTA Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

hAperMag3Err ultravistaSource, vhsSource, videoSource, vikingSource, vvvSource VSAQC Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

hAperMag4 svNgc253Source VSASVNGC253 Extended source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

hAperMag4 svOrionSource VSASVORION Extended source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

hAperMag4 ultravistaSource VSAUltraVISTA Extended source H mag, no aperture correction applied real 4 mag -0.9999995e9 PHOT_MAG

hAperMag4 ultravistaSource, videoSource VSAQC Extended source H mag, no aperture correction applied real 4 mag -0.9999995e9 PHOT_MAG

hAperMag4 vhsSource VSAVHS Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

hAperMag4 vhsSource, vikingSource VSAQC Point source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

hAperMag4 vvvSource VSAQC Extended source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

hAperMag4 vvvSource VSAVVV Extended source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

hAperMag4Err svNgc253Source VSASVNGC253 Error in extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

hAperMag4Err svOrionSource VSASVORION Error in extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

hAperMag4Err ultravistaSource VSAUltraVISTA Error in extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

hAperMag4Err ultravistaSource, videoSource, vvvSource VSAQC Error in extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

hAperMag4Err vhsSource VSAVHS Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

hAperMag4Err vhsSource, vikingSource VSAQC Error in point/extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

hAperMag6 svNgc253Source VSASVNGC253 Extended source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

hAperMag6 svOrionSource VSASVORION Extended source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

hAperMag6 ultravistaSource VSAUltraVISTA Extended source H mag, no aperture correction applied real 4 mag -0.9999995e9 PHOT_MAG

hAperMag6 ultravistaSource, videoSource VSAQC Extended source H mag, no aperture correction applied real 4 mag -0.9999995e9 PHOT_MAG

hAperMag6 vhsSource VSAVHS Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

hAperMag6 vhsSource, vikingSource VSAQC Point source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

hAperMag6Err svNgc253Source VSASVNGC253 Error in extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

hAperMag6Err svOrionSource VSASVORION Error in extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

hAperMag6Err ultravistaSource VSAUltraVISTA Error in extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

hAperMag6Err ultravistaSource, videoSource VSAQC Error in extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

hAperMag6Err vhsSource VSAVHS Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

hAperMag6Err vhsSource, vikingSource VSAQC Error in point/extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

hAperMagNoAperCorr3 vhsSource VSAVHS Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

hAperMagNoAperCorr3 vhsSource, vikingSource VSAQC Default extended source H aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

hAperMagNoAperCorr4 vhsSource VSAVHS Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

hAperMagNoAperCorr4 vhsSource, vikingSource VSAQC Extended source H aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

hAperMagNoAperCorr6 vhsSource VSAVHS Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

hAperMagNoAperCorr6 vhsSource, vikingSource VSAQC Extended source H aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

haStratAst videoVarFrameSetInfo VSAVIDEO Strateva parameter, a, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

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

haStratAst videoVarFrameSetInfo, vikingVarFrameSetInfo, vvvVarFrameSetInfo VSAQC Strateva parameter, a, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

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

haStratPht videoVarFrameSetInfo VSAVIDEO Strateva parameter, a, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

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

haStratPht videoVarFrameSetInfo, vikingVarFrameSetInfo, vvvVarFrameSetInfo VSAQC Strateva parameter, a, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

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

hAverageConf svNgc253Source VSASVNGC253 average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -99999999 CODE_MISC

hAverageConf svOrionSource VSASVORION average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -99999999 CODE_MISC

hAverageConf vhsSource VSAVHS average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -99999999 CODE_MISC

hAverageConf vhsSource, vikingSource VSAQC average confidence in 2 arcsec diameter default aperture (aper3) H real 4 -99999999 CODE_MISC

hbestAper videoVariability VSAVIDEO Best aperture (1-6) for photometric statistics in the H band int 4 -9999

Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)

hbestAper videoVariability, vikingVariability, vvvVariability VSAQC Best aperture (1-6) for photometric statistics in the H band int 4 -9999

Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)

hbStratAst videoVarFrameSetInfo VSAVIDEO Strateva parameter, b, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

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

hbStratAst videoVarFrameSetInfo, vikingVarFrameSetInfo, vvvVarFrameSetInfo VSAQC Strateva parameter, b, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

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

hbStratPht videoVarFrameSetInfo VSAVIDEO Strateva parameter, b, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

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

hbStratPht videoVarFrameSetInfo, vikingVarFrameSetInfo, vvvVarFrameSetInfo VSAQC Strateva parameter, b, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

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

hchiSqAst videoVarFrameSetInfo VSAVIDEO Goodness of fit of Strateva function to astrometric data in H band real 4 -0.9999995e9

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

hchiSqAst videoVarFrameSetInfo, vikingVarFrameSetInfo, vvvVarFrameSetInfo VSAQC Goodness of fit of Strateva function to astrometric data in H band real 4 -0.9999995e9

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

hchiSqpd videoVariability VSAVIDEO Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9

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

hchiSqpd videoVariability, vikingVariability, vvvVariability VSAQC Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9

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

hchiSqPht videoVarFrameSetInfo VSAVIDEO Goodness of fit of Strateva function to photometric data in H band real 4 -0.9999995e9

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

hchiSqPht videoVarFrameSetInfo, vikingVarFrameSetInfo, vvvVarFrameSetInfo VSAQC Goodness of fit of Strateva function to photometric data in H band real 4 -0.9999995e9

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

hClass svNgc253Source VSASVNGC253 discrete image classification flag in H smallint 2 -9999 CLASS_MISC

hClass svOrionSource VSASVORION discrete image classification flag in H smallint 2 -9999 CLASS_MISC

hClass ultravistaSource VSAUltraVISTA discrete image classification flag in H smallint 2 -9999 CLASS_MISC

hClass ultravistaSource, ultravistaSourceRemeasurement, vhsSource, vhsSourceRemeasurement, videoSource, videoSourceRemeasurement, vikingSource, vikingSourceRemeasurement, vvvSource, vvvSourceRemeasurement VSAQC discrete image classification flag in H smallint 2 -9999 CLASS_MISC

hClassStat svNgc253Source VSASVNGC253 N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 STAT_PROP

hClassStat svOrionSource VSASVORION N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 STAT_PROP

hClassStat ultravistaSource VSAUltraVISTA S-Extractor classification statistic in H real 4 -0.9999995e9 STAT_PROP

hClassStat ultravistaSource, videoSource, vvvSource VSAQC S-Extractor classification statistic in H real 4 -0.9999995e9 STAT_PROP

hClassStat ultravistaSourceRemeasurement VSAUltraVISTA N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 STAT_PROP

hClassStat ultravistaSourceRemeasurement, vhsSource, vhsSourceRemeasurement, videoSourceRemeasurement, vikingSource, vikingSourceRemeasurement, vvvSourceRemeasurement VSAQC N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 STAT_PROP

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

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

hcStratAst videoVarFrameSetInfo, vikingVarFrameSetInfo, vvvVarFrameSetInfo VSAQC Strateva parameter, c, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

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

hcStratPht videoVarFrameSetInfo VSAVIDEO Strateva parameter, c, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

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

hcStratPht videoVarFrameSetInfo, vikingVarFrameSetInfo, vvvVarFrameSetInfo VSAQC Strateva parameter, c, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

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

hDeblend ultravistaSource VSAUltraVISTA placeholder flag indicating parent/child relation in H int 4 -99999999 CODE_MISC

hDeblend ultravistaSource, ultravistaSourceRemeasurement, vhsSourceRemeasurement, videoSource, videoSourceRemeasurement, vikingSourceRemeasurement, vvvSource, vvvSourceRemeasurement VSAQC placeholder flag indicating parent/child relation in H int 4 -99999999 CODE_MISC

hEll svNgc253Source VSASVNGC253 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 PHYS_ELLIPTICITY

hEll svOrionSource VSASVORION 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 PHYS_ELLIPTICITY

hEll ultravistaSource VSAUltraVISTA 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 PHYS_ELLIPTICITY

hEll ultravistaSource, ultravistaSourceRemeasurement, vhsSource, vhsSourceRemeasurement, videoSource, videoSourceRemeasurement, vikingSource, vikingSourceRemeasurement, vvvSource, vvvSourceRemeasurement VSAQC 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 PHYS_ELLIPTICITY

hemis twomass_psc 2MASS Hemisphere code for the TWOMASS Observatory from which this source was observed. varchar 1 OBS_CODE

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

hemis twomass_sixx2_scn 2MASS hemisphere (N/S) of observation varchar 1

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

heNum svNgc253MergeLog VSASVNGC253 the extension number of this H frame tinyint 1 NUMBER

heNum svOrionMergeLog VSASVORION the extension number of this H frame tinyint 1 NUMBER

heNum ultravistaMergeLog VSAUltraVISTA the extension number of this H frame tinyint 1 NUMBER

heNum ultravistaMergeLog, vhsMergeLog, videoMergeLog, vikingMergeLog, vvvMergeLog VSAQC the extension number of this H frame tinyint 1 NUMBER

hErrBits svNgc253Source VSASVNGC253 processing warning/error bitwise flags in H int 4 -99999999 CODE_MISC

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits svOrionSource VSASVORION processing warning/error bitwise flags in H int 4 -99999999 CODE_MISC

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits ultravistaSource VSAUltraVISTA processing warning/error bitwise flags in H int 4 -99999999 CODE_MISC

This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows:

Bit Flag Meaning

1 The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected).

2 The object was originally blended with another

4 At least one pixel is saturated (or very close to)

8 The object is truncated (too close to an image boundary)

16 Object's aperture data are incomplete or corrupted

32 Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters.

64 Memory overflow occurred during deblending

128 Memory overflow occurred during extraction

hErrBits ultravistaSource, videoSource VSAQC processing warning/error bitwise flags in H int 4 -99999999 CODE_MISC

This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows:

Bit Flag Meaning

1 The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected).

2 The object was originally blended with another

4 At least one pixel is saturated (or very close to)

8 The object is truncated (too close to an image boundary)

16 Object's aperture data are incomplete or corrupted

32 Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters.

64 Memory overflow occurred during deblending

128 Memory overflow occurred during extraction

hErrBits ultravistaSourceRemeasurement VSAUltraVISTA processing warning/error bitwise flags in H int 4 -99999999 CODE_MISC

hErrBits ultravistaSourceRemeasurement, vhsSourceRemeasurement, videoSourceRemeasurement, vikingSourceRemeasurement, vvvSourceRemeasurement VSAQC processing warning/error bitwise flags in H int 4 -99999999 CODE_MISC

hErrBits vhsSource VSAVHS processing warning/error bitwise flags in H int 4 -99999999 CODE_MISC

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hErrBits vhsSource, vikingSource, vvvSource VSAQC processing warning/error bitwise flags in H int 4 -99999999 CODE_MISC

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

hEta svNgc253Source VSASVNGC253 Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 POS_EQ_DEC_OFF

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.

hEta svOrionSource VSASVORION Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 POS_EQ_DEC_OFF

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.

hEta ultravistaSource VSAUltraVISTA Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 POS_EQ_DEC_OFF

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.

hEta ultravistaSource, vhsSource, videoSource, vikingSource, vvvSource VSAQC Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 POS_EQ_DEC_OFF

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.

hexpML videoVarFrameSetInfo VSAVIDEO Expected magnitude limit of frameSet in this in H band. real 4 -0.9999995e9

hexpML videoVarFrameSetInfo, vikingVarFrameSetInfo, vvvVarFrameSetInfo VSAQC Expected magnitude limit of frameSet in this in H band. real 4 -0.9999995e9

hExpRms videoVariability VSAVIDEO Rms calculated from polynomial fit to modal RMS as a function of magnitude in H band real 4 mag -0.9999995e9

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

hExpRms videoVariability, vikingVariability, vvvVariability VSAQC Rms calculated from polynomial fit to modal RMS as a function of magnitude in H band real 4 mag -0.9999995e9

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

hGausig svNgc253Source VSASVNGC253 RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 MORPH_PARAM

hGausig svOrionSource VSASVORION RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 MORPH_PARAM

hGausig ultravistaSource VSAUltraVISTA RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 MORPH_PARAM

hGausig ultravistaSource, ultravistaSourceRemeasurement, vhsSource, vhsSourceRemeasurement, videoSource, videoSourceRemeasurement, vikingSource, vikingSourceRemeasurement, vvvSource, vvvSourceRemeasurement VSAQC RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 MORPH_PARAM

hgl twomass_scn 2MASS Special flag indicating whether or not this scan has a single-frame H-band electronic glitch. smallint 2 CODE_MISC

hgl twomass_sixx2_scn 2MASS single-frame H-band glitch flag (0:not found|1:found) smallint 2

hHlCorSMjRadAs svNgc253Source VSASVNGC253 Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 EXTENSION_RAD

hHlCorSMjRadAs ultravistaSource VSAUltraVISTA Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 EXTENSION_RAD

hHlCorSMjRadAs ultravistaSource, vhsSource, videoSource, vikingSource VSAQC Seeing corrected half-light, semi-major axis in H band real 4 arcsec -0.9999995e9 EXTENSION_RAD

hIntRms videoVariability VSAVIDEO Intrinsic rms in H-band real 4 mag -0.9999995e9

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

hIntRms videoVariability, vikingVariability, vvvVariability VSAQC Intrinsic rms in H-band real 4 mag -0.9999995e9

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

hlCircRadAs svNgc253Detection VSASVNGC253 Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 EXTENSION_RAD

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition 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 svOrionDetection VSASVORION Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 EXTENSION_RAD

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition 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 ultravistaDetection VSAUltraVISTA Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 EXTENSION_RAD

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition 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 ultravistaDetection, vhsDetection, videoDetection, vikingDetection VSAQC Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total real 4 arcsec -0.9999995e9 EXTENSION_RAD

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition 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 ultravistaListRemeasurement VSAUltraVISTA Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total flux real 4 arcsec -0.9999995e9 EXTENSION_RAD

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition 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 ultravistaListRemeasurement, vhsListRemeasurement, videoListRemeasurement, vikingListRemeasurement VSAQC Circular half-light radius computed from curve of growth assuming petrosian flux is 90% of total flux real 4 arcsec -0.9999995e9 EXTENSION_RAD

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition 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 svNgc253Detection VSASVNGC253 Error in hlCircRadAs real 4 arcsec -0.9999995e9 EXTENSION_RAD

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition 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 svOrionDetection VSASVORION Error in hlCircRadAs real 4 arcsec -0.9999995e9 EXTENSION_RAD

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition 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 ultravistaDetection VSAUltraVISTA Error in hlCircRadAs real 4 arcsec -0.9999995e9 EXTENSION_RAD

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition 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 ultravistaDetection, ultravistaListRemeasurement, vhsDetection, vhsListRemeasurement, videoDetection, videoListRemeasurement, vikingDetection, vikingListRemeasurement VSAQC Error in hlCircRadAs real 4 arcsec -0.9999995e9 EXTENSION_RAD

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition 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 svNgc253Detection VSASVNGC253 Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9

hlCorSMjRadAs svOrionDetection VSASVORION Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9

hlCorSMjRadAs ultravistaDetection VSAUltraVISTA Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9

hlCorSMjRadAs ultravistaDetection, vhsDetection, videoDetection, vikingDetection VSAQC Seeing corrected Half-light semi-major axis real 4 arcsec -0.9999995e9

hlCorSMjRadAs ultravistaListRemeasurement VSAUltraVISTA Seeing corrected 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.

hlCorSMjRadAs ultravistaListRemeasurement, vhsListRemeasurement, videoListRemeasurement, vikingListRemeasurement VSAQC Seeing corrected 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.

hlCorSMnRadAs svNgc253Detection VSASVNGC253 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 svOrionDetection VSASVORION 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 ultravistaDetection VSAUltraVISTA 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 ultravistaDetection, ultravistaListRemeasurement, vhsDetection, vhsListRemeasurement, videoDetection, videoListRemeasurement, vikingDetection, vikingListRemeasurement VSAQC 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 svNgc253Detection VSASVNGC253 Geometric half-light radius real 4 arcsec -0.9999995e9 EXTENSION_RAD

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition 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 svOrionDetection VSASVORION Geometric half-light radius real 4 arcsec -0.9999995e9 EXTENSION_RAD

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition 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 ultravistaDetection VSAUltraVISTA Geometric half-light radius real 4 arcsec -0.9999995e9 EXTENSION_RAD

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition 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 ultravistaDetection, ultravistaListRemeasurement, vhsDetection, vhsListRemeasurement, videoDetection, videoListRemeasurement, vikingDetection, vikingListRemeasurement VSAQC Geometric half-light radius real 4 arcsec -0.9999995e9 EXTENSION_RAD

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition 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 svNgc253Detection VSASVNGC253 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 svOrionDetection VSASVORION 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 ultravistaDetection VSAUltraVISTA 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 ultravistaDetection, ultravistaListRemeasurement, vhsDetection, vhsListRemeasurement, videoDetection, videoListRemeasurement, vikingDetection, vikingListRemeasurement VSAQC 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 svNgc253Detection VSASVNGC253 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 svOrionDetection VSASVORION 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 ultravistaDetection VSAUltraVISTA 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 ultravistaDetection, ultravistaListRemeasurement, vhsDetection, vhsListRemeasurement, videoDetection, videoListRemeasurement, vikingDetection, vikingListRemeasurement VSAQC 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 mcps_lmcSource, mcps_smcSource MCPS The H band magnitude (from 2MASS) (0.00 if star not detected.) real 4 mag

hMag ukirtFSstars VSASVNGC253 H band total magnitude on the MKO(UFTI) system real 4 mag PHOT_INT-MAG

hMag ukirtFSstars VSASVORION H band total magnitude on the MKO(UFTI) system real 4 mag PHOT_INT-MAG

hMag ukirtFSstars VSAUltraVISTA H band total magnitude on the MKO(UFTI) system real 4 mag PHOT_INT-MAG

hMag ukirtFSstars VSAVHS H band total magnitude on the MKO(UFTI) system real 4 mag PHOT_INT-MAG

hMag ukirtFSstars VSAVIDEO H band total magnitude on the MKO(UFTI) system real 4 mag PHOT_INT-MAG

hMag ukirtFSstars VSAVIKING H band total magnitude on the MKO(UFTI) system real 4 mag PHOT_INT-MAG

hMag ukirtFSstars VSAVMC H band total magnitude on the MKO(UFTI) system real 4 mag PHOT_INT-MAG

hMag ukirtFSstars VSAVVV H band total magnitude on the MKO(UFTI) system real 4 mag PHOT_INT-MAG

hMag ultravistaSourceRemeasurement VSAUltraVISTA H mag (as appropriate for this merged source) real 4 mag -0.9999995e9 PHOT_MAG

hMag ultravistaSourceRemeasurement, vhsSourceRemeasurement, videoSourceRemeasurement, vikingSourceRemeasurement, vvvSourceRemeasurement VSAQC H mag (as appropriate for this merged source) real 4 mag -0.9999995e9 PHOT_MAG

Hmag2MASS spitzer_smcSource SPITZER The 2MASS H band magnitude. real 4 mag

hMagErr ukirtFSstars VSASVNGC253 H band magnitude error real 4 mag ERROR

hMagErr ukirtFSstars VSASVORION H band magnitude error real 4 mag ERROR

hMagErr ukirtFSstars VSAUltraVISTA H band magnitude error real 4 mag ERROR

hMagErr ukirtFSstars VSAVHS H band magnitude error real 4 mag ERROR

hMagErr ukirtFSstars VSAVIDEO H band magnitude error real 4 mag ERROR

hMagErr ukirtFSstars VSAVIKING H band magnitude error real 4 mag ERROR

hMagErr ukirtFSstars VSAVMC H band magnitude error real 4 mag ERROR

hMagErr ukirtFSstars VSAVVV H band magnitude error real 4 mag ERROR

hMagErr ultravistaSourceRemeasurement VSAUltraVISTA Error in H mag real 4 mag -0.9999995e9 ERROR

hMagErr ultravistaSourceRemeasurement, vhsSourceRemeasurement, videoSourceRemeasurement, vikingSourceRemeasurement, vvvSourceRemeasurement VSAQC Error in H mag real 4 mag -0.9999995e9 ERROR

hMagMAD videoVariability VSAVIDEO Median Absolute Deviation of H magnitude real 4 mag -0.9999995e9

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

hMagMAD videoVariability, vikingVariability, vvvVariability VSAQC Median Absolute Deviation of H magnitude real 4 mag -0.9999995e9

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

hMagRms videoVariability VSAVIDEO rms of H magnitude real 4 mag -0.9999995e9

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

hMagRms videoVariability, vikingVariability, vvvVariability VSAQC rms of H magnitude real 4 mag -0.9999995e9

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

hmaxCadence videoVariability VSAVIDEO maximum gap between observations real 4 days -0.9999995e9

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

hmaxCadence videoVariability, vikingVariability, vvvVariability VSAQC maximum gap between observations real 4 days -0.9999995e9

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

hMaxMag videoVariability VSAVIDEO Maximum magnitude in H band, of good detections real 4 -0.9999995e9

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

hMaxMag videoVariability, vikingVariability, vvvVariability VSAQC Maximum magnitude in H band, of good detections real 4 -0.9999995e9

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

hmeanMag videoVariability VSAVIDEO Mean H magnitude real 4 mag -0.9999995e9

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

hmeanMag videoVariability, vikingVariability, vvvVariability VSAQC Mean H magnitude real 4 mag -0.9999995e9

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

hmedCadence videoVariability VSAVIDEO median gap between observations real 4 days -0.9999995e9

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

hmedCadence videoVariability, vikingVariability, vvvVariability VSAQC median gap between observations real 4 days -0.9999995e9

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

hmedianMag videoVariability VSAVIDEO Median H magnitude real 4 mag -0.9999995e9

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

hmedianMag videoVariability, vikingVariability, vvvVariability VSAQC Median H magnitude real 4 mag -0.9999995e9

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

hmfID svNgc253MergeLog VSASVNGC253 the UID of the relevant H multiframe bigint 8 ID_FRAME

hmfID svOrionMergeLog VSASVORION the UID of the relevant H multiframe bigint 8 ID_FRAME

hmfID ultravistaMergeLog VSAUltraVISTA the UID of the relevant H multiframe bigint 8 ID_FRAME

hmfID ultravistaMergeLog, vhsMergeLog, videoMergeLog, vikingMergeLog, vvvMergeLog VSAQC the UID of the relevant H multiframe bigint 8 ID_FRAME

hminCadence videoVariability VSAVIDEO minimum gap between observations real 4 days -0.9999995e9

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

hminCadence videoVariability, vikingVariability, vvvVariability VSAQC minimum gap between observations real 4 days -0.9999995e9

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

hMinMag videoVariability VSAVIDEO Minimum magnitude in H band, of good detections real 4 -0.9999995e9

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

hMinMag videoVariability, vikingVariability, vvvVariability VSAQC Minimum magnitude in H band, of good detections real 4 -0.9999995e9

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

hmks ultravistaSourceRemeasurement VSAUltraVISTA Default colour H-Ks (using appropriate mags) real 4 mag PHOT_COLOR

hmks ultravistaSourceRemeasurement, vhsSourceRemeasurement, videoSourceRemeasurement, vikingSourceRemeasurement, vvvSourceRemeasurement VSAQC Default colour H-Ks (using appropriate mags) real 4 mag PHOT_COLOR

hmksErr ultravistaSourceRemeasurement VSAUltraVISTA Error on colour H-Ks real 4 mag ERROR

hmksErr ultravistaSourceRemeasurement, vhsSourceRemeasurement, videoSourceRemeasurement, vikingSourceRemeasurement, vvvSourceRemeasurement VSAQC Error on colour H-Ks real 4 mag ERROR

hmksExt svNgc253Source VSASVNGC253 Extended source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt svOrionSource VSASVORION Extended source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt ultravistaSource VSAUltraVISTA Extended source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt ultravistaSource, videoSource, vvvSource VSAQC Extended source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt vhsSource VSAVHS Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExt vhsSource, vikingSource VSAQC Extended source colour H-Ks (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr svNgc253Source VSASVNGC253 Error on extended source colour H-Ks real 4 mag -0.9999995e9 ERROR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr svOrionSource VSASVORION Error on extended source colour H-Ks real 4 mag -0.9999995e9 ERROR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr ultravistaSource VSAUltraVISTA Error on extended source colour H-Ks real 4 mag -0.9999995e9 ERROR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksExtErr ultravistaSource, vhsSource, videoSource, vikingSource, vvvSource VSAQC Error on extended source colour H-Ks real 4 mag -0.9999995e9 ERROR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt svNgc253Source VSASVNGC253 Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt svOrionSource VSASVORION Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt ultravistaSource VSAUltraVISTA Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPnt ultravistaSource, vhsSource, videoSource, vikingSource, vvvSource VSAQC Point source colour H-Ks (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr svNgc253Source VSASVNGC253 Error on point source colour H-Ks real 4 mag -0.9999995e9 ERROR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr svOrionSource VSASVORION Error on point source colour H-Ks real 4 mag -0.9999995e9 ERROR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr ultravistaSource VSAUltraVISTA Error on point source colour H-Ks real 4 mag -0.9999995e9 ERROR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmksPntErr ultravistaSource, vhsSource, videoSource, vikingSource, vvvSource VSAQC Error on point source colour H-Ks real 4 mag -0.9999995e9 ERROR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hndof videoVariability VSAVIDEO Number of degrees of freedom for chisquare smallint 2 -9999

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

hndof videoVariability, vikingVariability, vvvVariability VSAQC Number of degrees of freedom for chisquare smallint 2 -9999

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

hnDofAst videoVarFrameSetInfo VSAVIDEO Number of degrees of freedom of astrometric fit in H band. smallint 2 -9999

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

hnDofAst videoVarFrameSetInfo, vikingVarFrameSetInfo, vvvVarFrameSetInfo VSAQC Number of degrees of freedom of astrometric fit in H band. smallint 2 -9999

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

hnDofPht videoVarFrameSetInfo VSAVIDEO Number of degrees of freedom of photometric fit in H band. smallint 2 -9999

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

hnDofPht videoVarFrameSetInfo, vikingVarFrameSetInfo, vvvVarFrameSetInfo VSAQC Number of degrees of freedom of photometric fit in H band. smallint 2 -9999

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

hnFlaggedObs videoVariability VSAQC Number of detections in H band flagged as potentially spurious by videoDetection.ppErrBits int 4 0

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

hnFlaggedObs videoVariability VSAVIDEO Number of detections in H band flagged as potentially spurious by videoDetection.ppErrBits int 4 0

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

hnFlaggedObs vikingVariability VSAQC Number of detections in H band flagged as potentially spurious by vikingDetection.ppErrBits int 4 0

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

hnFlaggedObs vikingVariability VSAVIKING Number of detections in H band flagged as potentially spurious by vikingDetection.ppErrBits int 4 0

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

hnFlaggedObs vvvVariability VSAQC Number of detections in H band flagged as potentially spurious by vvvDetection.ppErrBits int 4 0

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

hnFlaggedObs vvvVariability VSAVVV Number of detections in H band flagged as potentially spurious by vvvDetection.ppErrBits int 4 0

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

hnGoodObs videoVariability VSAVIDEO Number of good detections in H band int 4 0

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

hnGoodObs videoVariability, vikingVariability, vvvVariability VSAQC Number of good detections in H band int 4 0

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

hNgt3sig videoVariability VSAVIDEO Number of good detections in H-band that are more than 3 sigma deviations smallint 2 -9999

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

hNgt3sig videoVariability, vikingVariability, vvvVariability VSAQC Number of good detections in H-band that are more than 3 sigma deviations smallint 2 -9999

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

hnMissingObs videoVariability VSAVIDEO Number of H band frames that this object should have been detected on and was not int 4 0

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

hnMissingObs videoVariability, vikingVariability, vvvVariability VSAQC Number of H band frames that this object should have been detected on and was not int 4 0

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

hPA svNgc253Source VSASVNGC253 ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 POS_POS-ANG

hPA svOrionSource VSASVORION ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 POS_POS-ANG

hPA ultravistaSource VSAUltraVISTA ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 POS_POS-ANG

hPA ultravistaSource, ultravistaSourceRemeasurement, vhsSource, vhsSourceRemeasurement, videoSource, videoSourceRemeasurement, vikingSource, vikingSourceRemeasurement, vvvSource, vvvSourceRemeasurement VSAQC ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 POS_POS-ANG

hPetroMag svNgc253Source VSASVNGC253 Extended source H mag (Petrosian) real 4 mag -0.9999995e9 PHOT_MAG

hPetroMag svOrionSource VSASVORION Extended source H mag (Petrosian) real 4 mag -0.9999995e9 PHOT_MAG

hPetroMag ultravistaSource VSAUltraVISTA Extended source H mag (Petrosian) real 4 mag -0.9999995e9 PHOT_MAG

hPetroMag ultravistaSource, vhsSource, videoSource, vikingSource VSAQC Extended source H mag (Petrosian) real 4 mag -0.9999995e9 PHOT_MAG

hPetroMagErr svNgc253Source VSASVNGC253 Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 ERROR

hPetroMagErr svOrionSource VSASVORION Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 ERROR

hPetroMagErr ultravistaSource VSAUltraVISTA Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 ERROR

hPetroMagErr ultravistaSource, vhsSource, videoSource, vikingSource VSAQC Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 ERROR

hppErrBits svNgc253Source VSASVNGC253 additional WFAU post-processing error bits in H int 4 0 CODE_MISC

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

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

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.

hppErrBits svOrionSource VSASVORION additional WFAU post-processing error bits in H int 4 0 CODE_MISC

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

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

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.

hppErrBits ultravistaSource VSAUltraVISTA additional WFAU post-processing error bits in H int 4 0 CODE_MISC

hppErrBits ultravistaSource, ultravistaSourceRemeasurement, vhsSourceRemeasurement, videoSource, videoSourceRemeasurement, vikingSourceRemeasurement, vvvSource, vvvSourceRemeasurement VSAQC additional WFAU post-processing error bits in H int 4 0 CODE_MISC

hppErrBits vhsSource VSAVHS additional WFAU post-processing error bits in H int 4 0 CODE_MISC

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

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

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.

hppErrBits vhsSource, vikingSource VSAQC additional WFAU post-processing error bits in H int 4 0 CODE_MISC

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

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

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.

hprobVar videoVariability VSAVIDEO Probability of variable from chi-square (and other data) real 4 -0.9999995e9

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

hprobVar videoVariability, vikingVariability, vvvVariability VSAQC Probability of variable from chi-square (and other data) real 4 -0.9999995e9

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

hPsfMag svNgc253Source VSASVNGC253 Point source profile-fitted H mag real 4 mag -0.9999995e9 PHOT_MAG

hPsfMag svOrionSource VSASVORION Point source profile-fitted H mag real 4 mag -0.9999995e9 PHOT_MAG

hPsfMag ultravistaSource VSAUltraVISTA Not available in SE output real 4 mag -0.9999995e9 PHOT_MAG

hPsfMag ultravistaSource, videoSource VSAQC Not available in SE output real 4 mag -0.9999995e9 PHOT_MAG

hPsfMag vhsSource VSAVHS Point source profile-fitted H mag real 4 mag -0.9999995e9 PHOT_MAG

hPsfMag vhsSource, vikingSource VSAQC Point source profile-fitted H mag real 4 mag -0.9999995e9 PHOT_MAG

hPsfMagErr svNgc253Source VSASVNGC253 Error in point source profile-fitted H mag real 4 mag -0.9999995e9 ERROR

hPsfMagErr svOrionSource VSASVORION Error in point source profile-fitted H mag real 4 mag -0.9999995e9 ERROR

hPsfMagErr ultravistaSource VSAUltraVISTA Not available in SE output real 4 mag -0.9999995e9 ERROR

hPsfMagErr ultravistaSource, videoSource VSAQC Not available in SE output real 4 mag -0.9999995e9 ERROR

hPsfMagErr vhsSource VSAVHS Error in point source profile-fitted H mag real 4 mag -0.9999995e9 ERROR

hPsfMagErr vhsSource, vikingSource VSAQC Error in point source profile-fitted H mag real 4 mag -0.9999995e9 ERROR

hr1 rosat_bsc, rosat_fsc ROSAT hardness ratio 1 float 8 SPECT_HARDNESS-RATIO

hr2 rosat_bsc, rosat_fsc ROSAT hardness ratio 2 float 8 SPECT_HARDNESS-RATIO

hry twomass_scn 2MASS Flag indicating the H-band array configuration for the camera. smallint 2 CODE_MISC

hry twomass_sixx2_scn 2MASS 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 REMARKS

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

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

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

hSeqNum svNgc253Source VSASVNGC253 the running number of the H detection int 4 -99999999 ID_NUMBER

hSeqNum svOrionSource VSASVORION the running number of the H detection int 4 -99999999 ID_NUMBER

hSeqNum ultravistaSource VSAUltraVISTA the running number of the H detection int 4 -99999999 ID_NUMBER

hSeqNum ultravistaSource, vhsSource, videoSource, vikingSource, vvvSource VSAQC the running number of the H detection int 4 -99999999 ID_NUMBER

hSeqNum ultravistaSourceRemeasurement VSAUltraVISTA the running number of the H remeasurement int 4 -99999999 ID_NUMBER

hSeqNum ultravistaSourceRemeasurement, vhsSourceRemeasurement, videoSourceRemeasurement, vikingSourceRemeasurement, vvvSourceRemeasurement VSAQC the running number of the H remeasurement int 4 -99999999 ID_NUMBER

hSerMag2D svNgc253Source VSASVNGC253 Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 PHOT_MAG

hSerMag2D svOrionSource VSASVORION Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 PHOT_MAG

hSerMag2D ultravistaSource VSAUltraVISTA Not available in SE output real 4 mag -0.9999995e9 PHOT_MAG

hSerMag2D ultravistaSource, videoSource VSAQC Not available in SE output real 4 mag -0.9999995e9 PHOT_MAG

hSerMag2D vhsSource VSAVHS Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 PHOT_MAG

hSerMag2D vhsSource, vikingSource VSAQC Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 PHOT_MAG

hSerMag2DErr svNgc253Source VSASVNGC253 Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 ERROR

hSerMag2DErr svOrionSource VSASVORION Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 ERROR

hSerMag2DErr ultravistaSource VSAUltraVISTA Not available in SE output real 4 mag -0.9999995e9 ERROR

hSerMag2DErr ultravistaSource, videoSource VSAQC Not available in SE output real 4 mag -0.9999995e9 ERROR

hSerMag2DErr vhsSource VSAVHS Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 ERROR

hSerMag2DErr vhsSource, vikingSource VSAQC Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 ERROR

hskewness videoVariability VSAVIDEO Skewness in H band (see Sesar et al. 2007) real 4 -0.9999995e9

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

hskewness videoVariability, vikingVariability, vvvVariability VSAQC Skewness in H band (see Sesar et al. 2007) real 4 -0.9999995e9

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

HTMID spectra SIXDF Hierarchical Triangular Mesh (20-deep), mainly useful internally for indexing on position bigint 8

HTMID target SIXDF Hierarchical Triangular Mesh (20-deep) number, mainly useful internally for indexing on position bigint 8

HTMID twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 POS_GENERAL

htmID CurrentAstrometry VSASVNGC253 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 POS_GENERAL

htmID CurrentAstrometry VSASVORION Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 POS_GENERAL

htmID CurrentAstrometry VSAUltraVISTA Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 POS_GENERAL

htmID CurrentAstrometry VSAVHS Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 POS_GENERAL

htmID CurrentAstrometry VSAVIDEO Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 POS_GENERAL

htmID CurrentAstrometry VSAVIKING Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 POS_GENERAL

htmID CurrentAstrometry VSAVMC Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 POS_GENERAL

htmID CurrentAstrometry VSAVVV Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 POS_GENERAL

htmID combo17CDFSSource COMBO17 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 POS_GENERAL

htmID first08Jul16Source, firstSource FIRST Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 POS_GENERAL

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_GENERAL

htmID grs_ngpSource, grs_ranSource, grs_sgpSource TWODFGRS Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 POS_GENERAL

htmID iras_psc IRAS Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 POS_GENERAL

htmID machoLMCSource, machoSMCSource MACHO Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 POS_GENERAL

htmID mcps_lmcSource, mcps_smcSource MCPS Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 POS_GENERAL

htmID mgcDetection MGC Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 POS_GENERAL

htmID nvssSource NVSS 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_GENERAL

htmID sage_lmcIracSource, sage_lmcMips160Source, sage_lmcMips24Source, sage_lmcMips70Source SPITZER 20-deep hierachical triangular mesh ID of this source bigint 8

htmID spitzer_smcSource SPITZER Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 POS_GENERAL

htmID svNgc253Detection, svNgc253MergeLog, svNgc253Source VSASVNGC253 Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 POS_GENERAL

htmID svOrionDetection, svOrionMergeLog, svOrionSource VSASVORION Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 POS_GENERAL

htmID twomass_psc, twomass_scn, twomass_sixx2_psc, twomass_sixx2_scn, twomass_sixx2_xsc, twomass_xsc 2MASS Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 POS_GENERAL

htmID ultravistaCurrentAstrometry, vhsCurrentAstrometry, videoCurrentAstrometry, vikingCurrentAstrometry, vmcCurrentAstrometry, vvvCurrentAstrometry VSAQC Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 POS_GENERAL

htmID ultravistaDetection VSAUltraVISTA Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 POS_GENERAL

htmID ultravistaDetection, ultravistaListRemeasurement, ultravistaMergeLog, ultravistaSource, ultravistaSourceRemeasurement, vhsDetection, vhsListRemeasurement, vhsMergeLog, vhsSource, vhsSourceRemeasurement, vhsTileDetections, vhsTileSet, videoDetection, videoListRemeasurement, videoMergeLog, videoSource, videoSourceRemeasurement, vikingDetection, vikingListRemeasurement, vikingMergeLog, vikingSource, vikingSourceRemeasurement, vmcDetection, vmcListRemeasurement, vmcMergeLog, vmcSource, vmcSourceRemeasurement, vmcSynopticMergeLog, vmcSynopticSource, vvvDetection, vvvListRemeasurement, vvvMergeLog, vvvSource, vvvSourceRemeasurement VSAQC Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 POS_GENERAL

htotalPeriod videoVariability VSAVIDEO total period of observations (last obs-first obs) real 4 days -0.9999995e9

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

htotalPeriod videoVariability, vikingVariability, vvvVariability VSAQC total period of observations (last obs-first obs) real 4 days -0.9999995e9

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

hVarClass videoVariability VSAVIDEO Classification of variability in this band smallint 2 -9999

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

hVarClass videoVariability, vikingVariability, vvvVariability VSAQC Classification of variability in this band smallint 2 -9999

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

hXi svNgc253Source VSASVNGC253 Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 POS_EQ_RA_OFF

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.

hXi svOrionSource VSASVORION Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 POS_EQ_RA_OFF

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.

hXi ultravistaSource VSAUltraVISTA Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 POS_EQ_RA_OFF

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.

hXi ultravistaSource, vhsSource, videoSource, vikingSource, vvvSource VSAQC Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 POS_EQ_RA_OFF

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.

WFAU, Institute for Astronomy,
Royal Observatory, Blackford Hill
Edinburgh, EH9 3HJ, UK
Tel +44 131 668 8356 (office)
or +44 131 668 8100 (switchboard)

vsa-support@roe.ac.uk
21/02/2011