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

J

Name Schema Table Database Description Type Length Unit Default Value Unified Content Descriptor

J twomass SIXDF J magnitude (JEXT) used for J selection real 4 mag

j_2mrat twomass_scn 2MASS J-band average 2nd image moment ratio. real 4 FIT_PARAM_VALUE

j_2mrat twomass_sixx2_scn 2MASS J band average 2nd image moment ratio for scan real 4

j_5sig_ba twomass_xsc 2MASS J minor/major axis ratio fit to the 5-sigma isophote. real 4 PHYS_AXIS-RATIO

j_5sig_phi twomass_xsc 2MASS J angle to 5-sigma major axis (E of N). smallint 2 degrees ERROR

j_5surf twomass_xsc 2MASS J central surface brightness (r<=5). real 4 mag PHOT_SB_GENERAL

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

j_back twomass_xsc 2MASS J coadd median background. real 4 CODE_MISC

j_bisym_chi twomass_xsc 2MASS J bi-symmetric cross-correlation chi. real 4 FIT_PARAM_VALUE

j_bisym_rat twomass_xsc 2MASS J bi-symmetric flux ratio. real 4 PHOT_FLUX_RATIO

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

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

j_chif_ellf twomass_xsc 2MASS J % chi-fraction for elliptical fit to 3-sig isophote. real 4 FIT_PARAM_VALUE

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

j_con_indx twomass_xsc 2MASS J concentration index r_75%/r_25%. real 4 PHYS_CONCENT_INDEX

j_d_area twomass_xsc 2MASS J 5-sigma to 3-sigma differential area. smallint 2 FIT_RESIDUAL

j_flg_10 twomass_xsc 2MASS J confusion flag for 10 arcsec circular ap. mag. smallint 2 CODE_MISC

j_flg_15 twomass_xsc 2MASS J confusion flag for 15 arcsec circular ap. mag. smallint 2 CODE_MISC

j_flg_20 twomass_xsc 2MASS J confusion flag for 20 arcsec circular ap. mag. smallint 2 CODE_MISC

j_flg_25 twomass_xsc 2MASS J confusion flag for 25 arcsec circular ap. mag. smallint 2 CODE_MISC

j_flg_30 twomass_xsc 2MASS J confusion flag for 30 arcsec circular ap. mag. smallint 2 CODE_MISC

j_flg_40 twomass_xsc 2MASS J confusion flag for 40 arcsec circular ap. mag. smallint 2 CODE_MISC

j_flg_5 twomass_xsc 2MASS J confusion flag for 5 arcsec circular ap. mag. smallint 2 CODE_MISC

j_flg_50 twomass_xsc 2MASS J confusion flag for 50 arcsec circular ap. mag. smallint 2 CODE_MISC

j_flg_60 twomass_xsc 2MASS J confusion flag for 60 arcsec circular ap. mag. smallint 2 CODE_MISC

j_flg_7 twomass_sixx2_xsc 2MASS J confusion flag for 7 arcsec circular ap. mag smallint 2

j_flg_7 twomass_xsc 2MASS J confusion flag for 7 arcsec circular ap. mag. smallint 2 CODE_MISC

j_flg_70 twomass_xsc 2MASS J confusion flag for 70 arcsec circular ap. mag. smallint 2 CODE_MISC

j_flg_c twomass_xsc 2MASS J confusion flag for Kron circular mag. smallint 2 CODE_MISC

j_flg_e twomass_xsc 2MASS J confusion flag for Kron elliptical mag. smallint 2 CODE_MISC

j_flg_fc twomass_xsc 2MASS J confusion flag for fiducial Kron circ. mag. smallint 2 CODE_MISC

j_flg_fe twomass_xsc 2MASS J confusion flag for fiducial Kron ell. mag. smallint 2 CODE_MISC

j_flg_i20c twomass_xsc 2MASS J confusion flag for 20mag/sq." iso. circ. mag. smallint 2 CODE_MISC

j_flg_i20e twomass_xsc 2MASS J confusion flag for 20mag/sq." iso. ell. mag. smallint 2 CODE_MISC

j_flg_i21c twomass_xsc 2MASS J confusion flag for 21mag/sq." iso. circ. mag. smallint 2 CODE_MISC

j_flg_i21e twomass_xsc 2MASS J confusion flag for 21mag/sq." iso. ell. mag. smallint 2 CODE_MISC

j_flg_j21fc twomass_xsc 2MASS J confusion flag for 21mag/sq." iso. fid. circ. mag. smallint 2 CODE_MISC

j_flg_j21fe twomass_xsc 2MASS J confusion flag for 21mag/sq." iso. fid. ell. mag. smallint 2 CODE_MISC

j_flg_k20fc twomass_xsc 2MASS J confusion flag for 20mag/sq." iso. fid. circ. mag. smallint 2 CODE_MISC

j_flg_k20fe twomass_sixx2_xsc 2MASS J confusion flag for 20mag/sq.″ iso. fid. ell. mag smallint 2

j_flg_k20fe twomass_xsc 2MASS J confusion flag for 20mag/sq." iso. fid. ell. mag. smallint 2 CODE_MISC

j_h twomass_sixx2_psc 2MASS The J-H color, computed from the J-band and H-band magnitudes (j_m and h_m, respectively) of the source. In cases where the first or second 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

j_k twomass_sixx2_psc 2MASS The J-Ks color, computed from the J-band and Ks-band magnitudes (j_m and k_m, respectively) of the source. In cases where the first 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

j_m twomass_psc 2MASS Default J-band magnitude real 4 mag SPECT_FLUX_VALUE

j_m twomass_sixx2_psc 2MASS J selected "default" magnitude real 4 mag

j_m_10 twomass_xsc 2MASS J 10 arcsec radius circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

j_m_15 twomass_xsc 2MASS J 15 arcsec radius circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

j_m_20 twomass_xsc 2MASS J 20 arcsec radius circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

j_m_25 twomass_xsc 2MASS J 25 arcsec radius circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

j_m_30 twomass_xsc 2MASS J 30 arcsec radius circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

j_m_40 twomass_xsc 2MASS J 40 arcsec radius circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

j_m_5 twomass_xsc 2MASS J 5 arcsec radius circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

j_m_50 twomass_xsc 2MASS J 50 arcsec radius circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

j_m_60 twomass_xsc 2MASS J 60 arcsec radius circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

j_m_7 twomass_sixx2_xsc 2MASS J 7 arcsec radius circular aperture magnitude real 4 mag

j_m_7 twomass_xsc 2MASS J 7 arcsec radius circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

j_m_70 twomass_xsc 2MASS J 70 arcsec radius circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

j_m_c twomass_xsc 2MASS J Kron circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

j_m_e twomass_xsc 2MASS J Kron elliptical aperture magnitude. real 4 mag SPECT_FLUX_VALUE

j_m_ext twomass_sixx2_xsc 2MASS J mag from fit extrapolation real 4 mag

j_m_ext twomass_xsc 2MASS J mag from fit extrapolation. real 4 mag SPECT_FLUX_VALUE

j_m_fc twomass_xsc 2MASS J fiducial Kron circular magnitude. real 4 mag SPECT_FLUX_VALUE

j_m_fe twomass_xsc 2MASS J fiducial Kron ell. mag aperture magnitude. real 4 mag SPECT_FLUX_VALUE

j_m_i20c twomass_xsc 2MASS J 20mag/sq." isophotal circular ap. magnitude. real 4 mag SPECT_FLUX_VALUE

j_m_i20e twomass_xsc 2MASS J 20mag/sq." isophotal elliptical ap. magnitude. real 4 mag SPECT_FLUX_VALUE

j_m_i21c twomass_xsc 2MASS J 21mag/sq." isophotal circular ap. magnitude. real 4 mag SPECT_FLUX_VALUE

j_m_i21e twomass_xsc 2MASS J 21mag/sq." isophotal elliptical ap. magnitude. real 4 mag SPECT_FLUX_VALUE

j_m_j21fc twomass_xsc 2MASS J 21mag/sq." isophotal fiducial circ. ap. mag. real 4 mag SPECT_FLUX_VALUE

j_m_j21fe twomass_xsc 2MASS J 21mag/sq." isophotal fiducial ell. ap. magnitude. real 4 mag SPECT_FLUX_VALUE

j_m_k20fc twomass_xsc 2MASS J 20mag/sq." isophotal fiducial circ. ap. mag. real 4 mag SPECT_FLUX_VALUE

J_M_K20FE twomass SIXDF J 20mag/sq." isophotal fiducial ell. ap. magnitude real 4 mag

j_m_k20fe twomass_sixx2_xsc 2MASS J 20mag/sq.″ isophotal fiducial ell. ap. magnitude real 4 mag

j_m_k20fe twomass_xsc 2MASS J 20mag/sq." isophotal fiducial ell. ap. magnitude. real 4 mag SPECT_FLUX_VALUE

j_m_stdap twomass_psc 2MASS J-band "standard" aperture magnitude. real 4 mag SPECT_FLUX_VALUE

j_m_sys twomass_xsc 2MASS J system photometry magnitude. real 4 mag SPECT_FLUX_VALUE

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

j_msig twomass_sixx2_psc 2MASS J "default" mag uncertainty real 4 mag

j_msig_10 twomass_xsc 2MASS J 1-sigma uncertainty in 10 arcsec circular ap. mag. real 4 mag ERROR

j_msig_15 twomass_xsc 2MASS J 1-sigma uncertainty in 15 arcsec circular ap. mag. real 4 mag ERROR

j_msig_20 twomass_xsc 2MASS J 1-sigma uncertainty in 20 arcsec circular ap. mag. real 4 mag ERROR

j_msig_25 twomass_xsc 2MASS J 1-sigma uncertainty in 25 arcsec circular ap. mag. real 4 mag ERROR

j_msig_30 twomass_xsc 2MASS J 1-sigma uncertainty in 30 arcsec circular ap. mag. real 4 mag ERROR

j_msig_40 twomass_xsc 2MASS J 1-sigma uncertainty in 40 arcsec circular ap. mag. real 4 mag ERROR

j_msig_5 twomass_xsc 2MASS J 1-sigma uncertainty in 5 arcsec circular ap. mag. real 4 mag ERROR

j_msig_50 twomass_xsc 2MASS J 1-sigma uncertainty in 50 arcsec circular ap. mag. real 4 mag ERROR

j_msig_60 twomass_xsc 2MASS J 1-sigma uncertainty in 60 arcsec circular ap. mag. real 4 mag ERROR

j_msig_7 twomass_sixx2_xsc 2MASS J 1-sigma uncertainty in 7 arcsec circular ap. mag real 4 mag

j_msig_7 twomass_xsc 2MASS J 1-sigma uncertainty in 7 arcsec circular ap. mag. real 4 mag ERROR

j_msig_70 twomass_xsc 2MASS J 1-sigma uncertainty in 70 arcsec circular ap. mag. real 4 mag ERROR

j_msig_c twomass_xsc 2MASS J 1-sigma uncertainty in Kron circular mag. real 4 mag ERROR

j_msig_e twomass_xsc 2MASS J 1-sigma uncertainty in Kron elliptical mag. real 4 mag ERROR

j_msig_ext twomass_sixx2_xsc 2MASS J 1-sigma uncertainty in mag from fit extrapolation real 4 mag

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

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

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

j_msig_i20c twomass_xsc 2MASS J 1-sigma uncertainty in 20mag/sq." iso. circ. mag. real 4 mag ERROR

j_msig_i20e twomass_xsc 2MASS J 1-sigma uncertainty in 20mag/sq." iso. ell. mag. real 4 mag ERROR

j_msig_i21c twomass_xsc 2MASS J 1-sigma uncertainty in 21mag/sq." iso. circ. mag. real 4 mag ERROR

j_msig_i21e twomass_xsc 2MASS J 1-sigma uncertainty in 21mag/sq." iso. ell. mag. real 4 mag ERROR

j_msig_j21fc twomass_xsc 2MASS J 1-sigma uncertainty in 21mag/sq." iso.fid.circ.mag. real 4 mag ERROR

j_msig_j21fe twomass_xsc 2MASS J 1-sigma uncertainty in 21mag/sq." iso.fid.ell.mag. real 4 mag ERROR

j_msig_k20fc twomass_xsc 2MASS J 1-sigma uncertainty in 20mag/sq." iso.fid.circ. mag. real 4 mag ERROR

j_msig_k20fe twomass_xsc 2MASS J 1-sigma uncertainty in 20mag/sq." iso.fid.ell.mag. real 4 mag ERROR

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

j_msig_sys twomass_xsc 2MASS J 1-sigma uncertainty in system photometry mag. real 4 mag ERROR

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

j_msigcom twomass_sixx2_psc 2MASS combined (total) J band photometric uncertainty real 4 mag

j_msnr10 twomass_scn 2MASS The estimated J-band magnitude at which SNR=10 is achieved for this scan. real 4 mag SPECT_FLUX_VALUE

j_msnr10 twomass_sixx2_scn 2MASS J mag at which SNR=10 is achieved, from j_psp and j_zp_ap real 4 mag

j_n_snr10 twomass_scn 2MASS Number of point sources at J-band with SNR>10 (instrumental mag <=15.8) int 4 NUMBER

j_n_snr10 twomass_sixx2_scn 2MASS number of J point sources with SNR>10 (instrumental m<=15.8) int 4

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

j_peak twomass_xsc 2MASS J peak pixel brightness. real 4 mag PHOT_SB_GENERAL

j_perc_darea twomass_xsc 2MASS J 5-sigma to 3-sigma percent area change. smallint 2 FIT_PARAM

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

j_psfchi twomass_psc 2MASS Reduced chi-squared goodness-of-fit value for the J-band profile-fit photometry made on the 1.3 s "Read_2" exposures. real 4 FIT_PARAM_VALUE

j_psp twomass_scn 2MASS J-band photometric sensitivity paramater (PSP). real 4 INST_SENSITIVITY

j_psp twomass_sixx2_scn 2MASS J photometric sensitivity param: j_shape_avg*(j_fbg_avg^.29) real 4

j_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 J-band photometric errors and is expressed in units of mJy. real 4 INST_NOISE

j_pts_noise twomass_sixx2_scn 2MASS log10 of J band modal point src noise estimate real 4 logmJy

j_r_c twomass_xsc 2MASS J Kron circular aperture radius. real 4 arcsec EXTENSION_RAD

j_r_e twomass_xsc 2MASS J Kron elliptical aperture semi-major axis. real 4 arcsec EXTENSION_RAD

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

j_r_i20c twomass_xsc 2MASS J 20mag/sq." isophotal circular aperture radius. real 4 arcsec EXTENSION_RAD

j_r_i20e twomass_xsc 2MASS J 20mag/sq." isophotal elliptical ap. semi-major axis. real 4 arcsec EXTENSION_RAD

j_r_i21c twomass_xsc 2MASS J 21mag/sq." isophotal circular aperture radius. real 4 arcsec EXTENSION_RAD

j_r_i21e twomass_xsc 2MASS J 21mag/sq." isophotal elliptical ap. semi-major axis. real 4 arcsec EXTENSION_RAD

j_resid_ann twomass_xsc 2MASS J residual annulus background median. real 4 DN CODE_MISC

j_sc_1mm twomass_xsc 2MASS J 1st moment (score) (LCSB: super blk 2,4,8 SNR). real 4 CODE_MISC

j_sc_2mm twomass_xsc 2MASS J 2nd moment (score) (LCSB: SNRMAX - super SNR max). real 4 CODE_MISC

j_sc_msh twomass_xsc 2MASS J median shape score. real 4 CODE_MISC

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

j_sc_r1 twomass_xsc 2MASS J r1 (score). real 4 CODE_MISC

j_sc_r23 twomass_xsc 2MASS J r23 (score) (LCSB: TSNR - integrated SNR for r=15). real 4 CODE_MISC

j_sc_sh twomass_xsc 2MASS J shape (score). real 4 CODE_MISC

j_sc_vint twomass_xsc 2MASS J vint (score). real 4 CODE_MISC

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

j_seetrack twomass_xsc 2MASS J band seetracking score. real 4 CODE_MISC

j_sh0 twomass_xsc 2MASS J ridge shape (LCSB: BSNR limit). real 4 FIT_PARAM

j_shape_avg twomass_scn 2MASS J-band average seeing shape for scan. real 4 INST_SEEING

j_shape_avg twomass_sixx2_scn 2MASS J band average seeing shape for scan real 4

j_shape_rms twomass_scn 2MASS RMS-error of J-band average seeing shape. real 4 INST_SEEING

j_shape_rms twomass_sixx2_scn 2MASS rms of J band avg seeing shape for scan real 4

j_sig_sh0 twomass_xsc 2MASS J ridge shape sigma (LCSB: B2SNR limit). real 4 FIT_PARAM

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

j_snr twomass_sixx2_psc 2MASS J band "scan" signal-to-noise ratio real 4

j_subst2 twomass_xsc 2MASS J residual background #2 (score). real 4 CODE_MISC

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

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

jAperMag1 vmcSynopticSource VSAQC Extended source J aperture corrected mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

jAperMag1 vmcSynopticSource VSAVMC Extended source J aperture corrected mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

jAperMag1 vvvSource VSAQC Extended source J aperture corrected mag (0.7 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

jAperMag1 vvvSource VSAVVV Extended source J aperture corrected mag (0.7 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

jAperMag1Err vmcSynopticSource VSAQC Error in extended source J mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag1Err vmcSynopticSource VSAVMC Error in extended source J mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag1Err vvvSource VSAQC Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag1Err vvvSource VSAVVV Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag2 vmcSynopticSource VSAQC Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

jAperMag2 vmcSynopticSource VSAVMC Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

jAperMag2Err vmcSynopticSource VSAQC Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag2Err vmcSynopticSource VSAVMC Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag3 svNgc253Source VSASVNGC253 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

jAperMag3 svOrionSource VSASVORION Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

jAperMag3 ultravistaSource VSAUltraVISTA Default point/extended source J mag, no aperture correction applied
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

jAperMag3 ultravistaSource, videoSource VSAQC Default point/extended source J mag, no aperture correction applied
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

jAperMag3 vhsSource VSAVHS Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

jAperMag3 vhsSource, vikingSource, vmcSource VSAQC Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

jAperMag3 vmcSynopticSource VSAQC Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

jAperMag3 vmcSynopticSource VSAVMC Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

jAperMag3 vvvSource VSAQC Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

jAperMag3 vvvSource VSAVVV Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

jAperMag3Err svNgc253Source VSASVNGC253 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag3Err svOrionSource VSASVORION Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag3Err ultravistaSource VSAUltraVISTA Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag3Err ultravistaSource, vhsSource, videoSource, vikingSource, vmcSource, vmcSynopticSource, vvvSource VSAQC Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag4 svNgc253Source VSASVNGC253 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

jAperMag4 svOrionSource VSASVORION Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

jAperMag4 ultravistaSource VSAUltraVISTA Extended source J mag, no aperture correction applied real 4 mag -0.9999995e9 PHOT_MAG

jAperMag4 ultravistaSource, videoSource VSAQC Extended source J mag, no aperture correction applied real 4 mag -0.9999995e9 PHOT_MAG

jAperMag4 vhsSource VSAVHS Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

jAperMag4 vhsSource, vikingSource, vmcSource VSAQC Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

jAperMag4 vmcSynopticSource VSAVMC Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

jAperMag4 vmcSynopticSource, vvvSource VSAQC Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

jAperMag4Err svNgc253Source VSASVNGC253 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag4Err svOrionSource VSASVORION Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag4Err ultravistaSource VSAUltraVISTA Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag4Err ultravistaSource, videoSource, vmcSynopticSource, vvvSource VSAQC Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag4Err vhsSource VSAVHS Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag4Err vhsSource, vikingSource, vmcSource VSAQC Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag5 vmcSynopticSource VSAQC Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

jAperMag5 vmcSynopticSource VSAVMC Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

jAperMag5Err vmcSynopticSource VSAQC Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag5Err vmcSynopticSource VSAVMC Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag6 svNgc253Source VSASVNGC253 Extended source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

jAperMag6 svOrionSource VSASVORION Extended source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

jAperMag6 ultravistaSource VSAUltraVISTA Extended source J mag, no aperture correction applied real 4 mag -0.9999995e9 PHOT_MAG

jAperMag6 ultravistaSource, videoSource VSAQC Extended source J mag, no aperture correction applied real 4 mag -0.9999995e9 PHOT_MAG

jAperMag6 vhsSource VSAVHS Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

jAperMag6 vhsSource, vikingSource, vmcSource VSAQC Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

jAperMag6Err svNgc253Source VSASVNGC253 Error in extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag6Err svOrionSource VSASVORION Error in extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag6Err ultravistaSource VSAUltraVISTA Error in extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag6Err ultravistaSource, videoSource VSAQC Error in extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag6Err vhsSource VSAVHS Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag6Err vhsSource, vikingSource, vmcSource VSAQC Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMagNoAperCorr3 vhsSource VSAVHS Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

jAperMagNoAperCorr3 vhsSource, vikingSource, vmcSource VSAQC Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

jAperMagNoAperCorr4 vhsSource VSAVHS Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

jAperMagNoAperCorr4 vhsSource, vikingSource, vmcSource VSAQC Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

jAperMagNoAperCorr6 vhsSource VSAVHS Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

jAperMagNoAperCorr6 vhsSource, vikingSource, vmcSource VSAQC Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

jaStratAst videoVarFrameSetInfo VSAVIDEO Strateva parameter, a, in fit to astrometric rms vs magnitude in J 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.

jaStratAst videoVarFrameSetInfo, vikingVarFrameSetInfo, vmcVarFrameSetInfo, vvvVarFrameSetInfo VSAQC Strateva parameter, a, in fit to astrometric rms vs magnitude in J 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.

jaStratPht videoVarFrameSetInfo VSAVIDEO Strateva parameter, a, in fit to photometric rms vs magnitude in J 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.

jaStratPht videoVarFrameSetInfo, vikingVarFrameSetInfo, vmcVarFrameSetInfo, vvvVarFrameSetInfo VSAQC Strateva parameter, a, in fit to photometric rms vs magnitude in J 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.

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

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

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

jAverageConf vhsSource, vikingSource, vmcSource, vmcSynopticSource VSAQC average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -99999999 CODE_MISC

jbestAper videoVariability VSAVIDEO Best aperture (1-6) for photometric statistics in the J 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)

jbestAper videoVariability, vikingVariability, vmcVariability, vvvVariability VSAQC Best aperture (1-6) for photometric statistics in the J 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)

jbStratAst videoVarFrameSetInfo VSAVIDEO Strateva parameter, b, in fit to astrometric rms vs magnitude in J 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.

jbStratAst videoVarFrameSetInfo, vikingVarFrameSetInfo, vmcVarFrameSetInfo, vvvVarFrameSetInfo VSAQC Strateva parameter, b, in fit to astrometric rms vs magnitude in J 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.

jbStratPht videoVarFrameSetInfo VSAVIDEO Strateva parameter, b, in fit to photometric rms vs magnitude in J 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.

jbStratPht videoVarFrameSetInfo, vikingVarFrameSetInfo, vmcVarFrameSetInfo, vvvVarFrameSetInfo VSAQC Strateva parameter, b, in fit to photometric rms vs magnitude in J 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.

jchiSqAst videoVarFrameSetInfo VSAVIDEO Goodness of fit of Strateva function to astrometric data in J 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.

jchiSqAst videoVarFrameSetInfo, vikingVarFrameSetInfo, vmcVarFrameSetInfo, vvvVarFrameSetInfo VSAQC Goodness of fit of Strateva function to astrometric data in J 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.

jchiSqpd 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.

jchiSqpd videoVariability, vikingVariability, vmcVariability, 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.

jchiSqPht videoVarFrameSetInfo VSAVIDEO Goodness of fit of Strateva function to photometric data in J 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.

jchiSqPht videoVarFrameSetInfo, vikingVarFrameSetInfo, vmcVarFrameSetInfo, vvvVarFrameSetInfo VSAQC Goodness of fit of Strateva function to photometric data in J 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.

jClass svNgc253Source VSASVNGC253 discrete image classification flag in J smallint 2 -9999 CLASS_MISC

jClass svOrionSource VSASVORION discrete image classification flag in J smallint 2 -9999 CLASS_MISC

jClass ultravistaSource VSAUltraVISTA discrete image classification flag in J smallint 2 -9999 CLASS_MISC

jClass ultravistaSource, ultravistaSourceRemeasurement, vhsSource, vhsSourceRemeasurement, videoSource, videoSourceRemeasurement, vikingSource, vikingSourceRemeasurement, vmcSource, vmcSourceRemeasurement, vmcSynopticSource, vvvSource, vvvSourceRemeasurement VSAQC discrete image classification flag in J smallint 2 -9999 CLASS_MISC

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

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

jClassStat ultravistaSource VSAUltraVISTA S-Extractor classification statistic in J real 4 -0.9999995e9 STAT_PROP

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

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

jClassStat ultravistaSourceRemeasurement, vhsSource, vhsSourceRemeasurement, videoSourceRemeasurement, vikingSource, vikingSourceRemeasurement, vmcSource, vmcSourceRemeasurement, vmcSynopticSource, vvvSourceRemeasurement VSAQC N(0,1) stellarness-of-profile statistic in J real 4 -0.9999995e9 STAT_PROP

jcStratAst videoVarFrameSetInfo VSAVIDEO Strateva parameter, c, in fit to astrometric rms vs magnitude in J 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.

jcStratAst videoVarFrameSetInfo, vikingVarFrameSetInfo, vmcVarFrameSetInfo, vvvVarFrameSetInfo VSAQC Strateva parameter, c, in fit to astrometric rms vs magnitude in J 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.

jcStratPht videoVarFrameSetInfo VSAVIDEO Strateva parameter, c, in fit to photometric rms vs magnitude in J 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.

jcStratPht videoVarFrameSetInfo, vikingVarFrameSetInfo, vmcVarFrameSetInfo, vvvVarFrameSetInfo VSAQC Strateva parameter, c, in fit to photometric rms vs magnitude in J 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.

jdate twomass_psc 2MASS The Julian Date of the source measurement accurate to +-30 seconds. float 8 Julian days TIME_DATE

jdate twomass_scn 2MASS Julian Date at beginning of scan. float 8 Julian days TIME_DATE

jdate twomass_sixx2_psc 2MASS julian date of source measurement to +/- 30 sec float 8 jdate

jdate twomass_sixx2_scn 2MASS Julian date beginning UT of scan data float 8 jdate

jdate twomass_xsc 2MASS Julian date of the source measurement accurate to +-3 minutes. float 8 Julian days TIME_DATE

jDeblend ultravistaSource VSAUltraVISTA placeholder flag indicating parent/child relation in J int 4 -99999999 CODE_MISC

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

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

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

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

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

jeNum svNgc253MergeLog VSASVNGC253 the extension number of this J frame tinyint 1 NUMBER

jeNum svOrionMergeLog VSASVORION the extension number of this J frame tinyint 1 NUMBER

jeNum ultravistaMergeLog VSAUltraVISTA the extension number of this J frame tinyint 1 NUMBER

jeNum ultravistaMergeLog, vhsMergeLog, videoMergeLog, vikingMergeLog, vmcMergeLog, vmcSynopticMergeLog, vvvMergeLog VSAQC the extension number of this J frame tinyint 1 NUMBER

jErrBits svNgc253Source VSASVNGC253 processing warning/error bitwise flags in J 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.

jErrBits svOrionSource VSASVORION processing warning/error bitwise flags in J 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.

jErrBits ultravistaSource VSAUltraVISTA processing warning/error bitwise flags in J 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

jErrBits ultravistaSource, videoSource VSAQC processing warning/error bitwise flags in J 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

jErrBits ultravistaSourceRemeasurement VSAUltraVISTA processing warning/error bitwise flags in J int 4 -99999999 CODE_MISC

jErrBits ultravistaSourceRemeasurement, vhsSourceRemeasurement, videoSourceRemeasurement, vikingSourceRemeasurement, vmcSourceRemeasurement, vvvSourceRemeasurement VSAQC processing warning/error bitwise flags in J int 4 -99999999 CODE_MISC

jErrBits vhsSource VSAVHS processing warning/error bitwise flags in J 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.

jErrBits vhsSource, vikingSource, vmcSource, vmcSynopticSource, vvvSource VSAQC processing warning/error bitwise flags in J 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.

jEta svNgc253Source VSASVNGC253 Offset of J 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.

jEta svOrionSource VSASVORION Offset of J 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.

jEta ultravistaSource VSAUltraVISTA Offset of J 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.

jEta ultravistaSource, vhsSource, videoSource, vikingSource, vmcSource, vmcSynopticSource, vvvSource VSAQC Offset of J 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.

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

jexpML videoVarFrameSetInfo, vikingVarFrameSetInfo, vmcVarFrameSetInfo, vvvVarFrameSetInfo VSAQC Expected magnitude limit of frameSet in this in J band. real 4 -0.9999995e9

jExpRms videoVariability VSAVIDEO Rms calculated from polynomial fit to modal RMS as a function of magnitude in J 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.

jExpRms videoVariability, vikingVariability, vmcVariability, vvvVariability VSAQC Rms calculated from polynomial fit to modal RMS as a function of magnitude in J 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.

jGausig svNgc253Source VSASVNGC253 RMS of axes of ellipse fit in J real 4 pixels -0.9999995e9 MORPH_PARAM

jGausig svOrionSource VSASVORION RMS of axes of ellipse fit in J real 4 pixels -0.9999995e9 MORPH_PARAM

jGausig ultravistaSource VSAUltraVISTA RMS of axes of ellipse fit in J real 4 pixels -0.9999995e9 MORPH_PARAM

jGausig ultravistaSource, ultravistaSourceRemeasurement, vhsSource, vhsSourceRemeasurement, videoSource, videoSourceRemeasurement, vikingSource, vikingSourceRemeasurement, vmcSource, vmcSourceRemeasurement, vmcSynopticSource, vvvSource, vvvSourceRemeasurement VSAQC RMS of axes of ellipse fit in J real 4 pixels -0.9999995e9 MORPH_PARAM

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

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

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

jIntRms videoVariability VSAVIDEO Intrinsic rms in J-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.

jIntRms videoVariability, vikingVariability, vmcVariability, vvvVariability VSAQC Intrinsic rms in J-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.

jitterID Multiframe VSASVNGC253 Sequence number of jitter {image primary HDU keyword: JITTER_I} smallint 2 -9999

jitterID Multiframe VSASVORION Sequence number of jitter {image primary HDU keyword: JITTER_I} smallint 2 -9999

jitterID Multiframe VSAUltraVISTA Sequence number of jitter {image primary HDU keyword: JITTER_I} smallint 2 -9999

jitterID Multiframe VSAVHS Sequence number of jitter {image primary HDU keyword: JITTER_I} smallint 2 -9999

jitterID Multiframe VSAVIDEO Sequence number of jitter {image primary HDU keyword: JITTER_I} smallint 2 -9999

jitterID Multiframe VSAVIKING Sequence number of jitter {image primary HDU keyword: JITTER_I} smallint 2 -9999

jitterID Multiframe VSAVMC Sequence number of jitter {image primary HDU keyword: JITTER_I} smallint 2 -9999

jitterID Multiframe VSAVVV Sequence number of jitter {image primary HDU keyword: JITTER_I} smallint 2 -9999

jitterID ultravistaMultiframe, vhsMultiframe, videoMultiframe, vikingMultiframe, vmcMultiframe, vvvMultiframe VSAQC Sequence number of jitter smallint 2 -9999

jitterName Multiframe VSASVNGC253 Name of jitter pattern {image primary HDU keyword: JITTR_ID} varchar 8 NONE

jitterName Multiframe VSASVORION Name of jitter pattern {image primary HDU keyword: JITTR_ID} varchar 8 NONE

jitterName Multiframe VSAUltraVISTA Name of jitter pattern {image primary HDU keyword: JITTR_ID} varchar 8 NONE

jitterName Multiframe VSAVHS Name of jitter pattern {image primary HDU keyword: JITTR_ID} varchar 8 NONE

jitterName Multiframe VSAVIDEO Name of jitter pattern {image primary HDU keyword: JITTR_ID} varchar 8 NONE

jitterName Multiframe VSAVIKING Name of jitter pattern {image primary HDU keyword: JITTR_ID} varchar 8 NONE

jitterName Multiframe VSAVMC Name of jitter pattern {image primary HDU keyword: JITTR_ID} varchar 8 NONE

jitterName Multiframe VSAVVV Name of jitter pattern {image primary HDU keyword: JITTR_ID} varchar 8 NONE

jitterName ultravistaMultiframe, vhsMultiframe, videoMultiframe, vikingMultiframe, vmcMultiframe, vvvMultiframe VSAQC Name of jitter pattern varchar 8 NONE

jitterX Multiframe VSASVNGC253 X offset in jitter pattern [arcsec] {image primary HDU keyword: JITTER_X} real 4 -0.9999995e9

jitterX Multiframe VSASVORION X offset in jitter pattern [arcsec] {image primary HDU keyword: JITTER_X} real 4 -0.9999995e9

jitterX Multiframe VSAUltraVISTA X offset in jitter pattern [arcsec] {image primary HDU keyword: JITTER_X} real 4 -0.9999995e9

jitterX Multiframe VSAVHS X offset in jitter pattern [arcsec] {image primary HDU keyword: JITTER_X} real 4 -0.9999995e9

jitterX Multiframe VSAVIDEO X offset in jitter pattern [arcsec] {image primary HDU keyword: JITTER_X} real 4 -0.9999995e9

jitterX Multiframe VSAVIKING X offset in jitter pattern [arcsec] {image primary HDU keyword: JITTER_X} real 4 -0.9999995e9

jitterX Multiframe VSAVMC X offset in jitter pattern [arcsec] {image primary HDU keyword: JITTER_X} real 4 -0.9999995e9

jitterX Multiframe VSAVVV X offset in jitter pattern [arcsec] {image primary HDU keyword: JITTER_X} real 4 -0.9999995e9

jitterX ultravistaMultiframe, vhsMultiframe, videoMultiframe, vikingMultiframe, vmcMultiframe, vvvMultiframe VSAQC X offset in jitter pattern [arcsec] real 4 -0.9999995e9

jitterY Multiframe VSASVNGC253 Y offset in jitter pattern [arcsec] {image primary HDU keyword: JITTER_Y} real 4 -0.9999995e9

jitterY Multiframe VSASVORION Y offset in jitter pattern [arcsec] {image primary HDU keyword: JITTER_Y} real 4 -0.9999995e9

jitterY Multiframe VSAUltraVISTA Y offset in jitter pattern [arcsec] {image primary HDU keyword: JITTER_Y} real 4 -0.9999995e9

jitterY Multiframe VSAVHS Y offset in jitter pattern [arcsec] {image primary HDU keyword: JITTER_Y} real 4 -0.9999995e9

jitterY Multiframe VSAVIDEO Y offset in jitter pattern [arcsec] {image primary HDU keyword: JITTER_Y} real 4 -0.9999995e9

jitterY Multiframe VSAVIKING Y offset in jitter pattern [arcsec] {image primary HDU keyword: JITTER_Y} real 4 -0.9999995e9

jitterY Multiframe VSAVMC Y offset in jitter pattern [arcsec] {image primary HDU keyword: JITTER_Y} real 4 -0.9999995e9

jitterY Multiframe VSAVVV Y offset in jitter pattern [arcsec] {image primary HDU keyword: JITTER_Y} real 4 -0.9999995e9

jitterY ultravistaMultiframe, vhsMultiframe, videoMultiframe, vikingMultiframe, vmcMultiframe, vvvMultiframe VSAQC Y offset in jitter pattern [arcsec] real 4 -0.9999995e9

jksiWS vmcVariability VSAQC Welch-Stetson statistic between J and Ks. This assumes colour does not vary much and helps remove variation due to a few poor detections real 4 -0.9999995e9

The Welch-Stetson statistic is a measure of the correlation of the variability between two bands. We use the calculation in Welch D.L. and Stetson P.B. 1993, AJ, 105, 5, which is also used in Sesar et al. 2007, AJ, 134, 2236. We use the aperMag3 magnitude when comparing between bands.

jksiWS vmcVariability VSAVMC Welch-Stetson statistic between J and Ks. This assumes colour does not vary much and helps remove variation due to a few poor detections real 4 -0.9999995e9

The Welch-Stetson statistic is a measure of the correlation of the variability between two bands. We use the calculation in Welch D.L. and Stetson P.B. 1993, AJ, 105, 5, which is also used in Sesar et al. 2007, AJ, 134, 2236. We use the aperMag3 magnitude when comparing between bands.

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

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

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

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

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

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

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

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

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

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

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

Jmag2MASS spitzer_smcSource SPITZER The 2MASS J band magnitude. real 4 mag

jMagErr ukirtFSstars VSASVNGC253 J band magnitude error real 4 mag ERROR

jMagErr ukirtFSstars VSASVORION J band magnitude error real 4 mag ERROR

jMagErr ukirtFSstars VSAUltraVISTA J band magnitude error real 4 mag ERROR

jMagErr ukirtFSstars VSAVHS J band magnitude error real 4 mag ERROR

jMagErr ukirtFSstars VSAVIDEO J band magnitude error real 4 mag ERROR

jMagErr ukirtFSstars VSAVIKING J band magnitude error real 4 mag ERROR

jMagErr ukirtFSstars VSAVMC J band magnitude error real 4 mag ERROR

jMagErr ukirtFSstars VSAVVV J band magnitude error real 4 mag ERROR

jMagErr ultravistaSourceRemeasurement VSAUltraVISTA Error in J mag real 4 mag -0.9999995e9 ERROR

jMagErr ultravistaSourceRemeasurement, vhsSourceRemeasurement, videoSourceRemeasurement, vikingSourceRemeasurement, vmcSourceRemeasurement, vvvSourceRemeasurement VSAQC Error in J mag real 4 mag -0.9999995e9 ERROR

jMagMAD videoVariability VSAVIDEO Median Absolute Deviation of J 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.

jMagMAD videoVariability, vikingVariability, vmcVariability, vvvVariability VSAQC Median Absolute Deviation of J 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.

jMagRms videoVariability VSAVIDEO rms of J 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.

jMagRms videoVariability, vikingVariability, vmcVariability, vvvVariability VSAQC rms of J 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.

jmaxCadence 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.

jmaxCadence videoVariability, vikingVariability, vmcVariability, 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.

jMaxMag videoVariability VSAVIDEO Maximum magnitude in J 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.

jMaxMag videoVariability, vikingVariability, vmcVariability, vvvVariability VSAQC Maximum magnitude in J 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.

jmeanMag videoVariability VSAVIDEO Mean J 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.

jmeanMag videoVariability, vikingVariability, vmcVariability, vvvVariability VSAQC Mean J 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.

jmedCadence 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.

jmedCadence videoVariability, vikingVariability, vmcVariability, 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.

jmedianMag videoVariability VSAVIDEO Median J 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.

jmedianMag videoVariability, vikingVariability, vmcVariability, vvvVariability VSAQC Median J 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.

jmfID svNgc253MergeLog VSASVNGC253 the UID of the relevant J multiframe bigint 8 ID_FRAME

jmfID svOrionMergeLog VSASVORION the UID of the relevant J multiframe bigint 8 ID_FRAME

jmfID ultravistaMergeLog VSAUltraVISTA the UID of the relevant J multiframe bigint 8 ID_FRAME

jmfID ultravistaMergeLog, vhsMergeLog, videoMergeLog, vikingMergeLog, vmcMergeLog, vmcSynopticMergeLog, vvvMergeLog VSAQC the UID of the relevant J multiframe bigint 8 ID_FRAME

jmh ultravistaSourceRemeasurement VSAUltraVISTA Default colour J-H (using appropriate mags) real 4 mag PHOT_COLOR

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

jmhErr ultravistaSourceRemeasurement VSAUltraVISTA Error on colour J-H real 4 mag ERROR

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

jmhExt svNgc253Source VSASVNGC253 Extended source colour J-H (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.

jmhExt svOrionSource VSASVORION Extended source colour J-H (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.

jmhExt ultravistaSource VSAUltraVISTA Extended source colour J-H (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.

jmhExt ultravistaSource, videoSource, vvvSource VSAQC Extended source colour J-H (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.

jmhExt vhsSource VSAVHS Extended source colour J-H (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.

jmhExt vhsSource, vikingSource VSAQC Extended source colour J-H (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.

jmhExtErr svNgc253Source VSASVNGC253 Error on extended source colour J-H 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.

jmhExtErr svOrionSource VSASVORION Error on extended source colour J-H 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.

jmhExtErr ultravistaSource VSAUltraVISTA Error on extended source colour J-H 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.

jmhExtErr ultravistaSource, vhsSource, videoSource, vikingSource, vvvSource VSAQC Error on extended source colour J-H 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.

jmhPnt svNgc253Source VSASVNGC253 Point source colour J-H (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.

jmhPnt svOrionSource VSASVORION Point source colour J-H (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.

jmhPnt ultravistaSource VSAUltraVISTA Point source colour J-H (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.

jmhPnt ultravistaSource, vhsSource, videoSource, vikingSource, vvvSource VSAQC Point source colour J-H (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.

jmhPntErr svNgc253Source VSASVNGC253 Error on point source colour J-H 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.

jmhPntErr svOrionSource VSASVORION Error on point source colour J-H 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.

jmhPntErr ultravistaSource VSAUltraVISTA Error on point source colour J-H 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.

jmhPntErr ultravistaSource, vhsSource, videoSource, vikingSource, vvvSource VSAQC Error on point source colour J-H 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.

jminCadence 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.

jminCadence videoVariability, vikingVariability, vmcVariability, 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.

jMinMag videoVariability VSAVIDEO Minimum magnitude in J 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.

jMinMag videoVariability, vikingVariability, vmcVariability, vvvVariability VSAQC Minimum magnitude in J 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.

jmks vmcSourceRemeasurement VSAQC Default colour J-Ks (using appropriate mags) real 4 mag PHOT_COLOR

jmks vmcSourceRemeasurement VSAVMC Default colour J-Ks (using appropriate mags) real 4 mag PHOT_COLOR

jmksErr vmcSourceRemeasurement VSAQC Error on colour J-Ks real 4 mag ERROR

jmksErr vmcSourceRemeasurement VSAVMC Error on colour J-Ks real 4 mag ERROR

jmksExt vhsSource VSAVHS Extended source colour J-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.

jmksExt vhsSource, vmcSource VSAQC Extended source colour J-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.

jmksExtErr vhsSource VSAVHS Error on extended source colour J-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.

jmksExtErr vhsSource, vmcSource VSAQC Error on extended source colour J-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.

jmksPnt vhsSource VSAVHS Point source colour J-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.

jmksPnt vhsSource, vmcSource, vmcSynopticSource VSAQC Point source colour J-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.

jmksPntErr vhsSource VSAVHS Error on point source colour J-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.

jmksPntErr vhsSource, vmcSource, vmcSynopticSource VSAQC Error on point source colour J-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.

jndof 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.

jndof videoVariability, vikingVariability, vmcVariability, 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.

jnDofAst videoVarFrameSetInfo VSAVIDEO Number of degrees of freedom of astrometric fit in J 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.

jnDofAst videoVarFrameSetInfo, vikingVarFrameSetInfo, vmcVarFrameSetInfo, vvvVarFrameSetInfo VSAQC Number of degrees of freedom of astrometric fit in J 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.

jnDofPht videoVarFrameSetInfo VSAVIDEO Number of degrees of freedom of photometric fit in J 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.

jnDofPht videoVarFrameSetInfo, vikingVarFrameSetInfo, vmcVarFrameSetInfo, vvvVarFrameSetInfo VSAQC Number of degrees of freedom of photometric fit in J 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.

jnFlaggedObs videoVariability VSAQC Number of detections in J 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.

jnFlaggedObs videoVariability VSAVIDEO Number of detections in J 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.

jnFlaggedObs vikingVariability VSAQC Number of detections in J 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.

jnFlaggedObs vikingVariability VSAVIKING Number of detections in J 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.

jnFlaggedObs vmcVariability VSAQC Number of detections in J band flagged as potentially spurious by vmcDetection.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.

jnFlaggedObs vmcVariability VSAVMC Number of detections in J band flagged as potentially spurious by vmcDetection.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.

jnFlaggedObs vvvVariability VSAQC Number of detections in J 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.

jnFlaggedObs vvvVariability VSAVVV Number of detections in J 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.

jnGoodObs videoVariability VSAVIDEO Number of good detections in J 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.

jnGoodObs videoVariability, vikingVariability, vmcVariability, vvvVariability VSAQC Number of good detections in J 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.

jNgt3sig videoVariability VSAVIDEO Number of good detections in J-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.

jNgt3sig videoVariability, vikingVariability, vmcVariability, vvvVariability VSAQC Number of good detections in J-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.

jnMissingObs videoVariability VSAVIDEO Number of J 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.

jnMissingObs videoVariability, vikingVariability, vmcVariability, vvvVariability VSAQC Number of J 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.

joinCriterion RequiredNeighbours VSAQC the join criterion (search radius for matches) real 4 arcminutes ??

joinCriterion RequiredNeighbours VSASVNGC253 the join criterion (search radius for matches) real 4 arcminutes ??

joinCriterion RequiredNeighbours VSASVORION the join criterion (search radius for matches) real 4 arcminutes ??

joinCriterion RequiredNeighbours VSAUltraVISTA the join criterion (search radius for matches) real 4 arcminutes ??

joinCriterion RequiredNeighbours VSAVHS the join criterion (search radius for matches) real 4 arcminutes ??

joinCriterion RequiredNeighbours VSAVIDEO the join criterion (search radius for matches) real 4 arcminutes ??

joinCriterion RequiredNeighbours VSAVIKING the join criterion (search radius for matches) real 4 arcminutes ??

joinCriterion RequiredNeighbours VSAVMC the join criterion (search radius for matches) real 4 arcminutes ??

joinCriterion RequiredNeighbours VSAVVV the join criterion (search radius for matches) real 4 arcminutes ??

JON grs_ngpSource, grs_ranSource, grs_sgpSource TWODFGRS Eyeball classification, value > 0 only for galaxies brighter than about 18th mag: 0 = noise; 1 = S0; 2 = elliptical; 3 = spiral; 4 = irregular; 5 = undetermined galaxy; 6 = star; 7 = star + star merger; 8 = galaxy + star merger; 9 = galaxy + galaxy merger int 4

jPA svNgc253Source VSASVNGC253 ellipse fit celestial orientation in J real 4 Degrees -0.9999995e9 POS_POS-ANG

jPA svOrionSource VSASVORION ellipse fit celestial orientation in J real 4 Degrees -0.9999995e9 POS_POS-ANG

jPA ultravistaSource VSAUltraVISTA ellipse fit celestial orientation in J real 4 Degrees -0.9999995e9 POS_POS-ANG

jPA ultravistaSource, ultravistaSourceRemeasurement, vhsSource, vhsSourceRemeasurement, videoSource, videoSourceRemeasurement, vikingSource, vikingSourceRemeasurement, vmcSource, vmcSourceRemeasurement, vmcSynopticSource, vvvSource, vvvSourceRemeasurement VSAQC ellipse fit celestial orientation in J real 4 Degrees -0.9999995e9 POS_POS-ANG

jPetroMag svNgc253Source VSASVNGC253 Extended source J mag (Petrosian) real 4 mag -0.9999995e9 PHOT_MAG

jPetroMag svOrionSource VSASVORION Extended source J mag (Petrosian) real 4 mag -0.9999995e9 PHOT_MAG

jPetroMag ultravistaSource VSAUltraVISTA Extended source J mag (Petrosian) real 4 mag -0.9999995e9 PHOT_MAG

jPetroMag ultravistaSource, vhsSource, videoSource, vikingSource, vmcSource VSAQC Extended source J mag (Petrosian) real 4 mag -0.9999995e9 PHOT_MAG

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

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

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

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

jppErrBits svNgc253Source VSASVNGC253 additional WFAU post-processing error bits in J 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.

jppErrBits svOrionSource VSASVORION additional WFAU post-processing error bits in J 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.

jppErrBits ultravistaSource VSAUltraVISTA additional WFAU post-processing error bits in J int 4 0 CODE_MISC

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

jppErrBits vhsSource VSAVHS additional WFAU post-processing error bits in J 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.

jppErrBits vhsSource, vikingSource, vmcSource, vmcSynopticSource VSAQC additional WFAU post-processing error bits in J 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.

jprobVar 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.

jprobVar videoVariability, vikingVariability, vmcVariability, 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.

jPsfMag svNgc253Source VSASVNGC253 Point source profile-fitted J mag real 4 mag -0.9999995e9 PHOT_MAG

jPsfMag svOrionSource VSASVORION Point source profile-fitted J mag real 4 mag -0.9999995e9 PHOT_MAG

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

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

jPsfMag vhsSource VSAVHS Point source profile-fitted J mag real 4 mag -0.9999995e9 PHOT_MAG

jPsfMag vhsSource, vikingSource, vmcSource VSAQC Point source profile-fitted J mag real 4 mag -0.9999995e9 PHOT_MAG

jPsfMagErr svNgc253Source VSASVNGC253 Error in point source profile-fitted J mag real 4 mag -0.9999995e9 ERROR

jPsfMagErr svOrionSource VSASVORION Error in point source profile-fitted J mag real 4 mag -0.9999995e9 ERROR

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

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

jPsfMagErr vhsSource VSAVHS Error in point source profile-fitted J mag real 4 mag -0.9999995e9 ERROR

jPsfMagErr vhsSource, vikingSource, vmcSource VSAQC Error in point source profile-fitted J mag real 4 mag -0.9999995e9 ERROR

jSeqNum svNgc253Source VSASVNGC253 the running number of the J detection int 4 -99999999 ID_NUMBER

jSeqNum svOrionSource VSASVORION the running number of the J detection int 4 -99999999 ID_NUMBER

jSeqNum ultravistaSource VSAUltraVISTA the running number of the J detection int 4 -99999999 ID_NUMBER

jSeqNum ultravistaSource, vhsSource, videoSource, vikingSource, vmcSource, vmcSynopticSource, vvvSource VSAQC the running number of the J detection int 4 -99999999 ID_NUMBER

jSeqNum ultravistaSourceRemeasurement VSAUltraVISTA the running number of the J remeasurement int 4 -99999999 ID_NUMBER

jSeqNum ultravistaSourceRemeasurement, vhsSourceRemeasurement, videoSourceRemeasurement, vikingSourceRemeasurement, vmcSourceRemeasurement, vvvSourceRemeasurement VSAQC the running number of the J remeasurement int 4 -99999999 ID_NUMBER

jSerMag2D svNgc253Source VSASVNGC253 Extended source J mag (profile-fitted) real 4 mag -0.9999995e9 PHOT_MAG

jSerMag2D svOrionSource VSASVORION Extended source J mag (profile-fitted) real 4 mag -0.9999995e9 PHOT_MAG

jSerMag2D ultravistaSource VSAUltraVISTA Not available in SE output real 4 mag -0.9999995e9 PHOT_MAG

jSerMag2D ultravistaSource, videoSource VSAQC Not available in SE output real 4 mag -0.9999995e9 PHOT_MAG

jSerMag2D vhsSource VSAVHS Extended source J mag (profile-fitted) real 4 mag -0.9999995e9 PHOT_MAG

jSerMag2D vhsSource, vikingSource, vmcSource VSAQC Extended source J mag (profile-fitted) real 4 mag -0.9999995e9 PHOT_MAG

jSerMag2DErr svNgc253Source VSASVNGC253 Error in extended source J mag (profile-fitted) real 4 mag -0.9999995e9 ERROR

jSerMag2DErr svOrionSource VSASVORION Error in extended source J mag (profile-fitted) real 4 mag -0.9999995e9 ERROR

jSerMag2DErr ultravistaSource VSAUltraVISTA Not available in SE output real 4 mag -0.9999995e9 ERROR

jSerMag2DErr ultravistaSource, videoSource VSAQC Not available in SE output real 4 mag -0.9999995e9 ERROR

jSerMag2DErr vhsSource VSAVHS Error in extended source J mag (profile-fitted) real 4 mag -0.9999995e9 ERROR

jSerMag2DErr vhsSource, vikingSource, vmcSource VSAQC Error in extended source J mag (profile-fitted) real 4 mag -0.9999995e9 ERROR

jskewness videoVariability VSAVIDEO Skewness in J 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.

jskewness videoVariability, vikingVariability, vmcVariability, vvvVariability VSAQC Skewness in J 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.

jtotalPeriod 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.

jtotalPeriod videoVariability, vikingVariability, vmcVariability, 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.

julianDayNum Multiframe VSASVNGC253 The Julian Day number of the VISTA night int 4 Julian days TIME_DATE

julianDayNum Multiframe VSASVORION The Julian Day number of the VISTA night int 4 Julian days TIME_DATE

julianDayNum Multiframe VSAUltraVISTA The Julian Day number of the VISTA night int 4 Julian days TIME_DATE

julianDayNum Multiframe VSAVHS The Julian Day number of the VISTA night int 4 Julian days TIME_DATE

julianDayNum Multiframe VSAVIDEO The Julian Day number of the VISTA night int 4 Julian days TIME_DATE

julianDayNum Multiframe VSAVIKING The Julian Day number of the VISTA night int 4 Julian days TIME_DATE

julianDayNum Multiframe VSAVMC The Julian Day number of the VISTA night int 4 Julian days TIME_DATE

julianDayNum Multiframe VSAVVV The Julian Day number of the VISTA night int 4 Julian days TIME_DATE

julianDayNum MultiframeDetector VSASVNGC253 The Julian Day number of the VISTA night {image primary HDU keyword: DATE-OBS} int 4 Julian days TIME_DATE

julianDayNum MultiframeDetector VSASVORION The Julian Day number of the VISTA night {image primary HDU keyword: DATE-OBS} int 4 Julian days TIME_DATE

julianDayNum MultiframeDetector VSAUltraVISTA The Julian Day number of the VISTA night {image primary HDU keyword: DATE-OBS} int 4 Julian days TIME_DATE

julianDayNum MultiframeDetector VSAVHS The Julian Day number of the VISTA night {image primary HDU keyword: DATE-OBS} int 4 Julian days TIME_DATE

julianDayNum MultiframeDetector VSAVIDEO The Julian Day number of the VISTA night {image primary HDU keyword: DATE-OBS} int 4 Julian days TIME_DATE

julianDayNum MultiframeDetector VSAVIKING The Julian Day number of the VISTA night {image primary HDU keyword: DATE-OBS} int 4 Julian days TIME_DATE

julianDayNum MultiframeDetector VSAVMC The Julian Day number of the VISTA night {image primary HDU keyword: DATE-OBS} int 4 Julian days TIME_DATE

julianDayNum MultiframeDetector VSAVVV The Julian Day number of the VISTA night {image primary HDU keyword: DATE-OBS} int 4 Julian days TIME_DATE

julianDayNum ultravistaMultiframe, ultravistaMultiframeDetector, vhsMultiframe, vhsMultiframeDetector, videoMultiframe, videoMultiframeDetector, vikingMultiframe, vikingMultiframeDetector, vmcMultiframe, vmcMultiframeDetector, vvvMultiframe, vvvMultiframeDetector VSAQC The Julian Day number of the VISTA night int 4 Julian days TIME_DATE

jVarClass 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.

jVarClass videoVariability, vikingVariability, vmcVariability, 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.

jXi svNgc253Source VSASVNGC253 Offset of J 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.

jXi svOrionSource VSASVORION Offset of J 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.

jXi ultravistaSource VSAUltraVISTA Offset of J 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.

jXi ultravistaSource, vhsSource, videoSource, vikingSource, vmcSource, vmcSynopticSource, vvvSource VSAQC Offset of J 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