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Glossary of VSA attributes

This Glossary alphabetically lists all attributes used in the VSAv20181120 database(s) held in the VSA. If you would like to have more information about the schema tables please use the VSAv20181120 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

K

NameSchema TableDatabaseDescriptionTypeLengthUnitDefault ValueUnified Content Descriptor
K twomass SIXDF K magnitude (corrected) used for K selection real 4 mag    
k_2mrat twomass_scn TWOMASS Ks-band average 2nd image moment ratio. real 4     stat.fit.param
k_2mrat twomass_sixx2_scn TWOMASS K band average 2nd image moment ratio for scan real 4      
k_5sig_ba twomass_xsc TWOMASS K minor/major axis ratio fit to the 5-sigma isophote. real 4     phys.size.axisRatio
k_5sig_phi twomass_xsc TWOMASS K angle to 5-sigma major axis (E of N). smallint 2 degrees   stat.error
k_5surf twomass_xsc TWOMASS K central surface brightness (r<=5). real 4 mag   phot.mag.sb
k_ba twomass_sixx2_xsc TWOMASS K minor/major axis ratio fit to the 3-sigma isophote real 4      
k_ba twomass_xsc TWOMASS K minor/major axis ratio fit to the 3-sigma isophote. real 4     phys.size.axisRatio
k_back twomass_xsc TWOMASS K coadd median background. real 4     meta.code
k_bisym_chi twomass_xsc TWOMASS K bi-symmetric cross-correlation chi. real 4     stat.fit.param
k_bisym_rat twomass_xsc TWOMASS K bi-symmetric flux ratio. real 4     phot.flux;arith.ratio
k_bndg_amp twomass_xsc TWOMASS K banding maximum FT amplitude on this side of coadd. real 4 DN   stat.fit.param
k_bndg_per twomass_xsc TWOMASS K banding Fourier Transf. period on this side of coadd. int 4 arcsec   stat.fit.param
k_chif_ellf twomass_xsc TWOMASS K % chi-fraction for elliptical fit to 3-sig isophote. real 4     stat.fit.param
k_cmsig twomass_psc TWOMASS Corrected photometric uncertainty for the default Ks-band magnitude. real 4 mag Ks-band phot.flux
k_con_indx twomass_xsc TWOMASS K concentration index r_75%/r_25%. real 4     phys.size;arith.ratio
k_d_area twomass_xsc TWOMASS K 5-sigma to 3-sigma differential area. smallint 2     stat.fit.residual
k_flg_10 twomass_xsc TWOMASS K confusion flag for 10 arcsec circular ap. mag. smallint 2     meta.code
k_flg_15 twomass_xsc TWOMASS K confusion flag for 15 arcsec circular ap. mag. smallint 2     meta.code
k_flg_20 twomass_xsc TWOMASS K confusion flag for 20 arcsec circular ap. mag. smallint 2     meta.code
k_flg_25 twomass_xsc TWOMASS K confusion flag for 25 arcsec circular ap. mag. smallint 2     meta.code
k_flg_30 twomass_xsc TWOMASS K confusion flag for 30 arcsec circular ap. mag. smallint 2     meta.code
k_flg_40 twomass_xsc TWOMASS K confusion flag for 40 arcsec circular ap. mag. smallint 2     meta.code
k_flg_5 twomass_xsc TWOMASS K confusion flag for 5 arcsec circular ap. mag. smallint 2     meta.code
k_flg_50 twomass_xsc TWOMASS K confusion flag for 50 arcsec circular ap. mag. smallint 2     meta.code
k_flg_60 twomass_xsc TWOMASS K confusion flag for 60 arcsec circular ap. mag. smallint 2     meta.code
k_flg_7 twomass_sixx2_xsc TWOMASS K confusion flag for 7 arcsec circular ap. mag smallint 2      
k_flg_7 twomass_xsc TWOMASS K confusion flag for 7 arcsec circular ap. mag. smallint 2     meta.code
k_flg_70 twomass_xsc TWOMASS K confusion flag for 70 arcsec circular ap. mag. smallint 2     meta.code
k_flg_c twomass_xsc TWOMASS K confusion flag for Kron circular mag. smallint 2     meta.code
k_flg_e twomass_xsc TWOMASS K confusion flag for Kron elliptical mag. smallint 2     meta.code
k_flg_fc twomass_xsc TWOMASS K confusion flag for fiducial Kron circ. mag. smallint 2     meta.code
k_flg_fe twomass_xsc TWOMASS K confusion flag for fiducial Kron ell. mag. smallint 2     meta.code
k_flg_i20c twomass_xsc TWOMASS K confusion flag for 20mag/sq." iso. circ. mag. smallint 2     meta.code
k_flg_i20e twomass_xsc TWOMASS K confusion flag for 20mag/sq." iso. ell. mag. smallint 2     meta.code
k_flg_i21c twomass_xsc TWOMASS K confusion flag for 21mag/sq." iso. circ. mag. smallint 2     meta.code
k_flg_i21e twomass_xsc TWOMASS K confusion flag for 21mag/sq." iso. ell. mag. smallint 2     meta.code
k_flg_j21fc twomass_xsc TWOMASS K confusion flag for 21mag/sq." iso. fid. circ. mag. smallint 2     meta.code
k_flg_j21fe twomass_xsc TWOMASS K confusion flag for 21mag/sq." iso. fid. ell. mag. smallint 2     meta.code
k_flg_k20fc twomass_xsc TWOMASS K confusion flag for 20mag/sq." iso. fid. circ. mag. smallint 2     meta.code
k_flg_k20fe twomass_sixx2_xsc TWOMASS K confusion flag for 20mag/sq.″ iso. fid. ell. mag smallint 2      
k_flg_k20fe twomass_xsc TWOMASS K confusion flag for 20mag/sq." iso. fid. ell. mag. smallint 2     meta.code
k_m twomass_psc TWOMASS Default Ks-band magnitude real 4 mag   phot.flux
k_m twomass_sixx2_psc TWOMASS K selected "default" magnitude real 4 mag    
k_m_10 twomass_xsc TWOMASS K 10 arcsec radius circular aperture magnitude. real 4 mag   phot.flux
k_m_15 twomass_xsc TWOMASS K 15 arcsec radius circular aperture magnitude. real 4 mag   phot.flux
k_m_20 twomass_xsc TWOMASS K 20 arcsec radius circular aperture magnitude. real 4 mag   phot.flux
k_m_25 twomass_xsc TWOMASS K 25 arcsec radius circular aperture magnitude. real 4 mag   phot.flux
k_m_2mass allwise_sc2 WISE 2MASS Ks-band magnitude of the associated 2MASS PSC source. This column is "null" if there is no associated 2MASS PSC source or if the 2MASS PSC Ks-band magnitude entry is "null". float 8 mag    
k_m_30 twomass_xsc TWOMASS K 30 arcsec radius circular aperture magnitude. real 4 mag   phot.flux
k_m_40 twomass_xsc TWOMASS K 40 arcsec radius circular aperture magnitude. real 4 mag   phot.flux
k_m_5 twomass_xsc TWOMASS K 5 arcsec radius circular aperture magnitude. real 4 mag   phot.flux
k_m_50 twomass_xsc TWOMASS K 50 arcsec radius circular aperture magnitude. real 4 mag   phot.flux
k_m_60 twomass_xsc TWOMASS K 60 arcsec radius circular aperture magnitude. real 4 mag   phot.flux
k_m_7 twomass_sixx2_xsc TWOMASS K 7 arcsec radius circular aperture magnitude real 4 mag    
k_m_7 twomass_xsc TWOMASS K 7 arcsec radius circular aperture magnitude. real 4 mag   phot.flux
k_m_70 twomass_xsc TWOMASS K 70 arcsec radius circular aperture magnitude. real 4 mag   phot.flux
k_m_c twomass_xsc TWOMASS K Kron circular aperture magnitude. real 4 mag   phot.flux
k_m_e twomass_xsc TWOMASS K Kron elliptical aperture magnitude. real 4 mag   phot.flux
k_m_ext twomass_sixx2_xsc TWOMASS K mag from fit extrapolation real 4 mag    
k_m_ext twomass_xsc TWOMASS K mag from fit extrapolation. real 4 mag   phot.flux
k_m_fc twomass_xsc TWOMASS K fiducial Kron circular magnitude. real 4 mag   phot.flux
k_m_fe twomass_xsc TWOMASS K fiducial Kron ell. mag aperture magnitude. real 4 mag   phot.flux
k_m_i20c twomass_xsc TWOMASS K 20mag/sq." isophotal circular ap. magnitude. real 4 mag   phot.flux
k_m_i20e twomass_xsc TWOMASS K 20mag/sq." isophotal elliptical ap. magnitude. real 4 mag   phot.flux
k_m_i21c twomass_xsc TWOMASS K 21mag/sq." isophotal circular ap. magnitude. real 4 mag   phot.flux
k_m_i21e twomass_xsc TWOMASS K 21mag/sq." isophotal elliptical ap. magnitude. real 4 mag   phot.flux
k_m_j21fc twomass_xsc TWOMASS K 21mag/sq." isophotal fiducial circ. ap. mag. real 4 mag   phot.flux
k_m_j21fe twomass_xsc TWOMASS K 21mag/sq." isophotal fiducial ell. ap. magnitude. real 4 mag   phot.flux
k_m_k20fc twomass_xsc TWOMASS K 20mag/sq." isophotal fiducial circ. ap. mag. real 4 mag   phot.flux
K_M_K20FE twomass SIXDF K 20mag/sq." isophotal fiducial ell. ap. magnitude real 4 mag    
k_m_k20fe twomass_sixx2_xsc TWOMASS K 20mag/sq.″ isophotal fiducial ell. ap. magnitude real 4 mag    
k_m_k20fe twomass_xsc TWOMASS K 20mag/sq." isophotal fiducial ell. ap. magnitude. real 4 mag   phot.flux
k_m_stdap twomass_psc TWOMASS Ks-band "standard" aperture magnitude. real 4 mag   phot.flux
k_m_sys twomass_xsc TWOMASS K system photometry magnitude. real 4 mag   phot.flux
k_mnsurfb_eff twomass_xsc TWOMASS K mean surface brightness at the half-light radius. real 4 mag   phot.mag.sb
k_msig twomass_sixx2_psc TWOMASS K "default" mag uncertainty real 4 mag    
k_msig_10 twomass_xsc TWOMASS K 1-sigma uncertainty in 10 arcsec circular ap. mag. real 4 mag   stat.error
k_msig_15 twomass_xsc TWOMASS K 1-sigma uncertainty in 15 arcsec circular ap. mag. real 4 mag   stat.error
k_msig_20 twomass_xsc TWOMASS K 1-sigma uncertainty in 20 arcsec circular ap. mag. real 4 mag   stat.error
k_msig_25 twomass_xsc TWOMASS K 1-sigma uncertainty in 25 arcsec circular ap. mag. real 4 mag   stat.error
k_msig_2mass allwise_sc2 WISE 2MASS Ks-band corrected photometric uncertainty of the associated 2MASS PSC source. This column is "null" if there is no associated 2MASS PSC source or if the 2MASS PSC Ks-band uncertainty entry is "null". float 8 mag    
k_msig_30 twomass_xsc TWOMASS K 1-sigma uncertainty in 30 arcsec circular ap. mag. real 4 mag   stat.error
k_msig_40 twomass_xsc TWOMASS K 1-sigma uncertainty in 40 arcsec circular ap. mag. real 4 mag   stat.error
k_msig_5 twomass_xsc TWOMASS K 1-sigma uncertainty in 5 arcsec circular ap. mag. real 4 mag   stat.error
k_msig_50 twomass_xsc TWOMASS K 1-sigma uncertainty in 50 arcsec circular ap. mag. real 4 mag   stat.error
k_msig_60 twomass_xsc TWOMASS K 1-sigma uncertainty in 60 arcsec circular ap. mag. real 4 mag   stat.error
k_msig_7 twomass_sixx2_xsc TWOMASS K 1-sigma uncertainty in 7 arcsec circular ap. mag real 4 mag    
k_msig_7 twomass_xsc TWOMASS K 1-sigma uncertainty in 7 arcsec circular ap. mag. real 4 mag   stat.error
k_msig_70 twomass_xsc TWOMASS K 1-sigma uncertainty in 70 arcsec circular ap. mag. real 4 mag   stat.error
k_msig_c twomass_xsc TWOMASS K 1-sigma uncertainty in Kron circular mag. real 4 mag   stat.error
k_msig_e twomass_xsc TWOMASS K 1-sigma uncertainty in Kron elliptical mag. real 4 mag   stat.error
k_msig_ext twomass_sixx2_xsc TWOMASS K 1-sigma uncertainty in mag from fit extrapolation real 4 mag    
k_msig_ext twomass_xsc TWOMASS K 1-sigma uncertainty in mag from fit extrapolation. real 4 mag   stat.error
k_msig_fc twomass_xsc TWOMASS K 1-sigma uncertainty in fiducial Kron circ. mag. real 4 mag   stat.error
k_msig_fe twomass_xsc TWOMASS K 1-sigma uncertainty in fiducial Kron ell. mag. real 4 mag   stat.error
k_msig_i20c twomass_xsc TWOMASS K 1-sigma uncertainty in 20mag/sq." iso. circ. mag. real 4 mag   stat.error
k_msig_i20e twomass_xsc TWOMASS K 1-sigma uncertainty in 20mag/sq." iso. ell. mag. real 4 mag   stat.error
k_msig_i21c twomass_xsc TWOMASS K 1-sigma uncertainty in 21mag/sq." iso. circ. mag. real 4 mag   stat.error
k_msig_i21e twomass_xsc TWOMASS K 1-sigma uncertainty in 21mag/sq." iso. ell. mag. real 4 mag   stat.error
k_msig_j21fc twomass_xsc TWOMASS K 1-sigma uncertainty in 21mag/sq." iso.fid.circ.mag. real 4 mag   stat.error
k_msig_j21fe twomass_xsc TWOMASS K 1-sigma uncertainty in 21mag/sq." iso.fid.ell.mag. real 4 mag   stat.error
k_msig_k20fc twomass_xsc TWOMASS K 1-sigma uncertainty in 20mag/sq." iso.fid.circ. mag. real 4 mag   stat.error
k_msig_k20fe twomass_sixx2_xsc TWOMASS K 1-sigma uncertainty in 20mag/sq.″ iso.fid.ell.mag real 4 mag    
k_msig_k20fe twomass_xsc TWOMASS K 1-sigma uncertainty in 20mag/sq." iso.fid.ell.mag. real 4 mag   stat.error
k_msig_stdap twomass_psc TWOMASS Uncertainty in the Ks-band standard aperture magnitude. real 4 mag   phot.flux
k_msig_sys twomass_xsc TWOMASS K 1-sigma uncertainty in system photometry mag. real 4 mag   stat.error
k_msigcom twomass_psc TWOMASS Combined, or total photometric uncertainty for the default Ks-band magnitude. real 4 mag Ks-band phot.flux
k_msigcom twomass_sixx2_psc TWOMASS combined (total) K band photometric uncertainty real 4 mag    
k_msnr10 twomass_scn TWOMASS The estimated Ks-band magnitude at which SNR=10 is achieved for this scan. real 4 mag   phot.flux
k_msnr10 twomass_sixx2_scn TWOMASS K mag at which SNR=10 is achieved, from k_psp and k_zp_ap real 4 mag    
k_n_snr10 twomass_scn TWOMASS Number of point sources at Ks-band with SNR>10 (instrumental mag <=14.3) int 4     meta.number
k_n_snr10 twomass_sixx2_scn TWOMASS number of K point sources with SNR>10 (instrumental m<=14.3) int 4      
k_pchi twomass_xsc TWOMASS K chi^2 of fit to rad. profile (LCSB: alpha scale len). real 4     stat.fit.param
k_peak twomass_xsc TWOMASS K peak pixel brightness. real 4 mag   phot.mag.sb
k_perc_darea twomass_xsc TWOMASS K 5-sigma to 3-sigma percent area change. smallint 2     FIT_PARAM
k_phi twomass_sixx2_xsc TWOMASS K angle to 3-sigma major axis (E of N) smallint 2 deg    
k_phi twomass_xsc TWOMASS K angle to 3-sigma major axis (E of N). smallint 2 degrees   pos.posAng
k_psfchi twomass_psc TWOMASS Reduced chi-squared goodness-of-fit value for the Ks-band profile-fit photometry made on the 1.3 s "Read_2" exposures. real 4     stat.fit.param
k_psp twomass_scn TWOMASS Ks-band photometric sensitivity paramater (PSP). real 4     instr.sensitivity
k_psp twomass_sixx2_scn TWOMASS K photometric sensitivity param: k_shape_avg*(k_fbg_avg^.29) real 4      
k_pts_noise twomass_scn TWOMASS Base-10 logarithm of the mode of the noise distribution for all point source detections in the scan, where the noise is estimated from the measured Ks-band photometric errors and is expressed in units of mJy. real 4     instr.det.noise
k_pts_noise twomass_sixx2_scn TWOMASS log10 of K band modal point src noise estimate real 4 logmJy    
k_r_c twomass_xsc TWOMASS K Kron circular aperture radius. real 4 arcsec   phys.angSize;src
k_r_e twomass_xsc TWOMASS K Kron elliptical aperture semi-major axis. real 4 arcsec   phys.angSize;src
k_r_eff twomass_xsc TWOMASS K half-light (integrated half-flux point) radius. real 4 arcsec   phys.angSize;src
k_r_i20c twomass_xsc TWOMASS K 20mag/sq." isophotal circular aperture radius. real 4 arcsec   phys.angSize;src
k_r_i20e twomass_xsc TWOMASS K 20mag/sq." isophotal elliptical ap. semi-major axis. real 4 arcsec   phys.angSize;src
k_r_i21c twomass_xsc TWOMASS K 21mag/sq." isophotal circular aperture radius. real 4 arcsec   phys.angSize;src
k_r_i21e twomass_xsc TWOMASS K 21mag/sq." isophotal elliptical ap. semi-major axis. real 4 arcsec   phys.angSize;src
k_resid_ann twomass_xsc TWOMASS K residual annulus background median. real 4 DN   meta.code
k_sc_1mm twomass_xsc TWOMASS K 1st moment (score) (LCSB: super blk 2,4,8 SNR). real 4     meta.code
k_sc_2mm twomass_xsc TWOMASS K 2nd moment (score) (LCSB: SNRMAX - super SNR max). real 4     meta.code
k_sc_msh twomass_xsc TWOMASS K median shape score. real 4     meta.code
k_sc_mxdn twomass_xsc TWOMASS K mxdn (score) (LCSB: BSNR - block/smoothed SNR). real 4     meta.code
k_sc_r1 twomass_xsc TWOMASS K r1 (score). real 4     meta.code
k_sc_r23 twomass_xsc TWOMASS K r23 (score) (LCSB: TSNR - integrated SNR for r=15). real 4     meta.code
k_sc_sh twomass_xsc TWOMASS K shape (score). real 4     meta.code
k_sc_vint twomass_xsc TWOMASS K vint (score). real 4     meta.code
k_sc_wsh twomass_xsc TWOMASS K wsh (score) (LCSB: PSNR - peak raw SNR). real 4     meta.code
k_seetrack twomass_xsc TWOMASS K band seetracking score. real 4     meta.code
k_sh0 twomass_xsc TWOMASS K ridge shape (LCSB: BSNR limit). real 4     FIT_PARAM
k_shape_avg twomass_scn TWOMASS Ks-band average seeing shape for scan. real 4     instr.obsty.seeing
k_shape_avg twomass_sixx2_scn TWOMASS K band average seeing shape for scan real 4      
k_shape_rms twomass_scn TWOMASS RMS-error of Ks-band average seeing shape. real 4     instr.obsty.seeing
k_shape_rms twomass_sixx2_scn TWOMASS rms of K band avg seeing shape for scan real 4      
k_sig_sh0 twomass_xsc TWOMASS K ridge shape sigma (LCSB: B2SNR limit). real 4     FIT_PARAM
k_snr twomass_psc TWOMASS Ks-band "scan" signal-to-noise ratio. real 4 mag   instr.det.noise
k_snr twomass_sixx2_psc TWOMASS K band "scan" signal-to-noise ratio real 4      
k_subst2 twomass_xsc TWOMASS K residual background #2 (score). real 4     meta.code
k_zp_ap twomass_scn TWOMASS Photometric zero-point for Ks-band aperture photometry. real 4 mag   phot.mag;arith.zp
k_zp_ap twomass_sixx2_scn TWOMASS K band ap. calibration photometric zero-point for scan real 4 mag    
k_zperr_ap twomass_scn TWOMASS RMS-error of zero-point for Ks-band aperture photometry real 4 mag   stat.error
k_zperr_ap twomass_sixx2_scn TWOMASS K band ap. calibration rms error of zero-point for scan real 4 mag    
KBESTR spectra SIXDF cross-correlation template int 4      
kCorr twompzPhotoz TWOMPZ K 20mag/sq." isophotal fiducial ell. ap. magnitude with Galactic dust correction {image primary HDU keyword: Kcorr} real 4 mag -0.9999995e9 phot.mag;em.IR.K
kCorrErr twompzPhotoz TWOMPZ K 1-sigma uncertainty in 20mag/sq." aperture {image primary HDU keyword: k_msig_k20fe} real 4 mag -0.9999995e9  
KEXT twomass SIXDF KEXT magnitude real 4 mag    
KEXT_K twomass SIXDF KEXT minus K (corrected) real 4 mag    
Kmag mcps_lmcSource, mcps_smcSource MCPS The K' band magnitude (from 2MASS) (0.00 if star not detected.) real 4 mag    
kMag ukirtFSstars VIDEOv20100513 K band total magnitude on the MKO(UFTI) system real 4 mag   phot.mag
kMag ukirtFSstars VIKINGv20110714 K band total magnitude on the MKO(UFTI) system real 4 mag   phot.mag
Kmag2MASS spitzer_smcSource SPITZER The 2MASS K band magnitude. real 4 mag    
Kmag_2MASS ravedr5Source RAVE K selected default magnitude from 2MASS real 4 mag magnitude phot.mag;em.IR.K
Kmag_DENIS ravedr5Source RAVE K selected default magnitude real 4 mag magnitude phot.mag;em.IR.K
kMagErr ukirtFSstars VIDEOv20100513 K band magnitude error real 4 mag   stat.error
kMagErr ukirtFSstars VIKINGv20110714 K band magnitude error real 4 mag   stat.error
kronFlux vhsDetection VHSDR2 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count;em.opt
kronFlux vhsDetection VHSDR3 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vhsDetection VHSDR4 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vhsDetection VHSv20120926 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vhsDetection VHSv20130417 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vhsDetection VHSv20140409 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vhsDetection VHSv20150108 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vhsDetection VHSv20160114 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vhsDetection VHSv20160507 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vhsDetection VHSv20170630 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vhsDetection VHSv20171207 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vhsDetection VHSv20180419 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vhsDetection, vhsListRemeasurement VHSDR1 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count;em.opt
kronFlux videoDetection VIDEODR2 flux within Kron radius circular aperture (SE: FLUX_AUTO) {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count;em.opt
kronFlux videoDetection VIDEODR3 flux within Kron radius circular aperture (SE: FLUX_AUTO) {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux videoDetection VIDEODR4 flux within Kron radius circular aperture (SE: FLUX_AUTO) {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux videoDetection VIDEODR5 flux within Kron radius circular aperture (SE: FLUX_AUTO) {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux videoDetection VIDEOv20100513 flux within Kron radius circular aperture (SE: FLUX_AUTO) {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count;em.opt
kronFlux videoDetection VIDEOv20111208 flux within Kron radius circular aperture (SE: FLUX_AUTO) {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count;em.opt
kronFlux videoListRemeasurement VIDEOv20100513 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count;em.opt
kronFlux vikingDetection VIKINGDR2 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count;em.opt
kronFlux vikingDetection VIKINGDR3 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vikingDetection VIKINGDR4 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vikingDetection VIKINGv20111019 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count;em.opt
kronFlux vikingDetection VIKINGv20130417 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vikingDetection VIKINGv20140402 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vikingDetection VIKINGv20150421 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vikingDetection VIKINGv20151230 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vikingDetection VIKINGv20160406 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vikingDetection VIKINGv20161202 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vikingDetection VIKINGv20170715 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vikingDetection VIKINGv20181012 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vikingDetection, vikingListRemeasurement VIKINGv20110714 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count;em.opt
kronFlux vikingMapRemeasurement VIKINGZYSELJv20160909 flux within Kron radius circular aperture (SE: FLUX_AUTO; CASU: default) {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count;em.opt
kronFlux vikingMapRemeasurement VIKINGZYSELJv20170124 flux within Kron radius circular aperture (SE: FLUX_AUTO; CASU: default) {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count;em.opt
kronFlux vmcDetection VMCDR1 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count;em.opt
kronFlux vmcDetection VMCDR2 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vmcDetection VMCDR3 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vmcDetection VMCDR4 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vmcDetection VMCv20110909 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count;em.opt
kronFlux vmcDetection VMCv20120126 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count;em.opt
kronFlux vmcDetection VMCv20121128 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vmcDetection VMCv20130304 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vmcDetection VMCv20130805 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vmcDetection VMCv20140428 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vmcDetection VMCv20140903 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vmcDetection VMCv20150309 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vmcDetection VMCv20151218 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vmcDetection VMCv20160311 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vmcDetection VMCv20160822 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vmcDetection VMCv20170109 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vmcDetection VMCv20170411 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vmcDetection VMCv20171101 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vmcDetection VMCv20180702 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vmcDetection VMCv20181120 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFlux vmcDetection, vmcListRemeasurement VMCv20110816 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count;em.opt
kronFlux vvvDetection VVVDR4 flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU   phot.count
kronFluxErr vhsDetection VHSDR2 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vhsDetection VHSDR3 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vhsDetection VHSDR4 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vhsDetection VHSv20120926 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vhsDetection VHSv20130417 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vhsDetection VHSv20140409 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vhsDetection VHSv20150108 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vhsDetection VHSv20160114 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vhsDetection VHSv20160507 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vhsDetection VHSv20170630 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vhsDetection VHSv20171207 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vhsDetection VHSv20180419 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vhsDetection, vhsListRemeasurement VHSDR1 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr videoDetection VIDEODR2 error on Kron flux (SE: FLUXERR_AUTO) {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr videoDetection VIDEODR3 error on Kron flux (SE: FLUXERR_AUTO) {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr videoDetection VIDEODR4 error on Kron flux (SE: FLUXERR_AUTO) {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr videoDetection VIDEODR5 error on Kron flux (SE: FLUXERR_AUTO) {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr videoDetection VIDEOv20100513 error on Kron flux (SE: FLUXERR_AUTO) {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr videoDetection VIDEOv20111208 error on Kron flux (SE: FLUXERR_AUTO) {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr videoListRemeasurement VIDEOv20100513 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vikingDetection VIKINGDR2 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vikingDetection VIKINGDR3 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vikingDetection VIKINGDR4 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vikingDetection VIKINGv20111019 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vikingDetection VIKINGv20130417 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vikingDetection VIKINGv20140402 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vikingDetection VIKINGv20150421 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vikingDetection VIKINGv20151230 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vikingDetection VIKINGv20160406 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vikingDetection VIKINGv20161202 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vikingDetection VIKINGv20170715 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vikingDetection VIKINGv20181012 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vikingDetection, vikingListRemeasurement VIKINGv20110714 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vikingMapRemeasurement VIKINGZYSELJv20160909 error on Kron flux (SE: FLUXERR_AUTO; CASU: default) {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vikingMapRemeasurement VIKINGZYSELJv20170124 error on Kron flux (SE: FLUXERR_AUTO; CASU: default) {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vmcDetection VMCDR1 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vmcDetection VMCDR2 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vmcDetection VMCDR3 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vmcDetection VMCDR4 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vmcDetection VMCv20110909 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vmcDetection VMCv20120126 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vmcDetection VMCv20121128 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vmcDetection VMCv20130304 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vmcDetection VMCv20130805 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vmcDetection VMCv20140428 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vmcDetection VMCv20140903 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vmcDetection VMCv20150309 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vmcDetection VMCv20151218 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vmcDetection VMCv20160311 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vmcDetection VMCv20160822 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vmcDetection VMCv20170109 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vmcDetection VMCv20170411 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vmcDetection VMCv20171101 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vmcDetection VMCv20180702 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vmcDetection VMCv20181120 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vmcDetection, vmcListRemeasurement VMCv20110816 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronFluxErr vvvDetection VVVDR4 error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU   stat.error
kronJky vikingMapRemeasurement VIKINGZYSELJv20160909 Calibrated Kron flux within aperture r_k (CASU: default) real 4 jansky   phot.mag
kronJky vikingMapRemeasurement VIKINGZYSELJv20170124 Calibrated Kron flux within aperture r_k (CASU: default) real 4 jansky   phot.mag
kronJkyErr vikingMapRemeasurement VIKINGZYSELJv20160909 error on calibrated Kron flux real 4 jansky (CASU: default)   stat.error
kronJkyErr vikingMapRemeasurement VIKINGZYSELJv20170124 error on calibrated Kron flux real 4 jansky (CASU: default)   stat.error
kronLup vikingMapRemeasurement VIKINGZYSELJv20160909 Calibrated Kron luptitude within aperture r_k (CASU: default) real 4 lup   phot.mag
kronLup vikingMapRemeasurement VIKINGZYSELJv20170124 Calibrated Kron luptitude within aperture r_k (CASU: default) real 4 lup   phot.mag
kronLupErr vikingMapRemeasurement VIKINGZYSELJv20160909 error on calibrated Kron luptitude real 4 lup (CASU: default)   stat.error
kronLupErr vikingMapRemeasurement VIKINGZYSELJv20170124 error on calibrated Kron luptitude real 4 lup (CASU: default)   stat.error
kronMag vhsDetection VHSDR2 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vhsDetection VHSDR3 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vhsDetection VHSDR4 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vhsDetection VHSv20120926 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vhsDetection VHSv20130417 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vhsDetection VHSv20140409 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vhsDetection VHSv20150108 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vhsDetection VHSv20160114 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vhsDetection VHSv20160507 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vhsDetection VHSv20170630 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vhsDetection VHSv20171207 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vhsDetection VHSv20180419 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vhsDetection, vhsListRemeasurement VHSDR1 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag videoDetection VIDEODR2 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag videoDetection VIDEODR3 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag videoDetection VIDEODR4 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag videoDetection VIDEODR5 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag videoDetection VIDEOv20111208 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag videoDetection, videoListRemeasurement VIDEOv20100513 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vikingDetection VIKINGDR2 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vikingDetection VIKINGDR3 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vikingDetection VIKINGDR4 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vikingDetection VIKINGv20111019 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vikingDetection VIKINGv20130417 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vikingDetection VIKINGv20140402 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vikingDetection VIKINGv20150421 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vikingDetection VIKINGv20151230 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vikingDetection VIKINGv20160406 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vikingDetection VIKINGv20161202 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vikingDetection VIKINGv20170715 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vikingDetection VIKINGv20181012 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vikingDetection, vikingListRemeasurement VIKINGv20110714 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vikingMapRemeasurement VIKINGZYSELJv20160909 Calibrated Kron magnitude within aperture r_k (CASU: default) real 4 mag   phot.mag
kronMag vikingMapRemeasurement VIKINGZYSELJv20170124 Calibrated Kron magnitude within aperture r_k (CASU: default) real 4 mag   phot.mag
kronMag vmcDetection VMCDR1 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vmcDetection VMCDR2 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vmcDetection VMCDR3 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vmcDetection VMCDR4 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vmcDetection VMCv20110909 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vmcDetection VMCv20120126 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vmcDetection VMCv20121128 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vmcDetection VMCv20130304 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vmcDetection VMCv20130805 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vmcDetection VMCv20140428 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vmcDetection VMCv20140903 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vmcDetection VMCv20150309 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vmcDetection VMCv20151218 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vmcDetection VMCv20160311 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vmcDetection VMCv20160822 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vmcDetection VMCv20170109 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vmcDetection VMCv20170411 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vmcDetection VMCv20171101 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vmcDetection VMCv20180702 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vmcDetection VMCv20181120 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vmcDetection, vmcListRemeasurement VMCv20110816 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMag vvvDetection VVVDR4 Calibrated Kron magnitude within circular aperture r_k real 4 mag   phot.mag
kronMagErr vhsDetection VHSDR2 error on calibrated Kron magnitude real 4 mag   stat.error
kronMagErr vhsDetection VHSDR3 error on calibrated Kron magnitude real 4 mag   stat.error
kronMagErr vhsDetection VHSDR4 error on calibrated Kron magnitude real 4 mag   stat.error;phot.mag
kronMagErr vhsDetection VHSv20120926 error on calibrated Kron magnitude real 4 mag   stat.error
kronMagErr vhsDetection VHSv20130417 error on calibrated Kron magnitude real 4 mag   stat.error
kronMagErr vhsDetection VHSv20140409 error on calibrated Kron magnitude real 4 mag   stat.error
kronMagErr vhsDetection VHSv20150108 error on calibrated Kron magnitude real 4 mag   stat.error;phot.mag
kronMagErr vhsDetection VHSv20160114 error on calibrated Kron magnitude real 4 mag   stat.error;phot.mag
kronMagErr vhsDetection VHSv20160507 error on calibrated Kron magnitude real 4 mag   stat.error;phot.mag
kronMagErr vhsDetection VHSv20170630 error on calibrated Kron magnitude real 4 mag   stat.error;phot.mag
kronMagErr vhsDetection VHSv20171207 error on calibrated Kron magnitude real 4 mag   stat.error;phot.mag
kronMagErr vhsDetection VHSv20180419 error on calibrated Kron magnitude real 4 mag   stat.error;phot.mag
kronMagErr vhsDetection, vhsListRemeasurement VHSDR1 error on calibrated Kron magnitude real 4 mag   stat.error
kronMagErr videoDetection VIDEODR2 error on calibrated Kron magnitude real 4 mag   stat.error
kronMagErr videoDetection VIDEODR3 error on calibrated Kron magnitude real 4 mag   stat.error
kronMagErr videoDetection VIDEODR4 error on calibrated Kron magnitude real 4 mag   stat.error;phot.mag
kronMagErr videoDetection VIDEODR5 error on calibrated Kron magnitude real 4 mag   stat.error;phot.mag
kronMagErr videoDetection VIDEOv20111208 error on calibrated Kron magnitude real 4 mag   stat.error
kronMagErr videoDetection, videoListRemeasurement VIDEOv20100513 error on calibrated Kron magnitude real 4 mag   stat.error
kronMagErr vikingDetection VIKINGDR2 error on calibrated Kron magnitude real 4 mag   stat.error
kronMagErr vikingDetection VIKINGDR3 error on calibrated Kron magnitude real 4 mag   stat.error
kronMagErr vikingDetection VIKINGDR4 error on calibrated Kron magnitude real 4 mag   stat.error
kronMagErr vikingDetection VIKINGv20111019 error on calibrated Kron magnitude real 4 mag   stat.error
kronMagErr vikingDetection VIKINGv20130417 error on calibrated Kron magnitude real 4 mag   stat.error
kronMagErr vikingDetection VIKINGv20140402 error on calibrated Kron magnitude real 4 mag   stat.error
kronMagErr vikingDetection VIKINGv20150421 error on calibrated Kron magnitude real 4 mag   stat.error;phot.mag
kronMagErr vikingDetection VIKINGv20151230 error on calibrated Kron magnitude real 4 mag   stat.error;phot.mag
kronMagErr vikingDetection VIKINGv20160406 error on calibrated Kron magnitude real 4 mag   stat.error;phot.mag
kronMagErr vikingDetection VIKINGv20161202 error on calibrated Kron magnitude real 4 mag   stat.error;phot.mag
kronMagErr vikingDetection VIKINGv20170715 error on calibrated Kron magnitude real 4 mag   stat.error;phot.mag
kronMagErr vikingDetection VIKINGv20181012 error on calibrated Kron magnitude real 4 mag   stat.error;phot.mag
kronMagErr vikingDetection, vikingListRemeasurement VIKINGv20110714 error on calibrated Kron magnitude real 4 mag   stat.error
kronMagErr vikingMapRemeasurement VIKINGZYSELJv20160909 error on calibrated Kron magnitude real 4 mag (CASU: default)   stat.error
kronMagErr vikingMapRemeasurement VIKINGZYSELJv20170124 error on calibrated Kron magnitude real 4 mag (CASU: default)   stat.error
kronMagErr vmcDetection VMCDR1 error on calibrated Kron magnitude real 4 mag   stat.error
kronMagErr vmcDetection VMCDR2 error on calibrated Kron magnitude real 4 mag   stat.error
kronMagErr vmcDetection VMCDR3 error on calibrated Kron magnitude real 4 mag   stat.error;phot.mag
kronMagErr vmcDetection VMCDR4 error on calibrated Kron magnitude real 4 mag   stat.error;phot.mag
kronMagErr vmcDetection VMCv20110909 error on calibrated Kron magnitude real 4 mag   stat.error
kronMagErr vmcDetection VMCv20120126 error on calibrated Kron magnitude real 4 mag   stat.error
kronMagErr vmcDetection VMCv20121128 error on calibrated Kron magnitude real 4 mag   stat.error
kronMagErr vmcDetection VMCv20130304 error on calibrated Kron magnitude real 4 mag   stat.error
kronMagErr vmcDetection VMCv20130805 error on calibrated Kron magnitude real 4 mag   stat.error
kronMagErr vmcDetection VMCv20140428 error on calibrated Kron magnitude real 4 mag   stat.error
kronMagErr vmcDetection VMCv20140903 error on calibrated Kron magnitude real 4 mag   stat.error;phot.mag
kronMagErr vmcDetection VMCv20150309 error on calibrated Kron magnitude real 4 mag   stat.error;phot.mag
kronMagErr vmcDetection VMCv20151218 error on calibrated Kron magnitude real 4 mag   stat.error;phot.mag
kronMagErr vmcDetection VMCv20160311 error on calibrated Kron magnitude real 4 mag   stat.error;phot.mag
kronMagErr vmcDetection VMCv20160822 error on calibrated Kron magnitude real 4 mag   stat.error;phot.mag
kronMagErr vmcDetection VMCv20170109 error on calibrated Kron magnitude real 4 mag   stat.error;phot.mag
kronMagErr vmcDetection VMCv20170411 error on calibrated Kron magnitude real 4 mag   stat.error;phot.mag
kronMagErr vmcDetection VMCv20171101 error on calibrated Kron magnitude real 4 mag   stat.error;phot.mag
kronMagErr vmcDetection VMCv20180702 error on calibrated Kron magnitude real 4 mag   stat.error;phot.mag
kronMagErr vmcDetection VMCv20181120 error on calibrated Kron magnitude real 4 mag   stat.error;phot.mag
kronMagErr vmcDetection, vmcListRemeasurement VMCv20110816 error on calibrated Kron magnitude real 4 mag   stat.error
kronMagErr vvvDetection VVVDR4 error on calibrated Kron magnitude real 4 mag   stat.error;phot.mag
kronRad vhsDetection VHSDR2 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize;src
kronRad vhsDetection VHSDR3 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vhsDetection VHSDR4 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vhsDetection VHSv20120926 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vhsDetection VHSv20130417 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vhsDetection VHSv20140409 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vhsDetection VHSv20150108 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vhsDetection VHSv20160114 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vhsDetection VHSv20160507 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vhsDetection VHSv20170630 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vhsDetection VHSv20171207 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vhsDetection VHSv20180419 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vhsDetection, vhsListRemeasurement VHSDR1 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize;src
kronRad videoDetection VIDEODR2 Kron radius as defined in SE by Graham and Driver (2005) (SE: KRON_RADIUS*A_IMAGE) {catalogue TType keyword: Kron_radius}
r_k = ∑R² I(R) / ∑R I(R)
real 4 pixels   phys.angSize;src
Since <FLUX>_RADIUS is expressed in multiples of the major axis, <FLUX>_RADIUS is multiplied by A_IMAGE to convert to pixels.
kronRad videoDetection VIDEODR3 Kron radius as defined in SE by Graham and Driver (2005) (SE: KRON_RADIUS*A_IMAGE) {catalogue TType keyword: Kron_radius}
r_k = ∑R² I(R) / ∑R I(R)
real 4 pixels   phys.angSize
Since <FLUX>_RADIUS is expressed in multiples of the major axis, <FLUX>_RADIUS is multiplied by A_IMAGE to convert to pixels.
kronRad videoDetection VIDEODR4 Kron radius as defined in SE by Graham and Driver (2005) (SE: KRON_RADIUS*A_IMAGE) {catalogue TType keyword: Kron_radius}
r_k = ∑R² I(R) / ∑R I(R)
real 4 pixels   phys.angSize
Since <FLUX>_RADIUS is expressed in multiples of the major axis, <FLUX>_RADIUS is multiplied by A_IMAGE to convert to pixels.
kronRad videoDetection VIDEODR5 Kron radius as defined in SE by Graham and Driver (2005) (SE: KRON_RADIUS*A_IMAGE) {catalogue TType keyword: Kron_radius}
r_k = ∑R² I(R) / ∑R I(R)
real 4 pixels   phys.angSize
Since <FLUX>_RADIUS is expressed in multiples of the major axis, <FLUX>_RADIUS is multiplied by A_IMAGE to convert to pixels.
kronRad videoDetection VIDEOv20100513 Kron radius as defined in SE by Graham and Driver (2005) (SE: KRON_RADIUS*A_IMAGE) {catalogue TType keyword: Kron_radius}
r_k = ∑R² I(R) / ∑R I(R)
real 4 pixels   phys.angSize;src
Since <FLUX>_RADIUS is expressed in multiples of the major axis, <FLUX>_RADIUS is multiplied by A_IMAGE to convert to pixels.
kronRad videoDetection VIDEOv20111208 Kron radius as defined in SE by Graham and Driver (2005) (SE: KRON_RADIUS*A_IMAGE) {catalogue TType keyword: Kron_radius}
r_k = ∑R² I(R) / ∑R I(R)
real 4 pixels   phys.angSize;src
Since <FLUX>_RADIUS is expressed in multiples of the major axis, <FLUX>_RADIUS is multiplied by A_IMAGE to convert to pixels.
kronRad videoListRemeasurement VIDEOv20100513 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize;src
kronRad vikingDetection VIKINGDR2 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize;src
kronRad vikingDetection VIKINGDR3 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vikingDetection VIKINGDR4 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vikingDetection VIKINGv20111019 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize;src
kronRad vikingDetection VIKINGv20130417 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vikingDetection VIKINGv20140402 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vikingDetection VIKINGv20150421 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vikingDetection VIKINGv20151230 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vikingDetection VIKINGv20160406 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vikingDetection VIKINGv20161202 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vikingDetection VIKINGv20170715 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vikingDetection VIKINGv20181012 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vikingDetection, vikingListRemeasurement VIKINGv20110714 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize;src
kronRad vikingMapRemeasurement VIKINGZYSELJv20160909 Kron radius as defined in SE by Graham and Driver (2005) (SE: KRON_RADIUS*A_IMAGE; CASU: default) {catalogue TType keyword: Kron_radius}
r_k = ∑R² I(R) / ∑R I(R)
real 4 pixels   phys.angSize;src
Since <FLUX>_RADIUS is expressed in multiples of the major axis, <FLUX>_RADIUS is multiplied by A_IMAGE to convert to pixels.
kronRad vikingMapRemeasurement VIKINGZYSELJv20170124 Kron radius as defined in SE by Graham and Driver (2005) (SE: KRON_RADIUS*A_IMAGE; CASU: default) {catalogue TType keyword: Kron_radius}
r_k = ∑R² I(R) / ∑R I(R)
real 4 pixels   phys.angSize;src
Since <FLUX>_RADIUS is expressed in multiples of the major axis, <FLUX>_RADIUS is multiplied by A_IMAGE to convert to pixels.
kronRad vmcDetection VMCDR1 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize;src
kronRad vmcDetection VMCDR2 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vmcDetection VMCDR3 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vmcDetection VMCDR4 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vmcDetection VMCv20110909 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize;src
kronRad vmcDetection VMCv20120126 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize;src
kronRad vmcDetection VMCv20121128 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vmcDetection VMCv20130304 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vmcDetection VMCv20130805 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vmcDetection VMCv20140428 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vmcDetection VMCv20140903 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vmcDetection VMCv20150309 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vmcDetection VMCv20151218 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vmcDetection VMCv20160311 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vmcDetection VMCv20160822 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vmcDetection VMCv20170109 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vmcDetection VMCv20170411 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vmcDetection VMCv20171101 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vmcDetection VMCv20180702 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vmcDetection VMCv20181120 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
kronRad vmcDetection, vmcListRemeasurement VMCv20110816 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize;src
kronRad vvvDetection VVVDR4 r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels   phys.angSize
ks_1eNum vvvPsfDophotZYJHKsMergeLog VVVDR4 the extension number of this 1st epoch Ks frame tinyint 1     meta.number;em.IR.K
ks_1mfID vvvPsfDophotZYJHKsMergeLog VVVDR4 the UID of the relevant 1st epoch Ks tile multiframe bigint 8     meta.id;obs.field;em.IR.K
ks_1Mjd vvvPsfDophotZYJHKsMergeLog VVVDR4 the MJD of the 1st epoch Ks tile multiframe float 8     time;em.IR.K
ks_2eNum vvvPsfDophotZYJHKsMergeLog VVVDR4 the extension number of this 2nd epoch Ks frame tinyint 1     meta.number;em.IR.K
ks_2mfID vvvPsfDophotZYJHKsMergeLog VVVDR4 the UID of the relevant 2nd epoch Ks tile multiframe bigint 8     meta.id;obs.field;em.IR.K
ks_2Mjd vvvPsfDophotZYJHKsMergeLog VVVDR4 the MJD of the 2nd epoch Ks tile multiframe float 8     time;em.IR.K
ksAmpl vmcCepheidVariables VMCDR3 Amplitude of Ks band magnitude variation {catalogue TType keyword: A(Ks)} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.K
ksAmpl vmcCepheidVariables VMCDR4 Peak-to-Peak amplitude in Ks band {catalogue TType keyword: A(Ks)} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.K
ksAmpl vmcCepheidVariables VMCv20121128 Amplitude of Ks band magnitude variation {catalogue TType keyword: A(Ks)} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.NIR
ksAmpl vmcCepheidVariables VMCv20140428 Amplitude of Ks band magnitude variation {catalogue TType keyword: A(Ks)} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.K
ksAmpl vmcCepheidVariables VMCv20140903 Amplitude of Ks band magnitude variation {catalogue TType keyword: A(Ks)} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.K
ksAmpl vmcCepheidVariables VMCv20150309 Amplitude of Ks band magnitude variation {catalogue TType keyword: A(Ks)} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.K
ksAmpl vmcCepheidVariables VMCv20151218 Amplitude of Ks band magnitude variation {catalogue TType keyword: A(Ks)} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.K
ksAmpl vmcCepheidVariables VMCv20160311 Peak-to-Peak amplitude in Ks band {catalogue TType keyword: A(Ks)} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.K
ksAmpl vmcCepheidVariables VMCv20160822 Peak-to-Peak amplitude in Ks band {catalogue TType keyword: A(Ks)} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.K
ksAmpl vmcCepheidVariables VMCv20170109 Peak-to-Peak amplitude in Ks band {catalogue TType keyword: A(Ks)} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.K
ksAmpl vmcCepheidVariables VMCv20170411 Peak-to-Peak amplitude in Ks band {catalogue TType keyword: A(Ks)} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.K
ksAmpl vmcCepheidVariables VMCv20171101 Peak-to-Peak amplitude in Ks band {catalogue TType keyword: A(Ks)} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.K
ksAmpl vmcCepheidVariables VMCv20180702 Peak-to-Peak amplitude in Ks band {catalogue TType keyword: A(Ks)} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.K
ksAmpl vmcCepheidVariables VMCv20181120 Peak-to-Peak amplitude in Ks band {catalogue TType keyword: A(Ks)} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.K
ksAmpl vmcRRlyraeVariables VMCDR4 Amplitude in K_s band provided by GRATIS {catalogue TType keyword: AMPL_K} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.K
ksAmpl vmcRRlyraeVariables VMCv20160822 Amplitude in K_s band provided by GRATIS {catalogue TType keyword: AMPL_K} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.K
ksAmpl vmcRRlyraeVariables VMCv20170109 Amplitude in K_s band provided by GRATIS {catalogue TType keyword: AMPL_K} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.K
ksAmpl vmcRRlyraeVariables VMCv20170411 Amplitude in K_s band provided by GRATIS {catalogue TType keyword: AMPL_K} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.K
ksAmpl vmcRRlyraeVariables VMCv20171101 Amplitude in K_s band provided by GRATIS {catalogue TType keyword: AMPL_K} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.K
ksAmpl vmcRRlyraeVariables VMCv20180702 Amplitude in K_s band provided by GRATIS {catalogue TType keyword: AMPL_K} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.K
ksAmpl vmcRRlyraeVariables VMCv20181120 Amplitude in K_s band provided by GRATIS {catalogue TType keyword: AMPL_K} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.K
ksAmplErr vmcCepheidVariables VMCDR4 Error in Peak-to-Peak amplitude in Ks band {catalogue TType keyword: e_A(Ks)} real 4 mag -0.9999995e9 stat.error;src.var.amplitude;em.IR.K
ksAmplErr vmcCepheidVariables VMCv20160311 Error in Peak-to-Peak amplitude in Ks band {catalogue TType keyword: e_A(Ks)} real 4 mag -0.9999995e9 stat.error;src.var.amplitude;em.IR.K
ksAmplErr vmcCepheidVariables VMCv20160822 Error in Peak-to-Peak amplitude in Ks band {catalogue TType keyword: e_A(Ks)} real 4 mag -0.9999995e9 stat.error;src.var.amplitude;em.IR.K
ksAmplErr vmcCepheidVariables VMCv20170109 Error in Peak-to-Peak amplitude in Ks band {catalogue TType keyword: e_A(Ks)} real 4 mag -0.9999995e9 stat.error;src.var.amplitude;em.IR.K
ksAmplErr vmcCepheidVariables VMCv20170411 Error in Peak-to-Peak amplitude in Ks band {catalogue TType keyword: e_A(Ks)} real 4 mag -0.9999995e9 stat.error;src.var.amplitude;em.IR.K
ksAmplErr vmcCepheidVariables VMCv20171101 Error in Peak-to-Peak amplitude in Ks band {catalogue TType keyword: e_A(Ks)} real 4 mag -0.9999995e9 stat.error;src.var.amplitude;em.IR.K
ksAmplErr vmcCepheidVariables VMCv20180702 Error in Peak-to-Peak amplitude in Ks band {catalogue TType keyword: e_A(Ks)} real 4 mag -0.9999995e9 stat.error;src.var.amplitude;em.IR.K
ksAmplErr vmcCepheidVariables VMCv20181120 Error in Peak-to-Peak amplitude in Ks band {catalogue TType keyword: e_A(Ks)} real 4 mag -0.9999995e9 stat.error;src.var.amplitude;em.IR.K
ksAperJky3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Default point source Ks aperture corrected (2.0 arcsec aperture diameter) calibrated flux
If in doubt use this flux estimator
real 4 jansky -0.9999995e9 phot.flux
ksAperJky3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Default point source Ks aperture corrected (2.0 arcsec aperture diameter) calibrated flux
If in doubt use this flux estimator
real 4 jansky -0.9999995e9 phot.flux
ksAperJky3Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in default point/extended source Ks (2.0 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error
ksAperJky3Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in default point/extended source Ks (2.0 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error
ksAperJky4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Point source Ks aperture corrected (2.8 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 phot.flux
ksAperJky4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Point source Ks aperture corrected (2.8 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 phot.flux
ksAperJky4Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in point/extended source Ks (2.8 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error
ksAperJky4Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in point/extended source Ks (2.8 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error
ksAperJky6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Point source Ks aperture corrected (5.7 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 phot.flux
ksAperJky6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Point source Ks aperture corrected (5.7 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 phot.flux
ksAperJky6Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in point/extended source Ks (5.7 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error
ksAperJky6Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in point/extended source Ks (5.7 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error
ksAperJkyNoAperCorr3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Default extended source Ks (2.0 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux
If in doubt use this flux estimator
real 4 jansky -0.9999995e9 phot.flux
ksAperJkyNoAperCorr3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Default extended source Ks (2.0 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux
If in doubt use this flux estimator
real 4 jansky -0.9999995e9 phot.flux
ksAperJkyNoAperCorr4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Extended source Ks (2.8 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux real 4 jansky -0.9999995e9 phot.flux
ksAperJkyNoAperCorr4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Extended source Ks (2.8 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux real 4 jansky -0.9999995e9 phot.flux
ksAperJkyNoAperCorr6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Extended source Ks (5.7 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux real 4 jansky -0.9999995e9 phot.flux
ksAperJkyNoAperCorr6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Extended source Ks (5.7 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux real 4 jansky -0.9999995e9 phot.flux
ksAperLup3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Default point source Ks aperture corrected (2.0 arcsec aperture diameter) luptitude
If in doubt use this flux estimator
real 4 lup -0.9999995e9 phot.lup
ksAperLup3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Default point source Ks aperture corrected (2.0 arcsec aperture diameter) luptitude
If in doubt use this flux estimator
real 4 lup -0.9999995e9 phot.lup
ksAperLup3Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in default point/extended source Ks (2.0 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error
ksAperLup3Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in default point/extended source Ks (2.0 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error
ksAperLup4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Point source Ks aperture corrected (2.8 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 phot.lup
ksAperLup4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Point source Ks aperture corrected (2.8 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 phot.lup
ksAperLup4Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in point/extended source Ks (2.8 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error
ksAperLup4Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in point/extended source Ks (2.8 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error
ksAperLup6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Point source Ks aperture corrected (5.7 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 phot.lup
ksAperLup6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Point source Ks aperture corrected (5.7 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 phot.lup
ksAperLup6Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in point/extended source Ks (5.7 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error
ksAperLup6Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in point/extended source Ks (5.7 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error
ksAperLupNoAperCorr3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Default extended source Ks (2.0 arcsec aperture diameter, but no aperture correction applied) aperture luptitude
If in doubt use this flux estimator
real 4 lup -0.9999995e9 phot.lup
ksAperLupNoAperCorr3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Default extended source Ks (2.0 arcsec aperture diameter, but no aperture correction applied) aperture luptitude
If in doubt use this flux estimator
real 4 lup -0.9999995e9 phot.lup
ksAperLupNoAperCorr4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Extended source Ks (2.8 arcsec aperture diameter, but no aperture correction applied) aperture luptitude real 4 lup -0.9999995e9 phot.lup
ksAperLupNoAperCorr4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Extended source Ks (2.8 arcsec aperture diameter, but no aperture correction applied) aperture luptitude real 4 lup -0.9999995e9 phot.lup
ksAperLupNoAperCorr6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Extended source Ks (5.7 arcsec aperture diameter, but no aperture correction applied) aperture luptitude real 4 lup -0.9999995e9 phot.lup
ksAperLupNoAperCorr6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Extended source Ks (5.7 arcsec aperture diameter, but no aperture correction applied) aperture luptitude real 4 lup -0.9999995e9 phot.lup
ksAperMag1 vmcSynopticSource VMCDR1 Extended source Ks aperture corrected mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag1 vmcSynopticSource VMCDR2 Extended source Ks aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag1 vmcSynopticSource VMCDR3 Extended source Ks aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag1 vmcSynopticSource VMCDR4 Extended source Ks aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag1 vmcSynopticSource VMCv20110816 Extended source Ks aperture corrected mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag1 vmcSynopticSource VMCv20110909 Extended source Ks aperture corrected mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag1 vmcSynopticSource VMCv20120126 Extended source Ks aperture corrected mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag1 vmcSynopticSource VMCv20121128 Extended source Ks aperture corrected mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag1 vmcSynopticSource VMCv20130304 Extended source Ks aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag1 vmcSynopticSource VMCv20130805 Extended source Ks aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag1 vmcSynopticSource VMCv20140428 Extended source Ks aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag1 vmcSynopticSource VMCv20140903 Extended source Ks aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag1 vmcSynopticSource VMCv20150309 Extended source Ks aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag1 vmcSynopticSource VMCv20151218 Extended source Ks aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag1 vmcSynopticSource VMCv20160311 Extended source Ks aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag1 vmcSynopticSource VMCv20160822 Extended source Ks aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag1 vmcSynopticSource VMCv20170109 Extended source Ks aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag1 vmcSynopticSource VMCv20170411 Extended source Ks aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag1 vmcSynopticSource VMCv20171101 Extended source Ks aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag1 vmcSynopticSource VMCv20180702 Extended source Ks aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag1 vmcSynopticSource VMCv20181120 Extended source Ks aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag1 vvvSource VVVDR4 Point source Ks aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag1 vvvSynopticSource VVVDR4 Extended source Ks aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag1Err vmcSynopticSource VMCDR1 Error in extended source Ks mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag1Err vmcSynopticSource VMCDR2 Error in extended source Ks mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag1Err vmcSynopticSource VMCDR3 Error in extended source Ks mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag1Err vmcSynopticSource VMCDR4 Error in extended source Ks mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag1Err vmcSynopticSource VMCv20110816 Error in extended source Ks mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag1Err vmcSynopticSource VMCv20110909 Error in extended source Ks mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag1Err vmcSynopticSource VMCv20120126 Error in extended source Ks mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag1Err vmcSynopticSource VMCv20121128 Error in extended source Ks mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag1Err vmcSynopticSource VMCv20130304 Error in extended source Ks mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag1Err vmcSynopticSource VMCv20130805 Error in extended source Ks mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag1Err vmcSynopticSource VMCv20140428 Error in extended source Ks mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K
ksAperMag1Err vmcSynopticSource VMCv20140903 Error in extended source Ks mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag1Err vmcSynopticSource VMCv20150309 Error in extended source Ks mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag1Err vmcSynopticSource VMCv20151218 Error in extended source Ks mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag1Err vmcSynopticSource VMCv20160311 Error in extended source Ks mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag1Err vmcSynopticSource VMCv20160822 Error in extended source Ks mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag1Err vmcSynopticSource VMCv20170109 Error in extended source Ks mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag1Err vmcSynopticSource VMCv20170411 Error in extended source Ks mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag1Err vmcSynopticSource VMCv20171101 Error in extended source Ks mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag1Err vmcSynopticSource VMCv20180702 Error in extended source Ks mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag1Err vmcSynopticSource VMCv20181120 Error in extended source Ks mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag1Err vvvSource VVVDR4 Error in point source Ks mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag1Err vvvSynopticSource VVVDR4 Error in extended source Ks mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag2 vmcSynopticSource VMCDR1 Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag2 vmcSynopticSource VMCDR2 Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag2 vmcSynopticSource VMCDR3 Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag2 vmcSynopticSource VMCDR4 Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag2 vmcSynopticSource VMCv20110816 Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag2 vmcSynopticSource VMCv20110909 Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag2 vmcSynopticSource VMCv20120126 Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag2 vmcSynopticSource VMCv20121128 Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag2 vmcSynopticSource VMCv20130304 Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag2 vmcSynopticSource VMCv20130805 Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag2 vmcSynopticSource VMCv20140428 Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag2 vmcSynopticSource VMCv20140903 Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag2 vmcSynopticSource VMCv20150309 Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag2 vmcSynopticSource VMCv20151218 Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag2 vmcSynopticSource VMCv20160311 Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag2 vmcSynopticSource VMCv20160822 Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag2 vmcSynopticSource VMCv20170109 Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag2 vmcSynopticSource VMCv20170411 Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag2 vmcSynopticSource VMCv20171101 Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag2 vmcSynopticSource VMCv20180702 Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag2 vmcSynopticSource VMCv20181120 Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag2 vvvSynopticSource VVVDR4 Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag2Err vmcSynopticSource VMCDR1 Error in extended source Ks mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag2Err vmcSynopticSource VMCDR2 Error in extended source Ks mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag2Err vmcSynopticSource VMCDR3 Error in extended source Ks mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag2Err vmcSynopticSource VMCDR4 Error in extended source Ks mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag2Err vmcSynopticSource VMCv20110816 Error in extended source Ks mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag2Err vmcSynopticSource VMCv20110909 Error in extended source Ks mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag2Err vmcSynopticSource VMCv20120126 Error in extended source Ks mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag2Err vmcSynopticSource VMCv20121128 Error in extended source Ks mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag2Err vmcSynopticSource VMCv20130304 Error in extended source Ks mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag2Err vmcSynopticSource VMCv20130805 Error in extended source Ks mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag2Err vmcSynopticSource VMCv20140428 Error in extended source Ks mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K
ksAperMag2Err vmcSynopticSource VMCv20140903 Error in extended source Ks mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag2Err vmcSynopticSource VMCv20150309 Error in extended source Ks mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag2Err vmcSynopticSource VMCv20151218 Error in extended source Ks mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag2Err vmcSynopticSource VMCv20160311 Error in extended source Ks mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag2Err vmcSynopticSource VMCv20160822 Error in extended source Ks mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag2Err vmcSynopticSource VMCv20170109 Error in extended source Ks mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag2Err vmcSynopticSource VMCv20170411 Error in extended source Ks mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag2Err vmcSynopticSource VMCv20171101 Error in extended source Ks mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag2Err vmcSynopticSource VMCv20180702 Error in extended source Ks mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag2Err vmcSynopticSource VMCv20181120 Error in extended source Ks mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag2Err vvvSynopticSource VVVDR4 Error in extended source Ks mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag3 vhsSource VHSDR1 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMag3 vhsSource VHSDR2 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMag3 vhsSource VHSDR3 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vhsSource VHSDR4 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vhsSource VHSv20120926 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMag3 vhsSource VHSv20130417 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMag3 vhsSource VHSv20140409 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vhsSource VHSv20150108 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vhsSource VHSv20160114 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vhsSource VHSv20160507 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vhsSource VHSv20170630 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vhsSource VHSv20171207 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vhsSource VHSv20180419 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 videoSource VIDEODR2 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMag3 videoSource VIDEODR3 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMag3 videoSource VIDEODR4 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 videoSource VIDEODR5 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 videoSource VIDEOv20100513 Default point/extended source Ks mag, no aperture correction applied
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMag3 videoSource VIDEOv20111208 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMag3 vikingSource VIKINGDR2 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMag3 vikingSource VIKINGDR3 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMag3 vikingSource VIKINGDR4 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vikingSource VIKINGv20110714 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMag3 vikingSource VIKINGv20111019 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMag3 vikingSource VIKINGv20130417 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMag3 vikingSource VIKINGv20140402 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vikingSource VIKINGv20150421 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vikingSource VIKINGv20151230 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vikingSource VIKINGv20160406 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vikingSource VIKINGv20161202 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vikingSource VIKINGv20170715 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vikingSource VIKINGv20181012 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Default point source Ks aperture corrected (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMag3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Default point source Ks aperture corrected (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMag3 vmcSource VMCDR1 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMag3 vmcSource VMCDR2 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vmcSource VMCDR3 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vmcSource VMCDR4 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vmcSource VMCv20110816 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMag3 vmcSource VMCv20110909 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMag3 vmcSource VMCv20120126 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMag3 vmcSource VMCv20121128 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMag3 vmcSource VMCv20130304 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMag3 vmcSource VMCv20130805 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vmcSource VMCv20140428 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vmcSource VMCv20140903 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vmcSource VMCv20150309 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vmcSource VMCv20151218 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vmcSource VMCv20160311 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vmcSource VMCv20160822 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vmcSource VMCv20170109 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vmcSource VMCv20170411 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vmcSource VMCv20171101 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vmcSource VMCv20180702 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vmcSource VMCv20181120 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vmcSynopticSource VMCDR1 Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag3 vmcSynopticSource VMCDR2 Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vmcSynopticSource VMCDR3 Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vmcSynopticSource VMCDR4 Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vmcSynopticSource VMCv20110816 Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag3 vmcSynopticSource VMCv20110909 Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag3 vmcSynopticSource VMCv20120126 Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag3 vmcSynopticSource VMCv20121128 Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag3 vmcSynopticSource VMCv20130304 Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag3 vmcSynopticSource VMCv20130805 Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vmcSynopticSource VMCv20140428 Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vmcSynopticSource VMCv20140903 Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vmcSynopticSource VMCv20150309 Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vmcSynopticSource VMCv20151218 Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vmcSynopticSource VMCv20160311 Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vmcSynopticSource VMCv20160822 Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vmcSynopticSource VMCv20170109 Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vmcSynopticSource VMCv20170411 Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vmcSynopticSource VMCv20171101 Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vmcSynopticSource VMCv20180702 Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vmcSynopticSource VMCv20181120 Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vvvSource VVVDR4 Default point source Ks aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3 vvvSynopticSource VVVDR4 Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag3Err vhsSource VHSDR1 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag3Err vhsSource VHSDR2 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag3Err vhsSource VHSDR3 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K
ksAperMag3Err vhsSource VHSDR4 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag3Err vhsSource VHSv20120926 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag3Err vhsSource VHSv20130417 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag3Err vhsSource VHSv20140409 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K
ksAperMag3Err vhsSource VHSv20150108 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag3Err vhsSource VHSv20160114 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag3Err vhsSource VHSv20160507 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag3Err vhsSource VHSv20170630 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag3Err vhsSource VHSv20171207 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag3Err vhsSource VHSv20180419 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag3Err videoSource VIDEODR2 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag3Err videoSource VIDEODR3 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag3Err videoSource VIDEODR4 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag3Err videoSource VIDEODR5 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag3Err videoSource VIDEOv20100513 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag3Err videoSource VIDEOv20111208 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag3Err vikingSource VIKINGDR2 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag3Err vikingSource VIKINGDR3 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag3Err vikingSource VIKINGDR4 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K
ksAperMag3Err vikingSource VIKINGv20110714 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag3Err vikingSource VIKINGv20111019 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag3Err vikingSource VIKINGv20130417 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag3Err vikingSource VIKINGv20140402 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag3Err vikingSource VIKINGv20150421 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag3Err vikingSource VIKINGv20151230 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag3Err vikingSource VIKINGv20160406 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag3Err vikingSource VIKINGv20161202 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag3Err vikingSource VIKINGv20170715 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag3Err vikingSource VIKINGv20181012 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag3Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in default point/extended source Ks (2.0 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error
ksAperMag3Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in default point/extended source Ks (2.0 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error
ksAperMag3Err vmcSource VMCDR2 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag3Err vmcSource VMCDR3 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag3Err vmcSource VMCDR4 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag3Err vmcSource VMCv20110816 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag3Err vmcSource VMCv20110909 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag3Err vmcSource VMCv20120126 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag3Err vmcSource VMCv20121128 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag3Err vmcSource VMCv20130304 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag3Err vmcSource VMCv20130805 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag3Err vmcSource VMCv20140428 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K
ksAperMag3Err vmcSource VMCv20140903 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag3Err vmcSource VMCv20150309 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag3Err vmcSource VMCv20151218 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag3Err vmcSource VMCv20160311 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag3Err vmcSource VMCv20160822 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag3Err vmcSource VMCv20170109 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag3Err vmcSource VMCv20170411 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag3Err vmcSource VMCv20171101 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag3Err vmcSource VMCv20180702 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag3Err vmcSource VMCv20181120 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag3Err vmcSource, vmcSynopticSource VMCDR1 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag3Err vvvSource VVVDR4 Error in default point source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag3Err vvvSynopticSource VVVDR4 Error in default point/extended source Ks mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag4 vhsSource VHSDR1 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag4 vhsSource VHSDR2 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag4 vhsSource VHSDR3 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vhsSource VHSDR4 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vhsSource VHSv20120926 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag4 vhsSource VHSv20130417 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag4 vhsSource VHSv20140409 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vhsSource VHSv20150108 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vhsSource VHSv20160114 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vhsSource VHSv20160507 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vhsSource VHSv20170630 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vhsSource VHSv20171207 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vhsSource VHSv20180419 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 videoSource VIDEODR2 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag4 videoSource VIDEODR3 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag4 videoSource VIDEODR4 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 videoSource VIDEODR5 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 videoSource VIDEOv20100513 Extended source Ks mag, no aperture correction applied real 4 mag -0.9999995e9 phot.mag
ksAperMag4 videoSource VIDEOv20111208 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag4 vikingSource VIKINGDR2 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag4 vikingSource VIKINGDR3 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag4 vikingSource VIKINGDR4 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vikingSource VIKINGv20110714 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag4 vikingSource VIKINGv20111019 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag4 vikingSource VIKINGv20130417 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag4 vikingSource VIKINGv20140402 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vikingSource VIKINGv20150421 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vikingSource VIKINGv20151230 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vikingSource VIKINGv20160406 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vikingSource VIKINGv20161202 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vikingSource VIKINGv20170715 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vikingSource VIKINGv20181012 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Point source Ks aperture corrected (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Point source Ks aperture corrected (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag4 vmcSource VMCDR1 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag4 vmcSource VMCDR2 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vmcSource VMCDR3 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vmcSource VMCDR4 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vmcSource VMCv20110816 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag4 vmcSource VMCv20110909 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag4 vmcSource VMCv20120126 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag4 vmcSource VMCv20121128 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag4 vmcSource VMCv20130304 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag4 vmcSource VMCv20130805 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vmcSource VMCv20140428 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vmcSource VMCv20140903 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vmcSource VMCv20150309 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vmcSource VMCv20151218 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vmcSource VMCv20160311 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vmcSource VMCv20160822 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vmcSource VMCv20170109 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vmcSource VMCv20170411 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vmcSource VMCv20171101 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vmcSource VMCv20180702 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vmcSource VMCv20181120 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vmcSynopticSource VMCDR1 Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag4 vmcSynopticSource VMCDR2 Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vmcSynopticSource VMCDR3 Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vmcSynopticSource VMCDR4 Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vmcSynopticSource VMCv20110816 Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag4 vmcSynopticSource VMCv20110909 Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag4 vmcSynopticSource VMCv20120126 Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag4 vmcSynopticSource VMCv20121128 Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag4 vmcSynopticSource VMCv20130304 Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag4 vmcSynopticSource VMCv20130805 Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vmcSynopticSource VMCv20140428 Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vmcSynopticSource VMCv20140903 Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vmcSynopticSource VMCv20150309 Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vmcSynopticSource VMCv20151218 Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vmcSynopticSource VMCv20160311 Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vmcSynopticSource VMCv20160822 Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vmcSynopticSource VMCv20170109 Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vmcSynopticSource VMCv20170411 Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vmcSynopticSource VMCv20171101 Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vmcSynopticSource VMCv20180702 Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vmcSynopticSource VMCv20181120 Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vvvSource VVVDR4 Point source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4 vvvSynopticSource VVVDR4 Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag4Err vhsSource VHSDR1 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag4Err vhsSource VHSDR2 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag4Err vhsSource VHSDR3 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K
ksAperMag4Err vhsSource VHSDR4 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag4Err vhsSource VHSv20120926 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag4Err vhsSource VHSv20130417 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag4Err vhsSource VHSv20140409 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K
ksAperMag4Err vhsSource VHSv20150108 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag4Err vhsSource VHSv20160114 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag4Err vhsSource VHSv20160507 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag4Err vhsSource VHSv20170630 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag4Err vhsSource VHSv20171207 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag4Err vhsSource VHSv20180419 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag4Err videoSource VIDEODR2 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag4Err videoSource VIDEODR3 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag4Err videoSource VIDEODR4 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag4Err videoSource VIDEODR5 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag4Err videoSource VIDEOv20100513 Error in extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag4Err videoSource VIDEOv20111208 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag4Err vikingSource VIKINGDR2 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag4Err vikingSource VIKINGDR3 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag4Err vikingSource VIKINGDR4 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K
ksAperMag4Err vikingSource VIKINGv20110714 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag4Err vikingSource VIKINGv20111019 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag4Err vikingSource VIKINGv20130417 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag4Err vikingSource VIKINGv20140402 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag4Err vikingSource VIKINGv20150421 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag4Err vikingSource VIKINGv20151230 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag4Err vikingSource VIKINGv20160406 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag4Err vikingSource VIKINGv20161202 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag4Err vikingSource VIKINGv20170715 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag4Err vikingSource VIKINGv20181012 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag4Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in point/extended source Ks (2.8 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error
ksAperMag4Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in point/extended source Ks (2.8 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error
ksAperMag4Err vmcSource VMCDR1 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag4Err vmcSource VMCDR2 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag4Err vmcSource VMCDR3 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag4Err vmcSource VMCDR4 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag4Err vmcSource VMCv20110816 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag4Err vmcSource VMCv20110909 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag4Err vmcSource VMCv20120126 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag4Err vmcSource VMCv20121128 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag4Err vmcSource VMCv20130304 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag4Err vmcSource VMCv20130805 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag4Err vmcSource VMCv20140428 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K
ksAperMag4Err vmcSource VMCv20140903 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag4Err vmcSource VMCv20150309 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag4Err vmcSource VMCv20151218 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag4Err vmcSource VMCv20160311 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag4Err vmcSource VMCv20160822 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag4Err vmcSource VMCv20170109 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag4Err vmcSource VMCv20170411 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag4Err vmcSource VMCv20171101 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag4Err vmcSource VMCv20180702 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag4Err vmcSource VMCv20181120 Error in point/extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag4Err vmcSynopticSource VMCDR1 Error in extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag4Err vmcSynopticSource VMCDR2 Error in extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag4Err vmcSynopticSource VMCDR3 Error in extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag4Err vmcSynopticSource VMCDR4 Error in extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag4Err vmcSynopticSource VMCv20110816 Error in extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag4Err vmcSynopticSource VMCv20110909 Error in extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag4Err vmcSynopticSource VMCv20120126 Error in extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag4Err vmcSynopticSource VMCv20121128 Error in extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag4Err vmcSynopticSource VMCv20130304 Error in extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag4Err vmcSynopticSource VMCv20130805 Error in extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag4Err vmcSynopticSource VMCv20140428 Error in extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K
ksAperMag4Err vmcSynopticSource VMCv20140903 Error in extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag4Err vmcSynopticSource VMCv20150309 Error in extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag4Err vmcSynopticSource VMCv20151218 Error in extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag4Err vmcSynopticSource VMCv20160311 Error in extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag4Err vmcSynopticSource VMCv20160822 Error in extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag4Err vmcSynopticSource VMCv20170109 Error in extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag4Err vmcSynopticSource VMCv20170411 Error in extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag4Err vmcSynopticSource VMCv20171101 Error in extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag4Err vmcSynopticSource VMCv20180702 Error in extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag4Err vmcSynopticSource VMCv20181120 Error in extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag4Err vvvSource VVVDR4 Error in point source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag4Err vvvSynopticSource VVVDR4 Error in extended source Ks mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag5 vmcSynopticSource VMCDR1 Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag5 vmcSynopticSource VMCDR2 Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag5 vmcSynopticSource VMCDR3 Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag5 vmcSynopticSource VMCDR4 Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag5 vmcSynopticSource VMCv20110816 Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag5 vmcSynopticSource VMCv20110909 Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag5 vmcSynopticSource VMCv20120126 Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag5 vmcSynopticSource VMCv20121128 Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag5 vmcSynopticSource VMCv20130304 Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag5 vmcSynopticSource VMCv20130805 Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag5 vmcSynopticSource VMCv20140428 Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag5 vmcSynopticSource VMCv20140903 Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag5 vmcSynopticSource VMCv20150309 Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag5 vmcSynopticSource VMCv20151218 Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag5 vmcSynopticSource VMCv20160311 Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag5 vmcSynopticSource VMCv20160822 Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag5 vmcSynopticSource VMCv20170109 Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag5 vmcSynopticSource VMCv20170411 Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag5 vmcSynopticSource VMCv20171101 Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag5 vmcSynopticSource VMCv20180702 Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag5 vmcSynopticSource VMCv20181120 Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag5 vvvSynopticSource VVVDR4 Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag5Err vmcSynopticSource VMCDR1 Error in extended source Ks mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag5Err vmcSynopticSource VMCDR2 Error in extended source Ks mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag5Err vmcSynopticSource VMCDR3 Error in extended source Ks mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag5Err vmcSynopticSource VMCDR4 Error in extended source Ks mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag5Err vmcSynopticSource VMCv20110816 Error in extended source Ks mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag5Err vmcSynopticSource VMCv20110909 Error in extended source Ks mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag5Err vmcSynopticSource VMCv20120126 Error in extended source Ks mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag5Err vmcSynopticSource VMCv20121128 Error in extended source Ks mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag5Err vmcSynopticSource VMCv20130304 Error in extended source Ks mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag5Err vmcSynopticSource VMCv20130805 Error in extended source Ks mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag5Err vmcSynopticSource VMCv20140428 Error in extended source Ks mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K
ksAperMag5Err vmcSynopticSource VMCv20140903 Error in extended source Ks mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag5Err vmcSynopticSource VMCv20150309 Error in extended source Ks mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag5Err vmcSynopticSource VMCv20151218 Error in extended source Ks mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag5Err vmcSynopticSource VMCv20160311 Error in extended source Ks mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag5Err vmcSynopticSource VMCv20160822 Error in extended source Ks mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag5Err vmcSynopticSource VMCv20170109 Error in extended source Ks mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag5Err vmcSynopticSource VMCv20170411 Error in extended source Ks mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag5Err vmcSynopticSource VMCv20171101 Error in extended source Ks mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag5Err vmcSynopticSource VMCv20180702 Error in extended source Ks mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag5Err vmcSynopticSource VMCv20181120 Error in extended source Ks mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag5Err vvvSynopticSource VVVDR4 Error in extended source Ks mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag6 vhsSource VHSDR1 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag6 vhsSource VHSDR2 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag6 vhsSource VHSDR3 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag6 vhsSource VHSDR4 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag6 vhsSource VHSv20120926 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag6 vhsSource VHSv20130417 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag6 vhsSource VHSv20140409 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag6 vhsSource VHSv20150108 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag6 vhsSource VHSv20160114 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag6 vhsSource VHSv20160507 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag6 vhsSource VHSv20170630 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag6 vhsSource VHSv20171207 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag6 vhsSource VHSv20180419 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag6 videoSource VIDEODR2 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag6 videoSource VIDEODR3 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag6 videoSource VIDEODR4 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag6 videoSource VIDEODR5 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag6 videoSource VIDEOv20100513 Extended source Ks mag, no aperture correction applied real 4 mag -0.9999995e9 phot.mag
ksAperMag6 videoSource VIDEOv20111208 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag6 vikingSource VIKINGDR2 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag6 vikingSource VIKINGDR3 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag6 vikingSource VIKINGDR4 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag6 vikingSource VIKINGv20110714 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag6 vikingSource VIKINGv20111019 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag6 vikingSource VIKINGv20130417 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag6 vikingSource VIKINGv20140402 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag6 vikingSource VIKINGv20150421 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag6 vikingSource VIKINGv20151230 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag6 vikingSource VIKINGv20160406 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag6 vikingSource VIKINGv20161202 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag6 vikingSource VIKINGv20170715 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag6 vikingSource VIKINGv20181012 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Point source Ks aperture corrected (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Point source Ks aperture corrected (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag6 vmcSource VMCDR1 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag6 vmcSource VMCDR2 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag6 vmcSource VMCDR3 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag6 vmcSource VMCDR4 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag6 vmcSource VMCv20110816 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag6 vmcSource VMCv20110909 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag6 vmcSource VMCv20120126 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag6 vmcSource VMCv20121128 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag6 vmcSource VMCv20130304 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMag6 vmcSource VMCv20130805 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag6 vmcSource VMCv20140428 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag6 vmcSource VMCv20140903 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag6 vmcSource VMCv20150309 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag6 vmcSource VMCv20151218 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag6 vmcSource VMCv20160311 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag6 vmcSource VMCv20160822 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag6 vmcSource VMCv20170109 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag6 vmcSource VMCv20170411 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag6 vmcSource VMCv20171101 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag6 vmcSource VMCv20180702 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag6 vmcSource VMCv20181120 Point source Ks aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMag6Err vhsSource VHSDR1 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag6Err vhsSource VHSDR2 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag6Err vhsSource VHSDR3 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K
ksAperMag6Err vhsSource VHSDR4 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag6Err vhsSource VHSv20120926 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag6Err vhsSource VHSv20130417 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag6Err vhsSource VHSv20140409 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K
ksAperMag6Err vhsSource VHSv20150108 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag6Err vhsSource VHSv20160114 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag6Err vhsSource VHSv20160507 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag6Err vhsSource VHSv20170630 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag6Err vhsSource VHSv20171207 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag6Err vhsSource VHSv20180419 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag6Err videoSource VIDEODR2 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag6Err videoSource VIDEODR3 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag6Err videoSource VIDEODR4 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag6Err videoSource VIDEODR5 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag6Err videoSource VIDEOv20100513 Error in extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag6Err videoSource VIDEOv20111208 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag6Err vikingSource VIKINGDR2 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag6Err vikingSource VIKINGDR3 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag6Err vikingSource VIKINGDR4 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K
ksAperMag6Err vikingSource VIKINGv20110714 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag6Err vikingSource VIKINGv20111019 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag6Err vikingSource VIKINGv20130417 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag6Err vikingSource VIKINGv20140402 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag6Err vikingSource VIKINGv20150421 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag6Err vikingSource VIKINGv20151230 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag6Err vikingSource VIKINGv20160406 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag6Err vikingSource VIKINGv20161202 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag6Err vikingSource VIKINGv20170715 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag6Err vikingSource VIKINGv20181012 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag6Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in point/extended source Ks (5.7 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error
ksAperMag6Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in point/extended source Ks (5.7 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error
ksAperMag6Err vmcSource VMCDR1 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag6Err vmcSource VMCDR2 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag6Err vmcSource VMCDR3 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag6Err vmcSource VMCDR4 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag6Err vmcSource VMCv20110816 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag6Err vmcSource VMCv20110909 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag6Err vmcSource VMCv20120126 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag6Err vmcSource VMCv20121128 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag6Err vmcSource VMCv20130304 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag6Err vmcSource VMCv20130805 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
ksAperMag6Err vmcSource VMCv20140428 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K
ksAperMag6Err vmcSource VMCv20140903 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag6Err vmcSource VMCv20150309 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.K;phot.mag
ksAperMag6Err vmcSource VMCv20151218 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag6Err vmcSource VMCv20160311 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag6Err vmcSource VMCv20160822 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag6Err vmcSource VMCv20170109 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag6Err vmcSource VMCv20170411 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag6Err vmcSource VMCv20171101 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag6Err vmcSource VMCv20180702 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMag6Err vmcSource VMCv20181120 Error in point/extended source Ks mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.K
ksAperMagNoAperCorr3 vhsSource VHSDR1 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr3 vhsSource VHSDR2 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr3 vhsSource VHSDR3 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr3 vhsSource VHSDR4 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr3 vhsSource VHSv20120926 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr3 vhsSource VHSv20130417 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr3 vhsSource VHSv20140409 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr3 vhsSource VHSv20150108 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr3 vhsSource VHSv20160114 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr3 vhsSource VHSv20160507 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr3 vhsSource VHSv20170630 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr3 vhsSource VHSv20171207 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr3 vhsSource VHSv20180419 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr3 videoSource VIDEODR2 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr3 videoSource VIDEODR3 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr3 videoSource VIDEODR4 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr3 videoSource VIDEODR5 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr3 videoSource VIDEOv20111208 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr3 vikingSource VIKINGDR2 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr3 vikingSource VIKINGDR3 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr3 vikingSource VIKINGDR4 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr3 vikingSource VIKINGv20110714 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr3 vikingSource VIKINGv20111019 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr3 vikingSource VIKINGv20130417 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr3 vikingSource VIKINGv20140402 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr3 vikingSource VIKINGv20150421 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr3 vikingSource VIKINGv20151230 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr3 vikingSource VIKINGv20160406 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr3 vikingSource VIKINGv20161202 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr3 vikingSource VIKINGv20170715 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr3 vikingSource VIKINGv20181012 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Default extended source Ks (2.0 arcsec aperture diameter, but no aperture correction applied) aperture magnitude
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Default extended source Ks (2.0 arcsec aperture diameter, but no aperture correction applied) aperture magnitude
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr3 vmcSource VMCDR1 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr3 vmcSource VMCDR2 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr3 vmcSource VMCDR3 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr3 vmcSource VMCDR4 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr3 vmcSource VMCv20110816 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr3 vmcSource VMCv20110909 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr3 vmcSource VMCv20120126 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr3 vmcSource VMCv20121128 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr3 vmcSource VMCv20130304 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr3 vmcSource VMCv20130805 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr3 vmcSource VMCv20140428 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr3 vmcSource VMCv20140903 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr3 vmcSource VMCv20150309 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr3 vmcSource VMCv20151218 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr3 vmcSource VMCv20160311 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr3 vmcSource VMCv20160822 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr3 vmcSource VMCv20170109 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr3 vmcSource VMCv20170411 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr3 vmcSource VMCv20171101 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr3 vmcSource VMCv20180702 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr3 vmcSource VMCv20181120 Default extended source Ks aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr4 vhsSource VHSDR1 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr4 vhsSource VHSDR2 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr4 vhsSource VHSDR3 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr4 vhsSource VHSDR4 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr4 vhsSource VHSv20120926 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr4 vhsSource VHSv20130417 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr4 vhsSource VHSv20140409 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr4 vhsSource VHSv20150108 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr4 vhsSource VHSv20160114 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr4 vhsSource VHSv20160507 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr4 vhsSource VHSv20170630 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr4 vhsSource VHSv20171207 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr4 vhsSource VHSv20180419 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr4 videoSource VIDEODR2 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr4 videoSource VIDEODR3 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr4 videoSource VIDEODR4 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr4 videoSource VIDEODR5 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr4 videoSource VIDEOv20111208 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr4 vikingSource VIKINGDR2 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr4 vikingSource VIKINGDR3 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr4 vikingSource VIKINGDR4 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr4 vikingSource VIKINGv20110714 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr4 vikingSource VIKINGv20111019 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr4 vikingSource VIKINGv20130417 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr4 vikingSource VIKINGv20140402 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr4 vikingSource VIKINGv20150421 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr4 vikingSource VIKINGv20151230 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr4 vikingSource VIKINGv20160406 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr4 vikingSource VIKINGv20161202 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr4 vikingSource VIKINGv20170715 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr4 vikingSource VIKINGv20181012 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Extended source Ks (2.8 arcsec aperture diameter, but no aperture correction applied) aperture magnitude real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Extended source Ks (2.8 arcsec aperture diameter, but no aperture correction applied) aperture magnitude real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr4 vmcSource VMCDR1 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr4 vmcSource VMCDR2 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr4 vmcSource VMCDR3 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr4 vmcSource VMCDR4 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr4 vmcSource VMCv20110816 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr4 vmcSource VMCv20110909 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr4 vmcSource VMCv20120126 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr4 vmcSource VMCv20121128 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr4 vmcSource VMCv20130304 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr4 vmcSource VMCv20130805 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr4 vmcSource VMCv20140428 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr4 vmcSource VMCv20140903 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr4 vmcSource VMCv20150309 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr4 vmcSource VMCv20151218 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr4 vmcSource VMCv20160311 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr4 vmcSource VMCv20160822 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr4 vmcSource VMCv20170109 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr4 vmcSource VMCv20170411 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr4 vmcSource VMCv20171101 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr4 vmcSource VMCv20180702 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr4 vmcSource VMCv20181120 Extended source Ks aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr6 vhsSource VHSDR1 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr6 vhsSource VHSDR2 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr6 vhsSource VHSDR3 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr6 vhsSource VHSDR4 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr6 vhsSource VHSv20120926 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr6 vhsSource VHSv20130417 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr6 vhsSource VHSv20140409 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr6 vhsSource VHSv20150108 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr6 vhsSource VHSv20160114 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr6 vhsSource VHSv20160507 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr6 vhsSource VHSv20170630 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr6 vhsSource VHSv20171207 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr6 vhsSource VHSv20180419 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr6 videoSource VIDEODR2 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr6 videoSource VIDEODR3 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr6 videoSource VIDEODR4 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr6 videoSource VIDEODR5 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr6 videoSource VIDEOv20111208 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr6 vikingSource VIKINGDR2 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr6 vikingSource VIKINGDR3 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr6 vikingSource VIKINGDR4 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr6 vikingSource VIKINGv20110714 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr6 vikingSource VIKINGv20111019 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr6 vikingSource VIKINGv20130417 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr6 vikingSource VIKINGv20140402 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr6 vikingSource VIKINGv20150421 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr6 vikingSource VIKINGv20151230 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr6 vikingSource VIKINGv20160406 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr6 vikingSource VIKINGv20161202 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr6 vikingSource VIKINGv20170715 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr6 vikingSource VIKINGv20181012 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Extended source Ks (5.7 arcsec aperture diameter, but no aperture correction applied) aperture magnitude real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Extended source Ks (5.7 arcsec aperture diameter, but no aperture correction applied) aperture magnitude real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr6 vmcSource VMCDR1 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr6 vmcSource VMCDR2 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr6 vmcSource VMCDR3 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr6 vmcSource VMCDR4 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr6 vmcSource VMCv20110816 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr6 vmcSource VMCv20110909 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr6 vmcSource VMCv20120126 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr6 vmcSource VMCv20121128 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr6 vmcSource VMCv20130304 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
ksAperMagNoAperCorr6 vmcSource VMCv20130805 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr6 vmcSource VMCv20140428 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr6 vmcSource VMCv20140903 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr6 vmcSource VMCv20150309 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr6 vmcSource VMCv20151218 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr6 vmcSource VMCv20160311 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr6 vmcSource VMCv20160822 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr6 vmcSource VMCv20170109 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr6 vmcSource VMCv20170411 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr6 vmcSource VMCv20171101 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr6 vmcSource VMCv20180702 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksAperMagNoAperCorr6 vmcSource VMCv20181120 Extended source Ks aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.K
ksaStratAst videoVarFrameSetInfo VIDEODR2 Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks 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.
ksaStratAst videoVarFrameSetInfo VIDEODR3 Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
ksaStratAst videoVarFrameSetInfo VIDEODR4 Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksaStratAst videoVarFrameSetInfo VIDEODR5 Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksaStratAst videoVarFrameSetInfo VIDEOv20100513 Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks 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.
ksaStratAst videoVarFrameSetInfo VIDEOv20111208 Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks 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.
ksaStratAst vikingVarFrameSetInfo VIKINGDR2 Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks 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.
ksaStratAst vikingVarFrameSetInfo VIKINGv20110714 Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks 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.
ksaStratAst vikingVarFrameSetInfo VIKINGv20111019 Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks 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.
ksaStratAst vmcVarFrameSetInfo VMCDR1 Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks 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.
ksaStratAst vmcVarFrameSetInfo VMCDR2 Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
ksaStratAst vmcVarFrameSetInfo VMCDR3 Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksaStratAst vmcVarFrameSetInfo VMCDR4 Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksaStratAst vmcVarFrameSetInfo VMCv20110816 Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks 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.
ksaStratAst vmcVarFrameSetInfo VMCv20110909 Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks 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.
ksaStratAst vmcVarFrameSetInfo VMCv20120126 Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks 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.
ksaStratAst vmcVarFrameSetInfo VMCv20121128 Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
ksaStratAst vmcVarFrameSetInfo VMCv20130304 Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
ksaStratAst vmcVarFrameSetInfo VMCv20130805 Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
ksaStratAst vmcVarFrameSetInfo VMCv20140428 Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksaStratAst vmcVarFrameSetInfo VMCv20140903 Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksaStratAst vmcVarFrameSetInfo VMCv20150309 Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksaStratAst vmcVarFrameSetInfo VMCv20151218 Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksaStratAst vmcVarFrameSetInfo VMCv20160311 Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksaStratAst vmcVarFrameSetInfo VMCv20160822 Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksaStratAst vmcVarFrameSetInfo VMCv20170109 Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksaStratAst vmcVarFrameSetInfo VMCv20170411 Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksaStratAst vmcVarFrameSetInfo VMCv20171101 Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksaStratAst vmcVarFrameSetInfo VMCv20180702 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Ks band. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksaStratAst vmcVarFrameSetInfo VMCv20181120 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Ks band. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksaStratAst vvvVarFrameSetInfo VVVDR4 Strateva parameter, a, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksaStratPht videoVarFrameSetInfo VIDEODR2 Strateva parameter, a, in fit to photometric rms vs magnitude in Ks 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.
ksaStratPht videoVarFrameSetInfo VIDEODR3 Strateva parameter, a, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
ksaStratPht videoVarFrameSetInfo VIDEODR4 Strateva parameter, a, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksaStratPht videoVarFrameSetInfo VIDEODR5 Strateva parameter, a, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksaStratPht videoVarFrameSetInfo VIDEOv20100513 Strateva parameter, a, in fit to photometric rms vs magnitude in Ks 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.
ksaStratPht videoVarFrameSetInfo VIDEOv20111208 Strateva parameter, a, in fit to photometric rms vs magnitude in Ks 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.
ksaStratPht vikingVarFrameSetInfo VIKINGDR2 Strateva parameter, a, in fit to photometric rms vs magnitude in Ks 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.
ksaStratPht vikingVarFrameSetInfo VIKINGv20110714 Strateva parameter, a, in fit to photometric rms vs magnitude in Ks 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.
ksaStratPht vikingVarFrameSetInfo VIKINGv20111019 Strateva parameter, a, in fit to photometric rms vs magnitude in Ks 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.
ksaStratPht vmcVarFrameSetInfo VMCDR1 Strateva parameter, a, in fit to photometric rms vs magnitude in Ks 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.
ksaStratPht vmcVarFrameSetInfo VMCDR2 Strateva parameter, a, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
ksaStratPht vmcVarFrameSetInfo VMCDR3 Strateva parameter, a, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksaStratPht vmcVarFrameSetInfo VMCDR4 Strateva parameter, a, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksaStratPht vmcVarFrameSetInfo VMCv20110816 Strateva parameter, a, in fit to photometric rms vs magnitude in Ks 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.
ksaStratPht vmcVarFrameSetInfo VMCv20110909 Strateva parameter, a, in fit to photometric rms vs magnitude in Ks 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.
ksaStratPht vmcVarFrameSetInfo VMCv20120126 Strateva parameter, a, in fit to photometric rms vs magnitude in Ks 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.
ksaStratPht vmcVarFrameSetInfo VMCv20121128 Strateva parameter, a, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
ksaStratPht vmcVarFrameSetInfo VMCv20130304 Strateva parameter, a, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
ksaStratPht vmcVarFrameSetInfo VMCv20130805 Strateva parameter, a, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
ksaStratPht vmcVarFrameSetInfo VMCv20140428 Strateva parameter, a, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksaStratPht vmcVarFrameSetInfo VMCv20140903 Strateva parameter, a, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksaStratPht vmcVarFrameSetInfo VMCv20150309 Strateva parameter, a, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksaStratPht vmcVarFrameSetInfo VMCv20151218 Strateva parameter, a, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksaStratPht vmcVarFrameSetInfo VMCv20160311 Strateva parameter, a, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksaStratPht vmcVarFrameSetInfo VMCv20160822 Strateva parameter, a, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksaStratPht vmcVarFrameSetInfo VMCv20170109 Strateva parameter, a, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksaStratPht vmcVarFrameSetInfo VMCv20170411 Strateva parameter, a, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksaStratPht vmcVarFrameSetInfo VMCv20171101 Strateva parameter, a, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksaStratPht vmcVarFrameSetInfo VMCv20180702 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Ks band. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksaStratPht vmcVarFrameSetInfo VMCv20181120 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Ks band. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksaStratPht vvvVarFrameSetInfo VVVDR4 Strateva parameter, a, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksAverageConf vhsSource VHSDR1 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -99999999 meta.code
ksAverageConf vhsSource VHSDR2 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -99999999 meta.code
ksAverageConf vhsSource VHSDR3 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.K
ksAverageConf vhsSource VHSDR4 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.K
ksAverageConf vhsSource VHSv20120926 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -99999999 stat.likelihood;em.IR.NIR
ksAverageConf vhsSource VHSv20130417 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.NIR
ksAverageConf vhsSource VHSv20140409 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.K
ksAverageConf vhsSource VHSv20150108 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.K
ksAverageConf vhsSource VHSv20160114 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.K
ksAverageConf vhsSource VHSv20160507 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.K
ksAverageConf vhsSource VHSv20170630 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.K
ksAverageConf vhsSource VHSv20171207 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.K
ksAverageConf vhsSource VHSv20180419 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.K
ksAverageConf vikingSource VIKINGDR2 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -99999999 meta.code
ksAverageConf vikingSource VIKINGDR3 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -99999999 stat.likelihood;em.IR.NIR
ksAverageConf vikingSource VIKINGDR4 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.K
ksAverageConf vikingSource VIKINGv20110714 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -99999999 meta.code
ksAverageConf vikingSource VIKINGv20111019 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -99999999 meta.code
ksAverageConf vikingSource VIKINGv20130417 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.NIR
ksAverageConf vikingSource VIKINGv20140402 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.NIR
ksAverageConf vikingSource VIKINGv20150421 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.K
ksAverageConf vikingSource VIKINGv20151230 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.K
ksAverageConf vikingSource VIKINGv20160406 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.K
ksAverageConf vikingSource VIKINGv20161202 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.K
ksAverageConf vikingSource VIKINGv20170715 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.K
ksAverageConf vikingSource VIKINGv20181012 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.K
ksAverageConf vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.NIR
ksAverageConf vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.NIR
ksAverageConf vmcSource VMCDR2 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.NIR
ksAverageConf vmcSource VMCDR3 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.K
ksAverageConf vmcSource VMCDR4 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.K
ksAverageConf vmcSource VMCv20110816 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -99999999 meta.code
ksAverageConf vmcSource VMCv20110909 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -99999999 meta.code
ksAverageConf vmcSource VMCv20120126 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -99999999 meta.code
ksAverageConf vmcSource VMCv20121128 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -99999999 stat.likelihood;em.IR.NIR
ksAverageConf vmcSource VMCv20130304 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.NIR
ksAverageConf vmcSource VMCv20130805 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.NIR
ksAverageConf vmcSource VMCv20140428 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.K
ksAverageConf vmcSource VMCv20140903 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.K
ksAverageConf vmcSource VMCv20150309 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.K
ksAverageConf vmcSource VMCv20151218 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.K
ksAverageConf vmcSource VMCv20160311 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.K
ksAverageConf vmcSource VMCv20160822 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.K
ksAverageConf vmcSource VMCv20170109 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.K
ksAverageConf vmcSource VMCv20170411 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.K
ksAverageConf vmcSource VMCv20171101 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.K
ksAverageConf vmcSource VMCv20180702 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.K
ksAverageConf vmcSource VMCv20181120 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.K
ksAverageConf vmcSource, vmcSynopticSource VMCDR1 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -99999999 meta.code
ksAverageConf vvvSource, vvvSynopticSource VVVDR4 average confidence in 2 arcsec diameter default aperture (aper3) Ks real 4   -0.9999995e9 stat.likelihood;em.IR.K
ksbestAper videoVariability VIDEODR2 Best aperture (1-6) for photometric statistics in the Ks 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)
ksbestAper videoVariability VIDEODR3 Best aperture (1-6) for photometric statistics in the Ks band int 4   -9999 meta.code.class;em.IR.NIR
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)
ksbestAper videoVariability VIDEODR4 Best aperture (1-6) for photometric statistics in the Ks band int 4   -9999 meta.code.class;em.IR.K
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)
ksbestAper videoVariability VIDEODR5 Best aperture (1-6) for photometric statistics in the Ks band int 4   -9999 meta.code.class;em.IR.K
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)
ksbestAper videoVariability VIDEOv20100513 Best aperture (1-6) for photometric statistics in the Ks 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)
ksbestAper videoVariability VIDEOv20111208 Best aperture (1-6) for photometric statistics in the Ks 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)
ksbestAper vikingVariability VIKINGDR2 Best aperture (1-6) for photometric statistics in the Ks 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)
ksbestAper vikingVariability VIKINGv20110714 Best aperture (1-6) for photometric statistics in the Ks 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)
ksbestAper vikingVariability VIKINGv20111019 Best aperture (1-6) for photometric statistics in the Ks 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)
ksbestAper vmcVariability VMCDR1 Best aperture (1-6) for photometric statistics in the Ks 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)
ksbestAper vmcVariability VMCDR2 Best aperture (1-6) for photometric statistics in the Ks band int 4   -9999 meta.code.class;em.IR.NIR
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)
ksbestAper vmcVariability VMCDR3 Best aperture (1-6) for photometric statistics in the Ks band int 4   -9999 meta.code.class;em.IR.K
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)
ksbestAper vmcVariability VMCDR4 Best aperture (1-6) for photometric statistics in the Ks band int 4   -9999 meta.code.class;em.IR.K
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)
ksbestAper vmcVariability VMCv20110816 Best aperture (1-6) for photometric statistics in the Ks 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)
ksbestAper vmcVariability VMCv20110909 Best aperture (1-6) for photometric statistics in the Ks 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)
ksbestAper vmcVariability VMCv20120126 Best aperture (1-6) for photometric statistics in the Ks 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)
ksbestAper vmcVariability VMCv20121128 Best aperture (1-6) for photometric statistics in the Ks band int 4   -9999 meta.code.class;em.IR.NIR
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)
ksbestAper vmcVariability VMCv20130304 Best aperture (1-6) for photometric statistics in the Ks band int 4   -9999 meta.code.class;em.IR.NIR
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)
ksbestAper vmcVariability VMCv20130805 Best aperture (1-6) for photometric statistics in the Ks band int 4   -9999 meta.code.class;em.IR.NIR
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)
ksbestAper vmcVariability VMCv20140428 Best aperture (1-6) for photometric statistics in the Ks band int 4   -9999 meta.code.class;em.IR.K
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)
ksbestAper vmcVariability VMCv20140903 Best aperture (1-6) for photometric statistics in the Ks band int 4   -9999 meta.code.class;em.IR.K
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)
ksbestAper vmcVariability VMCv20150309 Best aperture (1-6) for photometric statistics in the Ks band int 4   -9999 meta.code.class;em.IR.K
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)
ksbestAper vmcVariability VMCv20151218 Best aperture (1-6) for photometric statistics in the Ks band int 4   -9999 meta.code.class;em.IR.K
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)
ksbestAper vmcVariability VMCv20160311 Best aperture (1-6) for photometric statistics in the Ks band int 4   -9999 meta.code.class;em.IR.K
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)
ksbestAper vmcVariability VMCv20160822 Best aperture (1-6) for photometric statistics in the Ks band int 4   -9999 meta.code.class;em.IR.K
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)
ksbestAper vmcVariability VMCv20170109 Best aperture (1-6) for photometric statistics in the Ks band int 4   -9999 meta.code.class;em.IR.K
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)
ksbestAper vmcVariability VMCv20170411 Best aperture (1-6) for photometric statistics in the Ks band int 4   -9999 meta.code.class;em.IR.K
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)
ksbestAper vmcVariability VMCv20171101 Best aperture (1-6) for photometric statistics in the Ks band int 4   -9999 meta.code.class;em.IR.K
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)
ksbestAper vmcVariability VMCv20180702 Best aperture (1-6) for photometric statistics in the Ks band int 4   -9999 meta.code.class;em.IR.K
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)
ksbestAper vmcVariability VMCv20181120 Best aperture (1-6) for photometric statistics in the Ks band int 4   -9999 meta.code.class;em.IR.K
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)
ksbestAper vvvVariability VVVDR4 Best aperture (1-6) for photometric statistics in the Ks band int 4   -9999 meta.code.class;em.IR.K
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)
ksbStratAst videoVarFrameSetInfo VIDEODR2 Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks 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.
ksbStratAst videoVarFrameSetInfo VIDEODR3 Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
ksbStratAst videoVarFrameSetInfo VIDEODR4 Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksbStratAst videoVarFrameSetInfo VIDEODR5 Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksbStratAst videoVarFrameSetInfo VIDEOv20100513 Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks 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.
ksbStratAst videoVarFrameSetInfo VIDEOv20111208 Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks 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.
ksbStratAst vikingVarFrameSetInfo VIKINGDR2 Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks 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.
ksbStratAst vikingVarFrameSetInfo VIKINGv20110714 Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks 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.
ksbStratAst vikingVarFrameSetInfo VIKINGv20111019 Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks 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.
ksbStratAst vmcVarFrameSetInfo VMCDR1 Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks 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.
ksbStratAst vmcVarFrameSetInfo VMCDR2 Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
ksbStratAst vmcVarFrameSetInfo VMCDR3 Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksbStratAst vmcVarFrameSetInfo VMCDR4 Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksbStratAst vmcVarFrameSetInfo VMCv20110816 Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks 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.
ksbStratAst vmcVarFrameSetInfo VMCv20110909 Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks 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.
ksbStratAst vmcVarFrameSetInfo VMCv20120126 Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks 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.
ksbStratAst vmcVarFrameSetInfo VMCv20121128 Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
ksbStratAst vmcVarFrameSetInfo VMCv20130304 Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
ksbStratAst vmcVarFrameSetInfo VMCv20130805 Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
ksbStratAst vmcVarFrameSetInfo VMCv20140428 Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksbStratAst vmcVarFrameSetInfo VMCv20140903 Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksbStratAst vmcVarFrameSetInfo VMCv20150309 Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksbStratAst vmcVarFrameSetInfo VMCv20151218 Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksbStratAst vmcVarFrameSetInfo VMCv20160311 Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksbStratAst vmcVarFrameSetInfo VMCv20160822 Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksbStratAst vmcVarFrameSetInfo VMCv20170109 Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksbStratAst vmcVarFrameSetInfo VMCv20170411 Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksbStratAst vmcVarFrameSetInfo VMCv20171101 Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksbStratAst vmcVarFrameSetInfo VMCv20180702 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Ks band. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksbStratAst vmcVarFrameSetInfo VMCv20181120 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Ks band. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksbStratAst vvvVarFrameSetInfo VVVDR4 Strateva parameter, b, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksbStratPht videoVarFrameSetInfo VIDEODR2 Strateva parameter, b, in fit to photometric rms vs magnitude in Ks 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.
ksbStratPht videoVarFrameSetInfo VIDEODR3 Strateva parameter, b, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
ksbStratPht videoVarFrameSetInfo VIDEODR4 Strateva parameter, b, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksbStratPht videoVarFrameSetInfo VIDEODR5 Strateva parameter, b, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksbStratPht videoVarFrameSetInfo VIDEOv20100513 Strateva parameter, b, in fit to photometric rms vs magnitude in Ks 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.
ksbStratPht videoVarFrameSetInfo VIDEOv20111208 Strateva parameter, b, in fit to photometric rms vs magnitude in Ks 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.
ksbStratPht vikingVarFrameSetInfo VIKINGDR2 Strateva parameter, b, in fit to photometric rms vs magnitude in Ks 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.
ksbStratPht vikingVarFrameSetInfo VIKINGv20110714 Strateva parameter, b, in fit to photometric rms vs magnitude in Ks 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.
ksbStratPht vikingVarFrameSetInfo VIKINGv20111019 Strateva parameter, b, in fit to photometric rms vs magnitude in Ks 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.
ksbStratPht vmcVarFrameSetInfo VMCDR1 Strateva parameter, b, in fit to photometric rms vs magnitude in Ks 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.
ksbStratPht vmcVarFrameSetInfo VMCDR2 Strateva parameter, b, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
ksbStratPht vmcVarFrameSetInfo VMCDR3 Strateva parameter, b, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksbStratPht vmcVarFrameSetInfo VMCDR4 Strateva parameter, b, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksbStratPht vmcVarFrameSetInfo VMCv20110816 Strateva parameter, b, in fit to photometric rms vs magnitude in Ks 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.
ksbStratPht vmcVarFrameSetInfo VMCv20110909 Strateva parameter, b, in fit to photometric rms vs magnitude in Ks 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.
ksbStratPht vmcVarFrameSetInfo VMCv20120126 Strateva parameter, b, in fit to photometric rms vs magnitude in Ks 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.
ksbStratPht vmcVarFrameSetInfo VMCv20121128 Strateva parameter, b, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
ksbStratPht vmcVarFrameSetInfo VMCv20130304 Strateva parameter, b, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
ksbStratPht vmcVarFrameSetInfo VMCv20130805 Strateva parameter, b, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
ksbStratPht vmcVarFrameSetInfo VMCv20140428 Strateva parameter, b, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksbStratPht vmcVarFrameSetInfo VMCv20140903 Strateva parameter, b, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksbStratPht vmcVarFrameSetInfo VMCv20150309 Strateva parameter, b, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksbStratPht vmcVarFrameSetInfo VMCv20151218 Strateva parameter, b, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksbStratPht vmcVarFrameSetInfo VMCv20160311 Strateva parameter, b, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksbStratPht vmcVarFrameSetInfo VMCv20160822 Strateva parameter, b, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksbStratPht vmcVarFrameSetInfo VMCv20170109 Strateva parameter, b, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksbStratPht vmcVarFrameSetInfo VMCv20170411 Strateva parameter, b, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksbStratPht vmcVarFrameSetInfo VMCv20171101 Strateva parameter, b, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksbStratPht vmcVarFrameSetInfo VMCv20180702 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Ks band. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksbStratPht vmcVarFrameSetInfo VMCv20181120 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Ks band. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksbStratPht vvvVarFrameSetInfo VVVDR4 Strateva parameter, b, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
kschiSqAst videoVarFrameSetInfo VIDEODR2 Goodness of fit of Strateva function to astrometric data in Ks 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.
kschiSqAst videoVarFrameSetInfo VIDEODR3 Goodness of fit of Strateva function to astrometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
kschiSqAst videoVarFrameSetInfo VIDEODR4 Goodness of fit of Strateva function to astrometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.K
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.
kschiSqAst videoVarFrameSetInfo VIDEODR5 Goodness of fit of Strateva function to astrometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.K
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.
kschiSqAst videoVarFrameSetInfo VIDEOv20100513 Goodness of fit of Strateva function to astrometric data in Ks 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.
kschiSqAst videoVarFrameSetInfo VIDEOv20111208 Goodness of fit of Strateva function to astrometric data in Ks 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.
kschiSqAst vikingVarFrameSetInfo VIKINGDR2 Goodness of fit of Strateva function to astrometric data in Ks 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.
kschiSqAst vikingVarFrameSetInfo VIKINGv20110714 Goodness of fit of Strateva function to astrometric data in Ks 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.
kschiSqAst vikingVarFrameSetInfo VIKINGv20111019 Goodness of fit of Strateva function to astrometric data in Ks 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.
kschiSqAst vmcVarFrameSetInfo VMCDR1 Goodness of fit of Strateva function to astrometric data in Ks 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.
kschiSqAst vmcVarFrameSetInfo VMCDR2 Goodness of fit of Strateva function to astrometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
kschiSqAst vmcVarFrameSetInfo VMCDR3 Goodness of fit of Strateva function to astrometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.K
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.
kschiSqAst vmcVarFrameSetInfo VMCDR4 Goodness of fit of Strateva function to astrometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.K
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.
kschiSqAst vmcVarFrameSetInfo VMCv20110816 Goodness of fit of Strateva function to astrometric data in Ks 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.
kschiSqAst vmcVarFrameSetInfo VMCv20110909 Goodness of fit of Strateva function to astrometric data in Ks 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.
kschiSqAst vmcVarFrameSetInfo VMCv20120126 Goodness of fit of Strateva function to astrometric data in Ks 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.
kschiSqAst vmcVarFrameSetInfo VMCv20121128 Goodness of fit of Strateva function to astrometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
kschiSqAst vmcVarFrameSetInfo VMCv20130304 Goodness of fit of Strateva function to astrometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
kschiSqAst vmcVarFrameSetInfo VMCv20130805 Goodness of fit of Strateva function to astrometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
kschiSqAst vmcVarFrameSetInfo VMCv20140428 Goodness of fit of Strateva function to astrometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.K
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.
kschiSqAst vmcVarFrameSetInfo VMCv20140903 Goodness of fit of Strateva function to astrometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.K
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.
kschiSqAst vmcVarFrameSetInfo VMCv20150309 Goodness of fit of Strateva function to astrometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.K
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.
kschiSqAst vmcVarFrameSetInfo VMCv20151218 Goodness of fit of Strateva function to astrometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.K
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.
kschiSqAst vmcVarFrameSetInfo VMCv20160311 Goodness of fit of Strateva function to astrometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.K
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.
kschiSqAst vmcVarFrameSetInfo VMCv20160822 Goodness of fit of Strateva function to astrometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.K
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.
kschiSqAst vmcVarFrameSetInfo VMCv20170109 Goodness of fit of Strateva function to astrometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.K
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.
kschiSqAst vmcVarFrameSetInfo VMCv20170411 Goodness of fit of Strateva function to astrometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.K
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.
kschiSqAst vmcVarFrameSetInfo VMCv20171101 Goodness of fit of Strateva function to astrometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.K
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.
kschiSqAst vmcVarFrameSetInfo VMCv20180702 Goodness of fit of Strateva function to astrometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.K
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.
kschiSqAst vmcVarFrameSetInfo VMCv20181120 Goodness of fit of Strateva function to astrometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.K
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.
kschiSqAst vvvVarFrameSetInfo VVVDR4 Goodness of fit of Strateva function to astrometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.K
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.
kschiSqpd videoVariability VIDEODR2 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9  
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.
kschiSqpd videoVariability VIDEODR3 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.
kschiSqpd videoVariability VIDEODR4 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.K
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.
kschiSqpd videoVariability VIDEODR5 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.K
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.
kschiSqpd videoVariability VIDEOv20100513 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9  
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.
kschiSqpd videoVariability VIDEOv20111208 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9  
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.
kschiSqpd vikingVariability VIKINGDR2 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9  
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.
kschiSqpd vikingVariability VIKINGv20110714 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9  
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.
kschiSqpd vikingVariability VIKINGv20111019 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9  
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.
kschiSqpd vmcVariability VMCDR1 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.
kschiSqpd vmcVariability VMCDR2 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.
kschiSqpd vmcVariability VMCDR3 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.K
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.
kschiSqpd vmcVariability VMCDR4 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.K
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.
kschiSqpd vmcVariability VMCv20110816 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.
kschiSqpd vmcVariability VMCv20110909 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.
kschiSqpd vmcVariability VMCv20120126 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.
kschiSqpd vmcVariability VMCv20121128 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.
kschiSqpd vmcVariability VMCv20130304 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.
kschiSqpd vmcVariability VMCv20130805 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.
kschiSqpd vmcVariability VMCv20140428 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.K
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.
kschiSqpd vmcVariability VMCv20140903 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.K
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.
kschiSqpd vmcVariability VMCv20150309 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.K
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.
kschiSqpd vmcVariability VMCv20151218 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.K
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.
kschiSqpd vmcVariability VMCv20160311 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.K
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.
kschiSqpd vmcVariability VMCv20160822 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.K
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.
kschiSqpd vmcVariability VMCv20170109 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.K
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.
kschiSqpd vmcVariability VMCv20170411 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.K
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.
kschiSqpd vmcVariability VMCv20171101 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.K
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.
kschiSqpd vmcVariability VMCv20180702 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.K
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.
kschiSqpd vmcVariability VMCv20181120 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.K
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.
kschiSqpd vvvVariability VVVDR4 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.K
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.
kschiSqPht videoVarFrameSetInfo VIDEODR2 Goodness of fit of Strateva function to photometric data in Ks 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.
kschiSqPht videoVarFrameSetInfo VIDEODR3 Goodness of fit of Strateva function to photometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
kschiSqPht videoVarFrameSetInfo VIDEODR4 Goodness of fit of Strateva function to photometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.K
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.
kschiSqPht videoVarFrameSetInfo VIDEODR5 Goodness of fit of Strateva function to photometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.K
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.
kschiSqPht videoVarFrameSetInfo VIDEOv20100513 Goodness of fit of Strateva function to photometric data in Ks 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.
kschiSqPht videoVarFrameSetInfo VIDEOv20111208 Goodness of fit of Strateva function to photometric data in Ks 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.
kschiSqPht vikingVarFrameSetInfo VIKINGDR2 Goodness of fit of Strateva function to photometric data in Ks 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.
kschiSqPht vikingVarFrameSetInfo VIKINGv20110714 Goodness of fit of Strateva function to photometric data in Ks 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.
kschiSqPht vikingVarFrameSetInfo VIKINGv20111019 Goodness of fit of Strateva function to photometric data in Ks 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.
kschiSqPht vmcVarFrameSetInfo VMCDR1 Goodness of fit of Strateva function to photometric data in Ks 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.
kschiSqPht vmcVarFrameSetInfo VMCDR2 Goodness of fit of Strateva function to photometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
kschiSqPht vmcVarFrameSetInfo VMCDR3 Goodness of fit of Strateva function to photometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.K
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.
kschiSqPht vmcVarFrameSetInfo VMCDR4 Goodness of fit of Strateva function to photometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.K
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.
kschiSqPht vmcVarFrameSetInfo VMCv20110816 Goodness of fit of Strateva function to photometric data in Ks 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.
kschiSqPht vmcVarFrameSetInfo VMCv20110909 Goodness of fit of Strateva function to photometric data in Ks 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.
kschiSqPht vmcVarFrameSetInfo VMCv20120126 Goodness of fit of Strateva function to photometric data in Ks 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.
kschiSqPht vmcVarFrameSetInfo VMCv20121128 Goodness of fit of Strateva function to photometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
kschiSqPht vmcVarFrameSetInfo VMCv20130304 Goodness of fit of Strateva function to photometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
kschiSqPht vmcVarFrameSetInfo VMCv20130805 Goodness of fit of Strateva function to photometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
kschiSqPht vmcVarFrameSetInfo VMCv20140428 Goodness of fit of Strateva function to photometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.K
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.
kschiSqPht vmcVarFrameSetInfo VMCv20140903 Goodness of fit of Strateva function to photometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.K
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.
kschiSqPht vmcVarFrameSetInfo VMCv20150309 Goodness of fit of Strateva function to photometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.K
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.
kschiSqPht vmcVarFrameSetInfo VMCv20151218 Goodness of fit of Strateva function to photometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.K
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.
kschiSqPht vmcVarFrameSetInfo VMCv20160311 Goodness of fit of Strateva function to photometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.K
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.
kschiSqPht vmcVarFrameSetInfo VMCv20160822 Goodness of fit of Strateva function to photometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.K
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.
kschiSqPht vmcVarFrameSetInfo VMCv20170109 Goodness of fit of Strateva function to photometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.K
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.
kschiSqPht vmcVarFrameSetInfo VMCv20170411 Goodness of fit of Strateva function to photometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.K
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.
kschiSqPht vmcVarFrameSetInfo VMCv20171101 Goodness of fit of Strateva function to photometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.K
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.
kschiSqPht vmcVarFrameSetInfo VMCv20180702 Goodness of fit of Strateva function to photometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.K
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.
kschiSqPht vmcVarFrameSetInfo VMCv20181120 Goodness of fit of Strateva function to photometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.K
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.
kschiSqPht vvvVarFrameSetInfo VVVDR4 Goodness of fit of Strateva function to photometric data in Ks band real 4   -0.9999995e9 stat.fit.goodness;em.IR.K
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.
ksClass vhsSource VHSDR2 discrete image classification flag in Ks smallint 2   -9999 src.class
ksClass vhsSource VHSDR3 discrete image classification flag in Ks smallint 2   -9999 src.class;em.IR.K
ksClass vhsSource VHSDR4 discrete image classification flag in Ks smallint 2   -9999 src.class;em.IR.K
ksClass vhsSource VHSv20120926 discrete image classification flag in Ks smallint 2   -9999 src.class
ksClass vhsSource VHSv20130417 discrete image classification flag in Ks smallint 2   -9999 src.class
ksClass vhsSource VHSv20140409 discrete image classification flag in Ks smallint 2   -9999 src.class;em.IR.K
ksClass vhsSource VHSv20150108 discrete image classification flag in Ks smallint 2   -9999 src.class;em.IR.K
ksClass vhsSource VHSv20160114 discrete image classification flag in Ks smallint 2   -9999 src.class;em.IR.K
ksClass vhsSource VHSv20160507 discrete image classification flag in Ks smallint 2   -9999 src.class;em.IR.K
ksClass vhsSource VHSv20170630 discrete image classification flag in Ks smallint 2   -9999 src.class;em.IR.K
ksClass vhsSource VHSv20171207 discrete image classification flag in Ks smallint 2   -9999 src.class;em.IR.K
ksClass vhsSource VHSv20180419 discrete image classification flag in Ks smallint 2   -9999 src.class;em.IR.K
ksClass vhsSource, vhsSourceRemeasurement VHSDR1 discrete image classification flag in Ks smallint 2   -9999 src.class
ksClass videoSource VIDEODR2 discrete image classification flag in Ks smallint 2   -9999 src.class
ksClass videoSource VIDEODR3 discrete image classification flag in Ks smallint 2   -9999 src.class
ksClass videoSource VIDEODR4 discrete image classification flag in Ks smallint 2   -9999 src.class;em.IR.K
ksClass videoSource VIDEODR5 discrete image classification flag in Ks smallint 2   -9999 src.class;em.IR.K
ksClass videoSource VIDEOv20111208 discrete image classification flag in Ks smallint 2   -9999 src.class
ksClass videoSource, videoSourceRemeasurement VIDEOv20100513 discrete image classification flag in Ks smallint 2   -9999 src.class
ksClass vikingSource VIKINGDR2 discrete image classification flag in Ks smallint 2   -9999 src.class
ksClass vikingSource VIKINGDR3 discrete image classification flag in Ks smallint 2   -9999 src.class
ksClass vikingSource VIKINGDR4 discrete image classification flag in Ks smallint 2   -9999 src.class;em.IR.K
ksClass vikingSource VIKINGv20111019 discrete image classification flag in Ks smallint 2   -9999 src.class
ksClass vikingSource VIKINGv20130417 discrete image classification flag in Ks smallint 2   -9999 src.class
ksClass vikingSource VIKINGv20140402 discrete image classification flag in Ks smallint 2   -9999 src.class
ksClass vikingSource VIKINGv20150421 discrete image classification flag in Ks smallint 2   -9999 src.class;em.IR.K
ksClass vikingSource VIKINGv20151230 discrete image classification flag in Ks smallint 2   -9999 src.class;em.IR.K
ksClass vikingSource VIKINGv20160406 discrete image classification flag in Ks smallint 2   -9999 src.class;em.IR.K
ksClass vikingSource VIKINGv20161202 discrete image classification flag in Ks smallint 2   -9999 src.class;em.IR.K
ksClass vikingSource VIKINGv20170715 discrete image classification flag in Ks smallint 2   -9999 src.class;em.IR.K
ksClass vikingSource VIKINGv20181012 discrete image classification flag in Ks smallint 2   -9999 src.class;em.IR.K
ksClass vikingSource, vikingSourceRemeasurement VIKINGv20110714 discrete image classification flag in Ks smallint 2   -9999 src.class
ksClass vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 discrete image classification flag in Ks smallint 2   -9999 src.class
ksClass vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 discrete image classification flag in Ks smallint 2   -9999 src.class
ksClass vmcSource VMCDR2 discrete image classification flag in Ks smallint 2   -9999 src.class
ksClass vmcSource VMCDR3 discrete image classification flag in Ks smallint 2   -9999 src.class;em.IR.K
ksClass vmcSource VMCDR4 discrete image classification flag in Ks smallint 2   -9999 src.class;em.IR.K
ksClass vmcSource VMCv20110909 discrete image classification flag in Ks smallint 2   -9999 src.class
ksClass vmcSource VMCv20120126 discrete image classification flag in Ks smallint 2   -9999 src.class
ksClass vmcSource VMCv20121128 discrete image classification flag in Ks smallint 2   -9999 src.class
ksClass vmcSource VMCv20130304 discrete image classification flag in Ks smallint 2   -9999 src.class
ksClass vmcSource VMCv20130805 discrete image classification flag in Ks smallint 2   -9999 src.class
ksClass vmcSource VMCv20140428 discrete image classification flag in Ks smallint 2   -9999 src.class;em.IR.K
ksClass vmcSource VMCv20140903 discrete image classification flag in Ks smallint 2   -9999 src.class;em.IR.K
ksClass vmcSource VMCv20150309 discrete image classification flag in Ks smallint 2   -9999 src.class;em.IR.K
ksClass vmcSource VMCv20151218 discrete image classification flag in Ks smallint 2   -9999 src.class;em.IR.K
ksClass vmcSource VMCv20160311 discrete image classification flag in Ks smallint 2   -9999 src.class;em.IR.K
ksClass vmcSource VMCv20160822 discrete image classification flag in Ks smallint 2   -9999 src.class;em.IR.K
ksClass vmcSource VMCv20170109 discrete image classification flag in Ks smallint 2   -9999 src.class;em.IR.K
ksClass vmcSource VMCv20170411 discrete image classification flag in Ks smallint 2   -9999 src.class;em.IR.K
ksClass vmcSource VMCv20171101 discrete image classification flag in Ks smallint 2   -9999 src.class;em.IR.K
ksClass vmcSource VMCv20180702 discrete image classification flag in Ks smallint 2   -9999 src.class;em.IR.K
ksClass vmcSource VMCv20181120 discrete image classification flag in Ks smallint 2   -9999 src.class;em.IR.K
ksClass vmcSource, vmcSourceRemeasurement VMCv20110816 discrete image classification flag in Ks smallint 2   -9999 src.class
ksClass vmcSource, vmcSynopticSource VMCDR1 discrete image classification flag in Ks smallint 2   -9999 src.class
ksClass vvvSource, vvvSynopticSource VVVDR4 discrete image classification flag in Ks smallint 2   -9999 src.class;em.IR.K
ksClassStat vhsSource VHSDR2 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat
ksClassStat vhsSource VHSDR3 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat;em.IR.K
ksClassStat vhsSource VHSDR4 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat;em.IR.K
ksClassStat vhsSource VHSv20120926 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat
ksClassStat vhsSource VHSv20130417 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat
ksClassStat vhsSource VHSv20140409 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat;em.IR.K
ksClassStat vhsSource VHSv20150108 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat;em.IR.K
ksClassStat vhsSource VHSv20160114 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat;em.IR.K
ksClassStat vhsSource VHSv20160507 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat;em.IR.K
ksClassStat vhsSource VHSv20170630 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat;em.IR.K
ksClassStat vhsSource VHSv20171207 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat;em.IR.K
ksClassStat vhsSource VHSv20180419 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat;em.IR.K
ksClassStat vhsSource, vhsSourceRemeasurement VHSDR1 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat
ksClassStat videoSource VIDEODR2 S-Extractor classification statistic in Ks real 4   -0.9999995e9 stat
ksClassStat videoSource VIDEODR3 S-Extractor classification statistic in Ks real 4   -0.9999995e9 stat
ksClassStat videoSource VIDEODR4 S-Extractor classification statistic in Ks real 4   -0.9999995e9 stat;em.IR.K
ksClassStat videoSource VIDEODR5 S-Extractor classification statistic in Ks real 4   -0.9999995e9 stat;em.IR.K
ksClassStat videoSource VIDEOv20100513 S-Extractor classification statistic in Ks real 4   -0.9999995e9 stat
ksClassStat videoSource VIDEOv20111208 S-Extractor classification statistic in Ks real 4   -0.9999995e9 stat
ksClassStat videoSourceRemeasurement VIDEOv20100513 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat
ksClassStat vikingSource VIKINGDR2 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat
ksClassStat vikingSource VIKINGDR3 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat
ksClassStat vikingSource VIKINGDR4 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat;em.IR.K
ksClassStat vikingSource VIKINGv20111019 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat
ksClassStat vikingSource VIKINGv20130417 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat
ksClassStat vikingSource VIKINGv20140402 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat
ksClassStat vikingSource VIKINGv20150421 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat;em.IR.K
ksClassStat vikingSource VIKINGv20151230 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat;em.IR.K
ksClassStat vikingSource VIKINGv20160406 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat;em.IR.K
ksClassStat vikingSource VIKINGv20161202 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat;em.IR.K
ksClassStat vikingSource VIKINGv20170715 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat;em.IR.K
ksClassStat vikingSource VIKINGv20181012 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat;em.IR.K
ksClassStat vikingSource, vikingSourceRemeasurement VIKINGv20110714 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat
ksClassStat vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat
ksClassStat vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat
ksClassStat vmcSource VMCDR2 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat
ksClassStat vmcSource VMCDR3 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat;em.IR.K
ksClassStat vmcSource VMCDR4 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat;em.IR.K
ksClassStat vmcSource VMCv20110909 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat
ksClassStat vmcSource VMCv20120126 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat
ksClassStat vmcSource VMCv20121128 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat
ksClassStat vmcSource VMCv20130304 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat
ksClassStat vmcSource VMCv20130805 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat
ksClassStat vmcSource VMCv20140428 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat;em.IR.K
ksClassStat vmcSource VMCv20140903 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat;em.IR.K
ksClassStat vmcSource VMCv20150309 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat;em.IR.K
ksClassStat vmcSource VMCv20151218 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat;em.IR.K
ksClassStat vmcSource VMCv20160311 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat;em.IR.K
ksClassStat vmcSource VMCv20160822 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat;em.IR.K
ksClassStat vmcSource VMCv20170109 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat;em.IR.K
ksClassStat vmcSource VMCv20170411 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat;em.IR.K
ksClassStat vmcSource VMCv20171101 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat;em.IR.K
ksClassStat vmcSource VMCv20180702 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat;em.IR.K
ksClassStat vmcSource VMCv20181120 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat;em.IR.K
ksClassStat vmcSource, vmcSourceRemeasurement VMCv20110816 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat
ksClassStat vmcSource, vmcSynopticSource VMCDR1 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat
ksClassStat vvvSource VVVDR4 S-Extractor classification statistic in Ks real 4   -0.9999995e9 stat;em.IR.K
ksClassStat vvvSynopticSource VVVDR4 N(0,1) stellarness-of-profile statistic in Ks real 4   -0.9999995e9 stat;em.IR.K
kscStratAst videoVarFrameSetInfo VIDEODR2 Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks 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.
kscStratAst videoVarFrameSetInfo VIDEODR3 Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
kscStratAst videoVarFrameSetInfo VIDEODR4 Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
kscStratAst videoVarFrameSetInfo VIDEODR5 Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
kscStratAst videoVarFrameSetInfo VIDEOv20100513 Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks 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.
kscStratAst videoVarFrameSetInfo VIDEOv20111208 Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks 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.
kscStratAst vikingVarFrameSetInfo VIKINGDR2 Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks 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.
kscStratAst vikingVarFrameSetInfo VIKINGv20110714 Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks 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.
kscStratAst vikingVarFrameSetInfo VIKINGv20111019 Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks 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.
kscStratAst vmcVarFrameSetInfo VMCDR1 Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks 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.
kscStratAst vmcVarFrameSetInfo VMCDR2 Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
kscStratAst vmcVarFrameSetInfo VMCDR3 Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
kscStratAst vmcVarFrameSetInfo VMCDR4 Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
kscStratAst vmcVarFrameSetInfo VMCv20110816 Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks 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.
kscStratAst vmcVarFrameSetInfo VMCv20110909 Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks 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.
kscStratAst vmcVarFrameSetInfo VMCv20120126 Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks 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.
kscStratAst vmcVarFrameSetInfo VMCv20121128 Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
kscStratAst vmcVarFrameSetInfo VMCv20130304 Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
kscStratAst vmcVarFrameSetInfo VMCv20130805 Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
kscStratAst vmcVarFrameSetInfo VMCv20140428 Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
kscStratAst vmcVarFrameSetInfo VMCv20140903 Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
kscStratAst vmcVarFrameSetInfo VMCv20150309 Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
kscStratAst vmcVarFrameSetInfo VMCv20151218 Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
kscStratAst vmcVarFrameSetInfo VMCv20160311 Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
kscStratAst vmcVarFrameSetInfo VMCv20160822 Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
kscStratAst vmcVarFrameSetInfo VMCv20170109 Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
kscStratAst vmcVarFrameSetInfo VMCv20170411 Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
kscStratAst vmcVarFrameSetInfo VMCv20171101 Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
kscStratAst vmcVarFrameSetInfo VMCv20180702 Parameter, c2 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Ks band. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
kscStratAst vmcVarFrameSetInfo VMCv20181120 Parameter, c2 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Ks band. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
kscStratAst vvvVarFrameSetInfo VVVDR4 Strateva parameter, c, in fit to astrometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
kscStratPht videoVarFrameSetInfo VIDEODR2 Strateva parameter, c, in fit to photometric rms vs magnitude in Ks 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.
kscStratPht videoVarFrameSetInfo VIDEODR3 Strateva parameter, c, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
kscStratPht videoVarFrameSetInfo VIDEODR4 Strateva parameter, c, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
kscStratPht videoVarFrameSetInfo VIDEODR5 Strateva parameter, c, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
kscStratPht videoVarFrameSetInfo VIDEOv20100513 Strateva parameter, c, in fit to photometric rms vs magnitude in Ks 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.
kscStratPht videoVarFrameSetInfo VIDEOv20111208 Strateva parameter, c, in fit to photometric rms vs magnitude in Ks 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.
kscStratPht vikingVarFrameSetInfo VIKINGDR2 Strateva parameter, c, in fit to photometric rms vs magnitude in Ks 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.
kscStratPht vikingVarFrameSetInfo VIKINGv20110714 Strateva parameter, c, in fit to photometric rms vs magnitude in Ks 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.
kscStratPht vikingVarFrameSetInfo VIKINGv20111019 Strateva parameter, c, in fit to photometric rms vs magnitude in Ks 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.
kscStratPht vmcVarFrameSetInfo VMCDR1 Strateva parameter, c, in fit to photometric rms vs magnitude in Ks 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.
kscStratPht vmcVarFrameSetInfo VMCDR2 Strateva parameter, c, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
kscStratPht vmcVarFrameSetInfo VMCDR3 Strateva parameter, c, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
kscStratPht vmcVarFrameSetInfo VMCDR4 Strateva parameter, c, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
kscStratPht vmcVarFrameSetInfo VMCv20110816 Strateva parameter, c, in fit to photometric rms vs magnitude in Ks 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.
kscStratPht vmcVarFrameSetInfo VMCv20110909 Strateva parameter, c, in fit to photometric rms vs magnitude in Ks 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.
kscStratPht vmcVarFrameSetInfo VMCv20120126 Strateva parameter, c, in fit to photometric rms vs magnitude in Ks 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.
kscStratPht vmcVarFrameSetInfo VMCv20121128 Strateva parameter, c, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
kscStratPht vmcVarFrameSetInfo VMCv20130304 Strateva parameter, c, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
kscStratPht vmcVarFrameSetInfo VMCv20130805 Strateva parameter, c, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the 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.
kscStratPht vmcVarFrameSetInfo VMCv20140428 Strateva parameter, c, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
kscStratPht vmcVarFrameSetInfo VMCv20140903 Strateva parameter, c, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
kscStratPht vmcVarFrameSetInfo VMCv20150309 Strateva parameter, c, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
kscStratPht vmcVarFrameSetInfo VMCv20151218 Strateva parameter, c, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
kscStratPht vmcVarFrameSetInfo VMCv20160311 Strateva parameter, c, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
kscStratPht vmcVarFrameSetInfo VMCv20160822 Strateva parameter, c, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
kscStratPht vmcVarFrameSetInfo VMCv20170109 Strateva parameter, c, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
kscStratPht vmcVarFrameSetInfo VMCv20170411 Strateva parameter, c, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
kscStratPht vmcVarFrameSetInfo VMCv20171101 Strateva parameter, c, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
kscStratPht vmcVarFrameSetInfo VMCv20180702 Parameter, c2 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Ks band. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
kscStratPht vmcVarFrameSetInfo VMCv20181120 Parameter, c2 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Ks band. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
kscStratPht vvvVarFrameSetInfo VVVDR4 Strateva parameter, c, in fit to photometric rms vs magnitude in Ks band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.K
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.
ksDeblend vhsSourceRemeasurement VHSDR1 placeholder flag indicating parent/child relation in Ks int 4   -99999999 meta.code
ksDeblend videoSource, videoSourceRemeasurement VIDEOv20100513 placeholder flag indicating parent/child relation in Ks int 4   -99999999 meta.code
ksDeblend vikingSourceRemeasurement VIKINGv20110714 placeholder flag indicating parent/child relation in Ks int 4   -99999999 meta.code
ksDeblend vikingSourceRemeasurement VIKINGv20111019 placeholder flag indicating parent/child relation in Ks int 4   -99999999 meta.code
ksDeblend vmcSourceRemeasurement VMCv20110816 placeholder flag indicating parent/child relation in Ks int 4   -99999999 meta.code
ksDeblend vmcSourceRemeasurement VMCv20110909 placeholder flag indicating parent/child relation in Ks int 4   -99999999 meta.code
ksEll vhsSource VHSDR2 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity
ksEll vhsSource VHSDR3 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity;em.IR.K
ksEll vhsSource VHSDR4 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity;em.IR.K
ksEll vhsSource VHSv20120926 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity
ksEll vhsSource VHSv20130417 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity
ksEll vhsSource VHSv20140409 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity;em.IR.K
ksEll vhsSource VHSv20150108 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity;em.IR.K
ksEll vhsSource VHSv20160114 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity;em.IR.K
ksEll vhsSource VHSv20160507 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity;em.IR.K
ksEll vhsSource VHSv20170630 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity;em.IR.K
ksEll vhsSource VHSv20171207 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity;em.IR.K
ksEll vhsSource VHSv20180419 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity;em.IR.K
ksEll vhsSource, vhsSourceRemeasurement VHSDR1 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity
ksEll videoSource VIDEODR2 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity
ksEll videoSource VIDEODR3 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity
ksEll videoSource VIDEODR4 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity;em.IR.K
ksEll videoSource VIDEODR5 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity;em.IR.K
ksEll videoSource VIDEOv20111208 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity
ksEll videoSource, videoSourceRemeasurement VIDEOv20100513 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity
ksEll vikingSource VIKINGDR2 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity
ksEll vikingSource VIKINGDR3 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity
ksEll vikingSource VIKINGDR4 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity;em.IR.K
ksEll vikingSource VIKINGv20111019 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity
ksEll vikingSource VIKINGv20130417 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity
ksEll vikingSource VIKINGv20140402 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity
ksEll vikingSource VIKINGv20150421 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity;em.IR.K
ksEll vikingSource VIKINGv20151230 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity;em.IR.K
ksEll vikingSource VIKINGv20160406 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity;em.IR.K
ksEll vikingSource VIKINGv20161202 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity;em.IR.K
ksEll vikingSource VIKINGv20170715 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity;em.IR.K
ksEll vikingSource VIKINGv20181012 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity;em.IR.K
ksEll vikingSource, vikingSourceRemeasurement VIKINGv20110714 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity
ksEll vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity
ksEll vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity
ksEll vmcSource VMCDR2 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity
ksEll vmcSource VMCDR3 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity;em.IR.K
ksEll vmcSource VMCDR4 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity;em.IR.K
ksEll vmcSource VMCv20110909 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity
ksEll vmcSource VMCv20120126 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity
ksEll vmcSource VMCv20121128 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity
ksEll vmcSource VMCv20130304 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity
ksEll vmcSource VMCv20130805 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity
ksEll vmcSource VMCv20140428 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity;em.IR.K
ksEll vmcSource VMCv20140903 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity;em.IR.K
ksEll vmcSource VMCv20150309 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity;em.IR.K
ksEll vmcSource VMCv20151218 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity;em.IR.K
ksEll vmcSource VMCv20160311 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity;em.IR.K
ksEll vmcSource VMCv20160822 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity;em.IR.K
ksEll vmcSource VMCv20170109 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity;em.IR.K
ksEll vmcSource VMCv20170411 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity;em.IR.K
ksEll vmcSource VMCv20171101 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity;em.IR.K
ksEll vmcSource VMCv20180702 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity;em.IR.K
ksEll vmcSource VMCv20181120 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity;em.IR.K
ksEll vmcSource, vmcSourceRemeasurement VMCv20110816 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity
ksEll vmcSource, vmcSynopticSource VMCDR1 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity
ksEll vvvSource, vvvSynopticSource VVVDR4 1-b/a, where a/b=semi-major/minor axes in Ks real 4   -0.9999995e9 src.ellipticity;em.IR.K
kseNum vhsMergeLog VHSDR1 the extension number of this Ks frame tinyint 1     meta.number
kseNum vhsMergeLog VHSDR2 the extension number of this Ks frame tinyint 1     meta.number
kseNum vhsMergeLog VHSDR3 the extension number of this Ks frame tinyint 1     meta.number;em.IR.K
kseNum vhsMergeLog VHSDR4 the extension number of this Ks frame tinyint 1     meta.number;em.IR.K
kseNum vhsMergeLog VHSv20120926 the extension number of this Ks frame tinyint 1     meta.number
kseNum vhsMergeLog VHSv20130417 the extension number of this Ks frame tinyint 1     meta.number
kseNum vhsMergeLog VHSv20140409 the extension number of this Ks frame tinyint 1     meta.number;em.IR.K
kseNum vhsMergeLog VHSv20150108 the extension number of this Ks frame tinyint 1     meta.number;em.IR.K
kseNum vhsMergeLog VHSv20160114 the extension number of this Ks frame tinyint 1     meta.number;em.IR.K
kseNum vhsMergeLog VHSv20160507 the extension number of this Ks frame tinyint 1     meta.number;em.IR.K
kseNum vhsMergeLog VHSv20170630 the extension number of this Ks frame tinyint 1     meta.number;em.IR.K
kseNum vhsMergeLog VHSv20171207 the extension number of this Ks frame tinyint 1     meta.number;em.IR.K
kseNum vhsMergeLog VHSv20180419 the extension number of this Ks frame tinyint 1     meta.number;em.IR.K
kseNum videoMergeLog VIDEODR2 the extension number of this Ks frame tinyint 1     meta.number
kseNum videoMergeLog VIDEODR3 the extension number of this Ks frame tinyint 1     meta.number
kseNum videoMergeLog VIDEODR4 the extension number of this Ks frame tinyint 1     meta.number;em.IR.K
kseNum videoMergeLog VIDEODR5 the extension number of this Ks frame tinyint 1     meta.number;em.IR.K
kseNum videoMergeLog VIDEOv20100513 the extension number of this Ks frame tinyint 1     meta.number
kseNum videoMergeLog VIDEOv20111208 the extension number of this Ks frame tinyint 1     meta.number
kseNum vikingMergeLog VIKINGDR2 the extension number of this Ks frame tinyint 1     meta.number
kseNum vikingMergeLog VIKINGDR3 the extension number of this Ks frame tinyint 1     meta.number
kseNum vikingMergeLog VIKINGDR4 the extension number of this Ks frame tinyint 1     meta.number;em.IR.K
kseNum vikingMergeLog VIKINGv20110714 the extension number of this Ks frame tinyint 1     meta.number
kseNum vikingMergeLog VIKINGv20111019 the extension number of this Ks frame tinyint 1     meta.number
kseNum vikingMergeLog VIKINGv20130417 the extension number of this Ks frame tinyint 1     meta.number
kseNum vikingMergeLog VIKINGv20140402 the extension number of this Ks frame tinyint 1     meta.number
kseNum vikingMergeLog VIKINGv20150421 the extension number of this Ks frame tinyint 1     meta.number;em.IR.K
kseNum vikingMergeLog VIKINGv20151230 the extension number of this Ks frame tinyint 1     meta.number;em.IR.K
kseNum vikingMergeLog VIKINGv20160406 the extension number of this Ks frame tinyint 1     meta.number;em.IR.K
kseNum vikingMergeLog VIKINGv20161202 the extension number of this Ks frame tinyint 1     meta.number;em.IR.K
kseNum vikingMergeLog VIKINGv20170715 the extension number of this Ks frame tinyint 1     meta.number;em.IR.K
kseNum vikingMergeLog VIKINGv20181012 the extension number of this Ks frame tinyint 1     meta.number;em.IR.K
kseNum vikingZY_selJ_RemeasMergeLog VIKINGZYSELJv20160909 the extension number of this Ks frame tinyint 1     meta.number
kseNum vikingZY_selJ_RemeasMergeLog VIKINGZYSELJv20170124 the extension number of this Ks frame tinyint 1     meta.number
kseNum vmcMergeLog VMCDR2 the extension number of this Ks frame tinyint 1     meta.number
kseNum vmcMergeLog VMCDR3 the extension number of this Ks frame tinyint 1     meta.number;em.IR.K
kseNum vmcMergeLog VMCDR4 the extension number of this Ks frame tinyint 1     meta.number;em.IR.K
kseNum vmcMergeLog VMCv20110816 the extension number of this Ks frame tinyint 1     meta.number
kseNum vmcMergeLog VMCv20110909 the extension number of this Ks frame tinyint 1     meta.number
kseNum vmcMergeLog VMCv20120126 the extension number of this Ks frame tinyint 1     meta.number
kseNum vmcMergeLog VMCv20121128 the extension number of this Ks frame tinyint 1     meta.number
kseNum vmcMergeLog VMCv20130304 the extension number of this Ks frame tinyint 1     meta.number
kseNum vmcMergeLog VMCv20130805 the extension number of this Ks frame tinyint 1     meta.number
kseNum vmcMergeLog VMCv20140428 the extension number of this Ks frame tinyint 1     meta.number;em.IR.K
kseNum vmcMergeLog VMCv20140903 the extension number of this Ks frame tinyint 1     meta.number;em.IR.K
kseNum vmcMergeLog VMCv20150309 the extension number of this Ks frame tinyint 1     meta.number;em.IR.K
kseNum vmcMergeLog VMCv20151218 the extension number of this Ks frame tinyint 1     meta.number;em.IR.K
kseNum vmcMergeLog VMCv20160311 the extension number of this Ks frame tinyint 1     meta.number;em.IR.K
kseNum vmcMergeLog VMCv20160822 the extension number of this Ks frame tinyint 1     meta.number;em.IR.K
kseNum vmcMergeLog VMCv20170109 the extension number of this Ks frame tinyint 1     meta.number;em.IR.K
kseNum vmcMergeLog VMCv20170411 the extension number of this Ks frame tinyint 1     meta.number;em.IR.K
kseNum vmcMergeLog VMCv20171101 the extension number of this Ks frame tinyint 1     meta.number;em.IR.K
kseNum vmcMergeLog VMCv20180702 the extension number of this Ks frame tinyint 1     meta.number;em.IR.K
kseNum vmcMergeLog VMCv20181120 the extension number of this Ks frame tinyint 1     meta.number;em.IR.K
kseNum vmcMergeLog, vmcSynopticMergeLog VMCDR1 the extension number of this Ks frame tinyint 1     meta.number
kseNum vvvMergeLog, vvvPsfDaophotJKsMergeLog, vvvSynopticMergeLog VVVDR4 the extension number of this Ks frame tinyint 1     meta.number;em.IR.K
ksErrBits vhsSource VHSDR1 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vhsSource VHSDR2 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vhsSource VHSDR3 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code;em.IR.K
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vhsSource VHSDR4 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code;em.IR.K
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vhsSource VHSv20120926 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vhsSource VHSv20130417 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vhsSource VHSv20140409 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code;em.IR.K
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vhsSource VHSv20150108 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code;em.IR.K
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vhsSource VHSv20160114 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code;em.IR.K
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vhsSource VHSv20160507 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code;em.IR.K
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vhsSource VHSv20170630 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code;em.IR.K
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vhsSource VHSv20171207 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code;em.IR.K
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vhsSource VHSv20180419 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code;em.IR.K
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vhsSourceRemeasurement VHSDR1 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code
ksErrBits videoSource VIDEODR2 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code
This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows:
Bit FlagMeaning
1The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected).
2The object was originally blended with another
4At least one pixel is saturated (or very close to)
8The object is truncated (too close to an image boundary)
16Object's aperture data are incomplete or corrupted
32Object'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.
64Memory overflow occurred during deblending
128Memory overflow occurred during extraction

ksErrBits videoSource VIDEODR3 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code
This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows:
Bit FlagMeaning
1The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected).
2The object was originally blended with another
4At least one pixel is saturated (or very close to)
8The object is truncated (too close to an image boundary)
16Object's aperture data are incomplete or corrupted
32Object'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.
64Memory overflow occurred during deblending
128Memory overflow occurred during extraction

ksErrBits videoSource VIDEODR4 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code;em.IR.K
This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows:
Bit FlagMeaning
1The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected).
2The object was originally blended with another
4At least one pixel is saturated (or very close to)
8The object is truncated (too close to an image boundary)
16Object's aperture data are incomplete or corrupted
32Object'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.
64Memory overflow occurred during deblending
128Memory overflow occurred during extraction

ksErrBits videoSource VIDEODR5 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code;em.IR.K
This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows:
Bit FlagMeaning
1The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected).
2The object was originally blended with another
4At least one pixel is saturated (or very close to)
8The object is truncated (too close to an image boundary)
16Object's aperture data are incomplete or corrupted
32Object'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.
64Memory overflow occurred during deblending
128Memory overflow occurred during extraction

ksErrBits videoSource VIDEOv20100513 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code
This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows:
Bit FlagMeaning
1The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected).
2The object was originally blended with another
4At least one pixel is saturated (or very close to)
8The object is truncated (too close to an image boundary)
16Object's aperture data are incomplete or corrupted
32Object'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.
64Memory overflow occurred during deblending
128Memory overflow occurred during extraction

ksErrBits videoSource VIDEOv20111208 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code
This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows:
Bit FlagMeaning
1The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected).
2The object was originally blended with another
4At least one pixel is saturated (or very close to)
8The object is truncated (too close to an image boundary)
16Object's aperture data are incomplete or corrupted
32Object'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.
64Memory overflow occurred during deblending
128Memory overflow occurred during extraction

ksErrBits videoSourceRemeasurement VIDEOv20100513 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code
ksErrBits vikingSource VIKINGDR2 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vikingSource VIKINGDR3 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vikingSource VIKINGDR4 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code;em.IR.K
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vikingSource VIKINGv20110714 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vikingSource VIKINGv20111019 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vikingSource VIKINGv20130417 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vikingSource VIKINGv20140402 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vikingSource VIKINGv20150421 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code;em.IR.K
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vikingSource VIKINGv20151230 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code;em.IR.K
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vikingSource VIKINGv20160406 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code;em.IR.K
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vikingSource VIKINGv20161202 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code;em.IR.K
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vikingSource VIKINGv20170715 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code;em.IR.K
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vikingSource VIKINGv20181012 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code;em.IR.K
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vikingSourceRemeasurement VIKINGv20110714 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code
ksErrBits vikingSourceRemeasurement VIKINGv20111019 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code
ksErrBits vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vmcSource VMCDR2 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vmcSource VMCDR3 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code;em.IR.K
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vmcSource VMCDR4 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code;em.IR.K
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vmcSource VMCv20110816 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vmcSource VMCv20110909 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vmcSource VMCv20120126 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vmcSource VMCv20121128 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vmcSource VMCv20130304 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vmcSource VMCv20130805 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vmcSource VMCv20140428 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code;em.IR.K
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vmcSource VMCv20140903 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code;em.IR.K
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vmcSource VMCv20150309 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code;em.IR.K
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vmcSource VMCv20151218 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code;em.IR.K
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vmcSource VMCv20160311 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code;em.IR.K
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vmcSource VMCv20160822 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code;em.IR.K
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vmcSource VMCv20170109 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code;em.IR.K
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vmcSource VMCv20170411 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code;em.IR.K
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vmcSource VMCv20171101 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code;em.IR.K
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vmcSource VMCv20180702 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code;em.IR.K
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vmcSource VMCv20181120 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code;em.IR.K
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vmcSource, vmcSynopticSource VMCDR1 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits vmcSourceRemeasurement VMCv20110816 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code
ksErrBits vmcSourceRemeasurement VMCv20110909 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code
ksErrBits vvvSource, vvvSynopticSource VVVDR4 processing warning/error bitwise flags in Ks int 4   -99999999 meta.code;em.IR.K
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksEta vhsSource VHSDR1 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vhsSource VHSDR2 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vhsSource VHSDR3 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.K
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vhsSource VHSDR4 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.K
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vhsSource VHSv20120926 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vhsSource VHSv20130417 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vhsSource VHSv20140409 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.K
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vhsSource VHSv20150108 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.K
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vhsSource VHSv20160114 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.K
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vhsSource VHSv20160507 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.K
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vhsSource VHSv20170630 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.K
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vhsSource VHSv20171207 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.K
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vhsSource VHSv20180419 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.K
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta videoSource VIDEODR2 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta videoSource VIDEODR3 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta videoSource VIDEODR4 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.K
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta videoSource VIDEODR5 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.K
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta videoSource VIDEOv20100513 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta videoSource VIDEOv20111208 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vikingSource VIKINGDR2 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vikingSource VIKINGDR3 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vikingSource VIKINGDR4 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.K
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vikingSource VIKINGv20110714 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vikingSource VIKINGv20111019 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vikingSource VIKINGv20130417 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vikingSource VIKINGv20140402 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vikingSource VIKINGv20150421 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.K
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vikingSource VIKINGv20151230 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.K
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vikingSource VIKINGv20160406 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.K
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vikingSource VIKINGv20161202 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.K
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vikingSource VIKINGv20170715 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.K
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vikingSource VIKINGv20181012 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.K
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vmcSource VMCDR2 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vmcSource VMCDR3 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.K
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vmcSource VMCDR4 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.K
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vmcSource VMCv20110816 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vmcSource VMCv20110909 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vmcSource VMCv20120126 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vmcSource VMCv20121128 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vmcSource VMCv20130304 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vmcSource VMCv20130805 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vmcSource VMCv20140428 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.K
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vmcSource VMCv20140903 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.K
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vmcSource VMCv20150309 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.K
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vmcSource VMCv20151218 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.K
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vmcSource VMCv20160311 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.K
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vmcSource VMCv20160822 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.K
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vmcSource VMCv20170109 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.K
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vmcSource VMCv20170411 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.K
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vmcSource VMCv20171101 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.K
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vmcSource VMCv20180702 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.K
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vmcSource VMCv20181120 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.K
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vmcSource, vmcSynopticSource VMCDR1 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksEta vvvSource, vvvSynopticSource VVVDR4 Offset of Ks detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.K
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.
ksexpML videoVarFrameSetInfo VIDEODR2 Expected magnitude limit of frameSet in this in Ks band. real 4   -0.9999995e9  
ksexpML videoVarFrameSetInfo VIDEODR3 Expected magnitude limit of frameSet in this in Ks band. real 4   -0.9999995e9 phot.mag;stat.max;em.IR.NIR
ksexpML videoVarFrameSetInfo VIDEODR4 Expected magnitude limit of frameSet in this in Ks band. real 4 mag -0.9999995e9 phot.mag;em.IR.K;stat.max
ksexpML videoVarFrameSetInfo VIDEODR5 Expected magnitude limit of frameSet in this in Ks band. real 4 mag -0.9999995e9 phot.mag;em.IR.K;stat.max
ksexpML videoVarFrameSetInfo VIDEOv20100513 Expected magnitude limit of frameSet in this in Ks band. real 4   -0.9999995e9  
ksexpML videoVarFrameSetInfo VIDEOv20111208 Expected magnitude limit of frameSet in this in Ks band. real 4   -0.9999995e9  
ksexpML vikingVarFrameSetInfo VIKINGDR2 Expected magnitude limit of frameSet in this in Ks band. real 4   -0.9999995e9  
ksexpML vikingVarFrameSetInfo VIKINGv20110714 Expected magnitude limit of frameSet in this in Ks band. real 4   -0.9999995e9  
ksexpML vikingVarFrameSetInfo VIKINGv20111019 Expected magnitude limit of frameSet in this in Ks band. real 4   -0.9999995e9  
ksexpML vmcVarFrameSetInfo VMCDR1 Expected magnitude limit of frameSet in this in Ks band. real 4   -0.9999995e9  
ksexpML vmcVarFrameSetInfo VMCDR2 Expected magnitude limit of frameSet in this in Ks band. real 4 mag -0.9999995e9 phot.mag;em.IR.K;stat.max;em.IR.NIR
ksexpML vmcVarFrameSetInfo VMCDR3 Expected magnitude limit of frameSet in this in Ks band. real 4 mag -0.9999995e9 phot.mag;em.IR.K;stat.max
ksexpML vmcVarFrameSetInfo VMCDR4 Expected magnitude limit of frameSet in this in Ks band. real 4 mag -0.9999995e9 phot.mag;em.IR.K;stat.max
ksexpML vmcVarFrameSetInfo VMCv20110816 Expected magnitude limit of frameSet in this in Ks band. real 4   -0.9999995e9  
ksexpML vmcVarFrameSetInfo VMCv20110909 Expected magnitude limit of frameSet in this in Ks band. real 4   -0.9999995e9  
ksexpML vmcVarFrameSetInfo VMCv20120126 Expected magnitude limit of frameSet in this in Ks band. real 4   -0.9999995e9  
ksexpML vmcVarFrameSetInfo VMCv20121128 Expected magnitude limit of frameSet in this in Ks band. real 4 mag -0.9999995e9 phot.mag;stat.max;em.IR.NIR
ksexpML vmcVarFrameSetInfo VMCv20130304 Expected magnitude limit of frameSet in this in Ks band. real 4 mag -0.9999995e9 phot.mag;stat.max;em.IR.NIR
ksexpML vmcVarFrameSetInfo VMCv20130805 Expected magnitude limit of frameSet in this in Ks band. real 4 mag -0.9999995e9 phot.mag;em.IR.K;stat.max;em.IR.NIR
ksexpML vmcVarFrameSetInfo VMCv20140428 Expected magnitude limit of frameSet in this in Ks band. real 4 mag -0.9999995e9 phot.mag;em.IR.K;stat.max
ksexpML vmcVarFrameSetInfo VMCv20140903 Expected magnitude limit of frameSet in this in Ks band. real 4 mag -0.9999995e9 phot.mag;em.IR.K;stat.max
ksexpML vmcVarFrameSetInfo VMCv20150309 Expected magnitude limit of frameSet in this in Ks band. real 4 mag -0.9999995e9 phot.mag;em.IR.K;stat.max
ksexpML vmcVarFrameSetInfo VMCv20151218 Expected magnitude limit of frameSet in this in Ks band. real 4 mag -0.9999995e9 phot.mag;em.IR.K;stat.max
ksexpML vmcVarFrameSetInfo VMCv20160311 Expected magnitude limit of frameSet in this in Ks band. real 4 mag -0.9999995e9 phot.mag;em.IR.K;stat.max
ksexpML vmcVarFrameSetInfo VMCv20160822 Expected magnitude limit of frameSet in this in Ks band. real 4 mag -0.9999995e9 phot.mag;em.IR.K;stat.max
ksexpML vmcVarFrameSetInfo VMCv20170109 Expected magnitude limit of frameSet in this in Ks band. real 4 mag -0.9999995e9 phot.mag;em.IR.K;stat.max
ksexpML vmcVarFrameSetInfo VMCv20170411 Expected magnitude limit of frameSet in this in Ks band. real 4 mag -0.9999995e9 phot.mag;em.IR.K;stat.max
ksexpML vmcVarFrameSetInfo VMCv20171101 Expected magnitude limit of frameSet in this in Ks band. real 4 mag -0.9999995e9 phot.mag;em.IR.K;stat.max
ksexpML vmcVarFrameSetInfo VMCv20180702 Expected magnitude limit of frameSet in this in Ks band. real 4 mag -0.9999995e9 phot.mag;em.IR.K;stat.max
ksexpML vmcVarFrameSetInfo VMCv20181120 Expected magnitude limit of frameSet in this in Ks band. real 4 mag -0.9999995e9 phot.mag;em.IR.K;stat.max
ksexpML vvvVarFrameSetInfo VVVDR4 Expected magnitude limit of frameSet in this in Ks band. real 4 mag -0.9999995e9 phot.mag;em.IR.K;stat.max
ksExpRms videoVariability VIDEODR2 Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks 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.
ksExpRms videoVariability VIDEODR3 Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks band real 4 mag -0.9999995e9 stat.error;em.IR.NIR
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.
ksExpRms videoVariability VIDEODR4 Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks band real 4 mag -0.9999995e9 stat.error;em.IR.K
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.
ksExpRms videoVariability VIDEODR5 Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks band real 4 mag -0.9999995e9 stat.error;em.IR.K
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.
ksExpRms videoVariability VIDEOv20100513 Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks 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.
ksExpRms videoVariability VIDEOv20111208 Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks 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.
ksExpRms vikingVariability VIKINGDR2 Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks 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.
ksExpRms vikingVariability VIKINGv20110714 Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks 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.
ksExpRms vikingVariability VIKINGv20111019 Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks 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.
ksExpRms vmcVariability VMCDR1 Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks 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.
ksExpRms vmcVariability VMCDR2 Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks band real 4 mag -0.9999995e9 stat.error;em.IR.NIR
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.
ksExpRms vmcVariability VMCDR3 Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks band real 4 mag -0.9999995e9 stat.error;em.IR.K
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.
ksExpRms vmcVariability VMCDR4 Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks band real 4 mag -0.9999995e9 stat.error;em.IR.K
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.
ksExpRms vmcVariability VMCv20110816 Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks 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.
ksExpRms vmcVariability VMCv20110909 Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks 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.
ksExpRms vmcVariability VMCv20120126 Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks 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.
ksExpRms vmcVariability VMCv20121128 Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks band real 4 mag -0.9999995e9 stat.error;em.IR.NIR
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.
ksExpRms vmcVariability VMCv20130304 Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks band real 4 mag -0.9999995e9 stat.error;em.IR.NIR
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.
ksExpRms vmcVariability VMCv20130805 Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks band real 4 mag -0.9999995e9 stat.error;em.IR.NIR
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.
ksExpRms vmcVariability VMCv20140428 Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks band real 4 mag -0.9999995e9 stat.error;em.IR.K
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.
ksExpRms vmcVariability VMCv20140903 Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks band real 4 mag -0.9999995e9 stat.error;em.IR.K
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.
ksExpRms vmcVariability VMCv20150309 Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks band real 4 mag -0.9999995e9 stat.error;em.IR.K
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.
ksExpRms vmcVariability VMCv20151218 Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks band real 4 mag -0.9999995e9 stat.error;em.IR.K
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.
ksExpRms vmcVariability VMCv20160311 Rms calculated from polynomial fit to modal RMS as a function of magnitude in Ks band real 4 mag -0.9999995e9 stat.error;em.IR.K
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.
ksExpRms