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Glossary of VSA attributes
This Glossary alphabetically lists all attributes used in the VSAv20110218 database(s) held in the VSA. If you would like to have more information about the schema tables please use the VSAv20110218 Schema Browser (other Browser versions).

A

B

C

D

E

F

G

H

I

J

K

L

M

N

O

P

Q

R

S

T

U

V

W

X

Y

Z

K
Name	Schema Table	Database	Description	Type	Length	Unit	Default Value	Unified Content Descriptor
K	twomass	SIXDF	K magnitude (corrected) used for K selection	real	4	mag
k_2mrat	twomass_scn	2MASS	Ks-band average 2nd image moment ratio.	real	4			FIT_PARAM_VALUE
k_2mrat	twomass_sixx2_scn	2MASS	K band average 2nd image moment ratio for scan	real	4
k_5sig_ba	twomass_xsc	2MASS	K minor/major axis ratio fit to the 5-sigma isophote.	real	4			PHYS_AXIS-RATIO
k_5sig_phi	twomass_xsc	2MASS	K angle to 5-sigma major axis (E of N).	smallint	2	degrees		ERROR
k_5surf	twomass_xsc	2MASS	K central surface brightness (r<=5).	real	4	mag		PHOT_SB_GENERAL
k_ba	twomass_sixx2_xsc	2MASS	K minor/major axis ratio fit to the 3-sigma isophote	real	4
k_ba	twomass_xsc	2MASS	K minor/major axis ratio fit to the 3-sigma isophote.	real	4			PHYS_AXIS-RATIO
k_back	twomass_xsc	2MASS	K coadd median background.	real	4			CODE_MISC
k_bisym_chi	twomass_xsc	2MASS	K bi-symmetric cross-correlation chi.	real	4			FIT_PARAM_VALUE
k_bisym_rat	twomass_xsc	2MASS	K bi-symmetric flux ratio.	real	4			PHOT_FLUX_RATIO
k_bndg_amp	twomass_xsc	2MASS	K banding maximum FT amplitude on this side of coadd.	real	4	DN		FIT_PARAM_VALUE
k_bndg_per	twomass_xsc	2MASS	K banding Fourier Transf. period on this side of coadd.	int	4	arcsec		FIT_PARAM_VALUE
k_chif_ellf	twomass_xsc	2MASS	K % chi-fraction for elliptical fit to 3-sig isophote.	real	4			FIT_PARAM_VALUE
k_cmsig	twomass_psc	2MASS	Corrected photometric uncertainty for the default Ks-band magnitude.	real	4	mag		SPECT_FLUX_VALUE
k_con_indx	twomass_xsc	2MASS	K concentration index r_75%/r_25%.	real	4			PHYS_CONCENT_INDEX
k_d_area	twomass_xsc	2MASS	K 5-sigma to 3-sigma differential area.	smallint	2			FIT_RESIDUAL
k_flg_10	twomass_xsc	2MASS	K confusion flag for 10 arcsec circular ap. mag.	smallint	2			CODE_MISC
k_flg_15	twomass_xsc	2MASS	K confusion flag for 15 arcsec circular ap. mag.	smallint	2			CODE_MISC
k_flg_20	twomass_xsc	2MASS	K confusion flag for 20 arcsec circular ap. mag.	smallint	2			CODE_MISC
k_flg_25	twomass_xsc	2MASS	K confusion flag for 25 arcsec circular ap. mag.	smallint	2			CODE_MISC
k_flg_30	twomass_xsc	2MASS	K confusion flag for 30 arcsec circular ap. mag.	smallint	2			CODE_MISC
k_flg_40	twomass_xsc	2MASS	K confusion flag for 40 arcsec circular ap. mag.	smallint	2			CODE_MISC
k_flg_5	twomass_xsc	2MASS	K confusion flag for 5 arcsec circular ap. mag.	smallint	2			CODE_MISC
k_flg_50	twomass_xsc	2MASS	K confusion flag for 50 arcsec circular ap. mag.	smallint	2			CODE_MISC
k_flg_60	twomass_xsc	2MASS	K confusion flag for 60 arcsec circular ap. mag.	smallint	2			CODE_MISC
k_flg_7	twomass_sixx2_xsc	2MASS	K confusion flag for 7 arcsec circular ap. mag	smallint	2
k_flg_7	twomass_xsc	2MASS	K confusion flag for 7 arcsec circular ap. mag.	smallint	2			CODE_MISC
k_flg_70	twomass_xsc	2MASS	K confusion flag for 70 arcsec circular ap. mag.	smallint	2			CODE_MISC
k_flg_c	twomass_xsc	2MASS	K confusion flag for Kron circular mag.	smallint	2			CODE_MISC
k_flg_e	twomass_xsc	2MASS	K confusion flag for Kron elliptical mag.	smallint	2			CODE_MISC
k_flg_fc	twomass_xsc	2MASS	K confusion flag for fiducial Kron circ. mag.	smallint	2			CODE_MISC
k_flg_fe	twomass_xsc	2MASS	K confusion flag for fiducial Kron ell. mag.	smallint	2			CODE_MISC
k_flg_i20c	twomass_xsc	2MASS	K confusion flag for 20mag/sq." iso. circ. mag.	smallint	2			CODE_MISC
k_flg_i20e	twomass_xsc	2MASS	K confusion flag for 20mag/sq." iso. ell. mag.	smallint	2			CODE_MISC
k_flg_i21c	twomass_xsc	2MASS	K confusion flag for 21mag/sq." iso. circ. mag.	smallint	2			CODE_MISC
k_flg_i21e	twomass_xsc	2MASS	K confusion flag for 21mag/sq." iso. ell. mag.	smallint	2			CODE_MISC
k_flg_j21fc	twomass_xsc	2MASS	K confusion flag for 21mag/sq." iso. fid. circ. mag.	smallint	2			CODE_MISC
k_flg_j21fe	twomass_xsc	2MASS	K confusion flag for 21mag/sq." iso. fid. ell. mag.	smallint	2			CODE_MISC
k_flg_k20fc	twomass_xsc	2MASS	K confusion flag for 20mag/sq." iso. fid. circ. mag.	smallint	2			CODE_MISC
k_flg_k20fe	twomass_sixx2_xsc	2MASS	K confusion flag for 20mag/sq.″ iso. fid. ell. mag	smallint	2
k_flg_k20fe	twomass_xsc	2MASS	K confusion flag for 20mag/sq." iso. fid. ell. mag.	smallint	2			CODE_MISC
k_m	twomass_psc	2MASS	Default Ks-band magnitude	real	4	mag		SPECT_FLUX_VALUE
k_m	twomass_sixx2_psc	2MASS	K selected "default" magnitude	real	4	mag
k_m_10	twomass_xsc	2MASS	K 10 arcsec radius circular aperture magnitude.	real	4	mag		SPECT_FLUX_VALUE
k_m_15	twomass_xsc	2MASS	K 15 arcsec radius circular aperture magnitude.	real	4	mag		SPECT_FLUX_VALUE
k_m_20	twomass_xsc	2MASS	K 20 arcsec radius circular aperture magnitude.	real	4	mag		SPECT_FLUX_VALUE
k_m_25	twomass_xsc	2MASS	K 25 arcsec radius circular aperture magnitude.	real	4	mag		SPECT_FLUX_VALUE
k_m_30	twomass_xsc	2MASS	K 30 arcsec radius circular aperture magnitude.	real	4	mag		SPECT_FLUX_VALUE
k_m_40	twomass_xsc	2MASS	K 40 arcsec radius circular aperture magnitude.	real	4	mag		SPECT_FLUX_VALUE
k_m_5	twomass_xsc	2MASS	K 5 arcsec radius circular aperture magnitude.	real	4	mag		SPECT_FLUX_VALUE
k_m_50	twomass_xsc	2MASS	K 50 arcsec radius circular aperture magnitude.	real	4	mag		SPECT_FLUX_VALUE
k_m_60	twomass_xsc	2MASS	K 60 arcsec radius circular aperture magnitude.	real	4	mag		SPECT_FLUX_VALUE
k_m_7	twomass_sixx2_xsc	2MASS	K 7 arcsec radius circular aperture magnitude	real	4	mag
k_m_7	twomass_xsc	2MASS	K 7 arcsec radius circular aperture magnitude.	real	4	mag		SPECT_FLUX_VALUE
k_m_70	twomass_xsc	2MASS	K 70 arcsec radius circular aperture magnitude.	real	4	mag		SPECT_FLUX_VALUE
k_m_c	twomass_xsc	2MASS	K Kron circular aperture magnitude.	real	4	mag		SPECT_FLUX_VALUE
k_m_e	twomass_xsc	2MASS	K Kron elliptical aperture magnitude.	real	4	mag		SPECT_FLUX_VALUE
k_m_ext	twomass_sixx2_xsc	2MASS	K mag from fit extrapolation	real	4	mag
k_m_ext	twomass_xsc	2MASS	K mag from fit extrapolation.	real	4	mag		SPECT_FLUX_VALUE
k_m_fc	twomass_xsc	2MASS	K fiducial Kron circular magnitude.	real	4	mag		SPECT_FLUX_VALUE
k_m_fe	twomass_xsc	2MASS	K fiducial Kron ell. mag aperture magnitude.	real	4	mag		SPECT_FLUX_VALUE
k_m_i20c	twomass_xsc	2MASS	K 20mag/sq." isophotal circular ap. magnitude.	real	4	mag		SPECT_FLUX_VALUE
k_m_i20e	twomass_xsc	2MASS	K 20mag/sq." isophotal elliptical ap. magnitude.	real	4	mag		SPECT_FLUX_VALUE
k_m_i21c	twomass_xsc	2MASS	K 21mag/sq." isophotal circular ap. magnitude.	real	4	mag		SPECT_FLUX_VALUE
k_m_i21e	twomass_xsc	2MASS	K 21mag/sq." isophotal elliptical ap. magnitude.	real	4	mag		SPECT_FLUX_VALUE
k_m_j21fc	twomass_xsc	2MASS	K 21mag/sq." isophotal fiducial circ. ap. mag.	real	4	mag		SPECT_FLUX_VALUE
k_m_j21fe	twomass_xsc	2MASS	K 21mag/sq." isophotal fiducial ell. ap. magnitude.	real	4	mag		SPECT_FLUX_VALUE
k_m_k20fc	twomass_xsc	2MASS	K 20mag/sq." isophotal fiducial circ. ap. mag.	real	4	mag		SPECT_FLUX_VALUE
K_M_K20FE	twomass	SIXDF	K 20mag/sq." isophotal fiducial ell. ap. magnitude	real	4	mag
k_m_k20fe	twomass_sixx2_xsc	2MASS	K 20mag/sq.″ isophotal fiducial ell. ap. magnitude	real	4	mag
k_m_k20fe	twomass_xsc	2MASS	K 20mag/sq." isophotal fiducial ell. ap. magnitude.	real	4	mag		SPECT_FLUX_VALUE
k_m_stdap	twomass_psc	2MASS	Ks-band "standard" aperture magnitude.	real	4	mag		SPECT_FLUX_VALUE
k_m_sys	twomass_xsc	2MASS	K system photometry magnitude.	real	4	mag		SPECT_FLUX_VALUE
k_mnsurfb_eff	twomass_xsc	2MASS	K mean surface brightness at the half-light radius.	real	4	mag		PHOT_SB_GENERAL
k_msig	twomass_sixx2_psc	2MASS	K "default" mag uncertainty	real	4	mag
k_msig_10	twomass_xsc	2MASS	K 1-sigma uncertainty in 10 arcsec circular ap. mag.	real	4	mag		ERROR
k_msig_15	twomass_xsc	2MASS	K 1-sigma uncertainty in 15 arcsec circular ap. mag.	real	4	mag		ERROR
k_msig_20	twomass_xsc	2MASS	K 1-sigma uncertainty in 20 arcsec circular ap. mag.	real	4	mag		ERROR
k_msig_25	twomass_xsc	2MASS	K 1-sigma uncertainty in 25 arcsec circular ap. mag.	real	4	mag		ERROR
k_msig_30	twomass_xsc	2MASS	K 1-sigma uncertainty in 30 arcsec circular ap. mag.	real	4	mag		ERROR
k_msig_40	twomass_xsc	2MASS	K 1-sigma uncertainty in 40 arcsec circular ap. mag.	real	4	mag		ERROR
k_msig_5	twomass_xsc	2MASS	K 1-sigma uncertainty in 5 arcsec circular ap. mag.	real	4	mag		ERROR
k_msig_50	twomass_xsc	2MASS	K 1-sigma uncertainty in 50 arcsec circular ap. mag.	real	4	mag		ERROR
k_msig_60	twomass_xsc	2MASS	K 1-sigma uncertainty in 60 arcsec circular ap. mag.	real	4	mag		ERROR
k_msig_7	twomass_sixx2_xsc	2MASS	K 1-sigma uncertainty in 7 arcsec circular ap. mag	real	4	mag
k_msig_7	twomass_xsc	2MASS	K 1-sigma uncertainty in 7 arcsec circular ap. mag.	real	4	mag		ERROR
k_msig_70	twomass_xsc	2MASS	K 1-sigma uncertainty in 70 arcsec circular ap. mag.	real	4	mag		ERROR
k_msig_c	twomass_xsc	2MASS	K 1-sigma uncertainty in Kron circular mag.	real	4	mag		ERROR
k_msig_e	twomass_xsc	2MASS	K 1-sigma uncertainty in Kron elliptical mag.	real	4	mag		ERROR
k_msig_ext	twomass_sixx2_xsc	2MASS	K 1-sigma uncertainty in mag from fit extrapolation	real	4	mag
k_msig_ext	twomass_xsc	2MASS	K 1-sigma uncertainty in mag from fit extrapolation.	real	4	mag		ERROR
k_msig_fc	twomass_xsc	2MASS	K 1-sigma uncertainty in fiducial Kron circ. mag.	real	4	mag		ERROR
k_msig_fe	twomass_xsc	2MASS	K 1-sigma uncertainty in fiducial Kron ell. mag.	real	4	mag		ERROR
k_msig_i20c	twomass_xsc	2MASS	K 1-sigma uncertainty in 20mag/sq." iso. circ. mag.	real	4	mag		ERROR
k_msig_i20e	twomass_xsc	2MASS	K 1-sigma uncertainty in 20mag/sq." iso. ell. mag.	real	4	mag		ERROR
k_msig_i21c	twomass_xsc	2MASS	K 1-sigma uncertainty in 21mag/sq." iso. circ. mag.	real	4	mag		ERROR
k_msig_i21e	twomass_xsc	2MASS	K 1-sigma uncertainty in 21mag/sq." iso. ell. mag.	real	4	mag		ERROR
k_msig_j21fc	twomass_xsc	2MASS	K 1-sigma uncertainty in 21mag/sq." iso.fid.circ.mag.	real	4	mag		ERROR
k_msig_j21fe	twomass_xsc	2MASS	K 1-sigma uncertainty in 21mag/sq." iso.fid.ell.mag.	real	4	mag		ERROR
k_msig_k20fc	twomass_xsc	2MASS	K 1-sigma uncertainty in 20mag/sq." iso.fid.circ. mag.	real	4	mag		ERROR
k_msig_k20fe	twomass_sixx2_xsc	2MASS	K 1-sigma uncertainty in 20mag/sq.″ iso.fid.ell.mag	real	4	mag
k_msig_k20fe	twomass_xsc	2MASS	K 1-sigma uncertainty in 20mag/sq." iso.fid.ell.mag.	real	4	mag		ERROR
k_msig_stdap	twomass_psc	2MASS	Uncertainty in the Ks-band standard aperture magnitude.	real	4	mag		SPECT_FLUX_VALUE
k_msig_sys	twomass_xsc	2MASS	K 1-sigma uncertainty in system photometry mag.	real	4	mag		ERROR
k_msigcom	twomass_psc	2MASS	Combined, or total photometric uncertainty for the default Ks-band magnitude.	real	4	mag		SPECT_FLUX_VALUE
k_msigcom	twomass_sixx2_psc	2MASS	combined (total) K band photometric uncertainty	real	4	mag
k_msnr10	twomass_scn	2MASS	The estimated Ks-band magnitude at which SNR=10 is achieved for this scan.	real	4	mag		SPECT_FLUX_VALUE
k_msnr10	twomass_sixx2_scn	2MASS	K mag at which SNR=10 is achieved, from k_psp and k_zp_ap	real	4	mag
k_n_snr10	twomass_scn	2MASS	Number of point sources at Ks-band with SNR>10 (instrumental mag <=14.3)	int	4			NUMBER
k_n_snr10	twomass_sixx2_scn	2MASS	number of K point sources with SNR>10 (instrumental m<=14.3)	int	4
k_pchi	twomass_xsc	2MASS	K chi^2 of fit to rad. profile (LCSB: alpha scale len).	real	4			FIT_PARAM_VALUE
k_peak	twomass_xsc	2MASS	K peak pixel brightness.	real	4	mag		PHOT_SB_GENERAL
k_perc_darea	twomass_xsc	2MASS	K 5-sigma to 3-sigma percent area change.	smallint	2			FIT_PARAM
k_phi	twomass_sixx2_xsc	2MASS	K angle to 3-sigma major axis (E of N)	smallint	2	deg
k_phi	twomass_xsc	2MASS	K angle to 3-sigma major axis (E of N).	smallint	2	degrees		POS_POS-ANG
k_psfchi	twomass_psc	2MASS	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			FIT_PARAM_VALUE
k_psp	twomass_scn	2MASS	Ks-band photometric sensitivity paramater (PSP).	real	4			INST_SENSITIVITY
k_psp	twomass_sixx2_scn	2MASS	K photometric sensitivity param: k_shape_avg*(k_fbg_avg^.29)	real	4
k_pts_noise	twomass_scn	2MASS	Base-10 logarithm of the mode of the noise distribution for all point source detections in the scan, where the noise is estimated from the measured Ks-band photometric errors and is expressed in units of mJy.	real	4			INST_NOISE
k_pts_noise	twomass_sixx2_scn	2MASS	log10 of K band modal point src noise estimate	real	4	logmJy
k_r_c	twomass_xsc	2MASS	K Kron circular aperture radius.	real	4	arcsec		EXTENSION_RAD
k_r_e	twomass_xsc	2MASS	K Kron elliptical aperture semi-major axis.	real	4	arcsec		EXTENSION_RAD
k_r_eff	twomass_xsc	2MASS	K half-light (integrated half-flux point) radius.	real	4	arcsec		EXTENSION_RAD
k_r_i20c	twomass_xsc	2MASS	K 20mag/sq." isophotal circular aperture radius.	real	4	arcsec		EXTENSION_RAD
k_r_i20e	twomass_xsc	2MASS	K 20mag/sq." isophotal elliptical ap. semi-major axis.	real	4	arcsec		EXTENSION_RAD
k_r_i21c	twomass_xsc	2MASS	K 21mag/sq." isophotal circular aperture radius.	real	4	arcsec		EXTENSION_RAD
k_r_i21e	twomass_xsc	2MASS	K 21mag/sq." isophotal elliptical ap. semi-major axis.	real	4	arcsec		EXTENSION_RAD
k_resid_ann	twomass_xsc	2MASS	K residual annulus background median.	real	4	DN		CODE_MISC
k_sc_1mm	twomass_xsc	2MASS	K 1st moment (score) (LCSB: super blk 2,4,8 SNR).	real	4			CODE_MISC
k_sc_2mm	twomass_xsc	2MASS	K 2nd moment (score) (LCSB: SNRMAX - super SNR max).	real	4			CODE_MISC
k_sc_msh	twomass_xsc	2MASS	K median shape score.	real	4			CODE_MISC
k_sc_mxdn	twomass_xsc	2MASS	K mxdn (score) (LCSB: BSNR - block/smoothed SNR).	real	4			CODE_MISC
k_sc_r1	twomass_xsc	2MASS	K r1 (score).	real	4			CODE_MISC
k_sc_r23	twomass_xsc	2MASS	K r23 (score) (LCSB: TSNR - integrated SNR for r=15).	real	4			CODE_MISC
k_sc_sh	twomass_xsc	2MASS	K shape (score).	real	4			CODE_MISC
k_sc_vint	twomass_xsc	2MASS	K vint (score).	real	4			CODE_MISC
k_sc_wsh	twomass_xsc	2MASS	K wsh (score) (LCSB: PSNR - peak raw SNR).	real	4			CODE_MISC
k_seetrack	twomass_xsc	2MASS	K band seetracking score.	real	4			CODE_MISC
k_sh0	twomass_xsc	2MASS	K ridge shape (LCSB: BSNR limit).	real	4			FIT_PARAM
k_shape_avg	twomass_scn	2MASS	Ks-band average seeing shape for scan.	real	4			INST_SEEING
k_shape_avg	twomass_sixx2_scn	2MASS	K band average seeing shape for scan	real	4
k_shape_rms	twomass_scn	2MASS	RMS-error of Ks-band average seeing shape.	real	4			INST_SEEING
k_shape_rms	twomass_sixx2_scn	2MASS	rms of K band avg seeing shape for scan	real	4
k_sig_sh0	twomass_xsc	2MASS	K ridge shape sigma (LCSB: B2SNR limit).	real	4			FIT_PARAM
k_snr	twomass_psc	2MASS	Ks-band "scan" signal-to-noise ratio.	real	4	mag		INST_NOISE
k_snr	twomass_sixx2_psc	2MASS	K band "scan" signal-to-noise ratio	real	4
k_subst2	twomass_xsc	2MASS	K residual background #2 (score).	real	4			CODE_MISC
k_zp_ap	twomass_scn	2MASS	Photometric zero-point for Ks-band aperture photometry.	real	4	mag		PHOT_ZP
k_zp_ap	twomass_sixx2_scn	2MASS	K band ap. calibration photometric zero-point for scan	real	4	mag
k_zperr_ap	twomass_scn	2MASS	RMS-error of zero-point for Ks-band aperture photometry	real	4	mag		FIT_ERROR
k_zperr_ap	twomass_sixx2_scn	2MASS	K band ap. calibration rms error of zero-point for scan	real	4	mag
KBESTR	spectra	SIXDF	cross-correlation template	int	4
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	VSASVNGC253	K band total magnitude on the MKO(UFTI) system	real	4	mag		PHOT_INT-MAG
kMag	ukirtFSstars	VSASVORION	K band total magnitude on the MKO(UFTI) system	real	4	mag		PHOT_INT-MAG
kMag	ukirtFSstars	VSAUltraVISTA	K band total magnitude on the MKO(UFTI) system	real	4	mag		PHOT_INT-MAG
kMag	ukirtFSstars	VSAVHS	K band total magnitude on the MKO(UFTI) system	real	4	mag		PHOT_INT-MAG
kMag	ukirtFSstars	VSAVIDEO	K band total magnitude on the MKO(UFTI) system	real	4	mag		PHOT_INT-MAG
kMag	ukirtFSstars	VSAVIKING	K band total magnitude on the MKO(UFTI) system	real	4	mag		PHOT_INT-MAG
kMag	ukirtFSstars	VSAVMC	K band total magnitude on the MKO(UFTI) system	real	4	mag		PHOT_INT-MAG
kMag	ukirtFSstars	VSAVVV	K band total magnitude on the MKO(UFTI) system	real	4	mag		PHOT_INT-MAG
Kmag2MASS	spitzer_smcSource	SPITZER	The 2MASS K band magnitude.	real	4	mag
kMagErr	ukirtFSstars	VSASVNGC253	K band magnitude error	real	4	mag		ERROR
kMagErr	ukirtFSstars	VSASVORION	K band magnitude error	real	4	mag		ERROR
kMagErr	ukirtFSstars	VSAUltraVISTA	K band magnitude error	real	4	mag		ERROR
kMagErr	ukirtFSstars	VSAVHS	K band magnitude error	real	4	mag		ERROR
kMagErr	ukirtFSstars	VSAVIDEO	K band magnitude error	real	4	mag		ERROR
kMagErr	ukirtFSstars	VSAVIKING	K band magnitude error	real	4	mag		ERROR
kMagErr	ukirtFSstars	VSAVMC	K band magnitude error	real	4	mag		ERROR
kMagErr	ukirtFSstars	VSAVVV	K band magnitude error	real	4	mag		ERROR
kronFlux	svNgc253Detection	VSASVNGC253	flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux}	real	4	ADU		PHOT_INTENSITY_ADU
kronFlux	svOrionDetection	VSASVORION	flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux}	real	4	ADU		PHOT_INTENSITY_ADU
kronFlux	ultravistaDetection	VSAUltraVISTA	flux within Kron radius circular aperture (SE: FLUX_AUTO) {catalogue TType keyword: Kron_flux}	real	4	ADU		PHOT_INTENSITY_ADU
kronFlux	ultravistaDetection, videoDetection	VSAQC	flux within Kron radius circular aperture (SE: FLUX_AUTO) {catalogue TType keyword: Kron_flux}	real	4	ADU		PHOT_INTENSITY_ADU
kronFlux	ultravistaListRemeasurement	VSAUltraVISTA	flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux}	real	4	ADU		PHOT_INTENSITY_ADU
kronFlux	ultravistaListRemeasurement, vhsDetection, vhsListRemeasurement, videoListRemeasurement, vikingDetection, vikingListRemeasurement, vmcDetection, vmcListRemeasurement, vvvDetection, vvvListRemeasurement	VSAQC	flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux}	real	4	ADU		PHOT_INTENSITY_ADU
kronFluxErr	svNgc253Detection	VSASVNGC253	error on Kron flux {catalogue TType keyword: Kron_flux_err}	real	4	ADU		ERROR
kronFluxErr	svOrionDetection	VSASVORION	error on Kron flux {catalogue TType keyword: Kron_flux_err}	real	4	ADU		ERROR
kronFluxErr	ultravistaDetection	VSAUltraVISTA	error on Kron flux (SE: FLUXERR_AUTO) {catalogue TType keyword: Kron_flux_err}	real	4	ADU		ERROR
kronFluxErr	ultravistaDetection, videoDetection	VSAQC	error on Kron flux (SE: FLUXERR_AUTO) {catalogue TType keyword: Kron_flux_err}	real	4	ADU		ERROR
kronFluxErr	ultravistaListRemeasurement	VSAUltraVISTA	error on Kron flux {catalogue TType keyword: Kron_flux_err}	real	4	ADU		ERROR
kronFluxErr	ultravistaListRemeasurement, vhsDetection, vhsListRemeasurement, videoListRemeasurement, vikingDetection, vikingListRemeasurement, vmcDetection, vmcListRemeasurement, vvvDetection, vvvListRemeasurement	VSAQC	error on Kron flux {catalogue TType keyword: Kron_flux_err}	real	4	ADU		ERROR
kronMag	svNgc253Detection	VSASVNGC253	Calibrated Kron magnitude within circular aperture r_k	real	4	mag		PHOT_INT-MAG
kronMag	svOrionDetection	VSASVORION	Calibrated Kron magnitude within circular aperture r_k	real	4	mag		PHOT_INT-MAG
kronMag	ultravistaDetection	VSAUltraVISTA	Calibrated Kron magnitude within circular aperture r_k	real	4	mag		PHOT_INT-MAG
kronMag	ultravistaDetection, ultravistaListRemeasurement, vhsDetection, vhsListRemeasurement, videoDetection, videoListRemeasurement, vikingDetection, vikingListRemeasurement, vmcDetection, vmcListRemeasurement, vvvDetection, vvvListRemeasurement	VSAQC	Calibrated Kron magnitude within circular aperture r_k	real	4	mag		PHOT_INT-MAG
kronMagErr	svNgc253Detection	VSASVNGC253	error on calibrated Kron magnitude	real	4	mag		ERROR
kronMagErr	svOrionDetection	VSASVORION	error on calibrated Kron magnitude	real	4	mag		ERROR
kronMagErr	ultravistaDetection	VSAUltraVISTA	error on calibrated Kron magnitude	real	4	mag		ERROR
kronMagErr	ultravistaDetection, ultravistaListRemeasurement, vhsDetection, vhsListRemeasurement, videoDetection, videoListRemeasurement, vikingDetection, vikingListRemeasurement, vmcDetection, vmcListRemeasurement, vvvDetection, vvvListRemeasurement	VSAQC	error on calibrated Kron magnitude	real	4	mag		ERROR
kronRad	svNgc253Detection	VSASVNGC253	r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius}	real	4	pixels		EXTENSION_RAD
kronRad	svOrionDetection	VSASVORION	r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius}	real	4	pixels		EXTENSION_RAD
kronRad	ultravistaDetection	VSAUltraVISTA	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		EXTENSION_RAD
			Since <FLUX>_RADIUS is expressed in multiples of the major axis, <FLUX>_RADIUS is multiplied by A_IMAGE to convert to pixels.
kronRad	ultravistaDetection, videoDetection	VSAQC	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		EXTENSION_RAD
			Since <FLUX>_RADIUS is expressed in multiples of the major axis, <FLUX>_RADIUS is multiplied by A_IMAGE to convert to pixels.
kronRad	ultravistaListRemeasurement	VSAUltraVISTA	r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius}	real	4	pixels		EXTENSION_RAD
kronRad	ultravistaListRemeasurement, vhsDetection, vhsListRemeasurement, videoListRemeasurement, vikingDetection, vikingListRemeasurement, vmcDetection, vmcListRemeasurement, vvvDetection, vvvListRemeasurement	VSAQC	r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius}	real	4	pixels		EXTENSION_RAD
ksAperMag1	vmcSynopticSource	VSAQC	Extended source Ks aperture corrected mag (0.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	PHOT_MAG
ksAperMag1	vmcSynopticSource	VSAVMC	Extended source Ks aperture corrected mag (0.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	PHOT_MAG
ksAperMag1	vvvSource	VSAQC	Extended source Ks aperture corrected mag (0.7 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	PHOT_MAG
ksAperMag1	vvvSource	VSAVVV	Extended source Ks aperture corrected mag (0.7 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	PHOT_MAG
ksAperMag1Err	vmcSynopticSource	VSAQC	Error in extended source Ks mag (0.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	ERROR
ksAperMag1Err	vmcSynopticSource	VSAVMC	Error in extended source Ks mag (0.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	ERROR
ksAperMag1Err	vvvSource	VSAQC	Error in extended source Ks mag (1.4 arcsec aperture diameter)	real	4	mag	-0.9999995e9	ERROR
ksAperMag1Err	vvvSource	VSAVVV	Error in extended source Ks mag (1.4 arcsec aperture diameter)	real	4	mag	-0.9999995e9	ERROR
ksAperMag2	vmcSynopticSource	VSAQC	Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter)	real	4	mag	-0.9999995e9	PHOT_MAG
ksAperMag2	vmcSynopticSource	VSAVMC	Extended source Ks aperture corrected mag (1.4 arcsec aperture diameter)	real	4	mag	-0.9999995e9	PHOT_MAG
ksAperMag2Err	vmcSynopticSource	VSAQC	Error in extended source Ks mag (1.4 arcsec aperture diameter)	real	4	mag	-0.9999995e9	ERROR
ksAperMag2Err	vmcSynopticSource	VSAVMC	Error in extended source Ks mag (1.4 arcsec aperture diameter)	real	4	mag	-0.9999995e9	ERROR
ksAperMag3	svNgc253Source	VSASVNGC253	Default point/extended 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	svOrionSource	VSASVORION	Default point/extended 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	ultravistaSource	VSAUltraVISTA	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	ultravistaSource, videoSource	VSAQC	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	vhsSource	VSAVHS	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, vikingSource, vmcSource	VSAQC	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	vmcSynopticSource	VSAQC	Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	PHOT_MAG
ksAperMag3	vmcSynopticSource	VSAVMC	Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	PHOT_MAG
ksAperMag3	vvvSource	VSAQC	Default point/extended 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	vvvSource	VSAVVV	Default point/extended source Ks aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator	real	4	mag	-0.9999995e9	PHOT_MAG
ksAperMag3Err	svNgc253Source	VSASVNGC253	Error in default point/extended source Ks mag (2.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	ERROR
ksAperMag3Err	svOrionSource	VSASVORION	Error in default point/extended source Ks mag (2.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	ERROR
ksAperMag3Err	ultravistaSource	VSAUltraVISTA	Error in default point/extended source Ks mag (2.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	ERROR
ksAperMag3Err	ultravistaSource, vhsSource, videoSource, vikingSource, vmcSource, vmcSynopticSource, vvvSource	VSAQC	Error in default point/extended source Ks mag (2.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	ERROR
ksAperMag4	svNgc253Source	VSASVNGC253	Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	PHOT_MAG
ksAperMag4	svOrionSource	VSASVORION	Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	PHOT_MAG
ksAperMag4	ultravistaSource	VSAUltraVISTA	Extended source Ks mag, no aperture correction applied	real	4	mag	-0.9999995e9	PHOT_MAG
ksAperMag4	ultravistaSource, videoSource	VSAQC	Extended source Ks mag, no aperture correction applied	real	4	mag	-0.9999995e9	PHOT_MAG
ksAperMag4	vhsSource	VSAVHS	Point source Ks aperture corrected mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	PHOT_MAG
ksAperMag4	vhsSource, vikingSource, vmcSource	VSAQC	Point source Ks aperture corrected mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	PHOT_MAG
ksAperMag4	vmcSynopticSource	VSAVMC	Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	PHOT_MAG
ksAperMag4	vmcSynopticSource, vvvSource	VSAQC	Extended source Ks aperture corrected mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	PHOT_MAG
ksAperMag4Err	svNgc253Source	VSASVNGC253	Error in extended source Ks mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	ERROR
ksAperMag4Err	svOrionSource	VSASVORION	Error in extended source Ks mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	ERROR
ksAperMag4Err	ultravistaSource	VSAUltraVISTA	Error in extended source Ks mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	ERROR
ksAperMag4Err	ultravistaSource, videoSource, vmcSynopticSource, vvvSource	VSAQC	Error in extended source Ks mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	ERROR
ksAperMag4Err	vhsSource	VSAVHS	Error in point/extended source Ks mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	ERROR
ksAperMag4Err	vhsSource, vikingSource, vmcSource	VSAQC	Error in point/extended source Ks mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	ERROR
ksAperMag5	vmcSynopticSource	VSAQC	Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	PHOT_MAG
ksAperMag5	vmcSynopticSource	VSAVMC	Extended source Ks aperture corrected mag (4.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	PHOT_MAG
ksAperMag5Err	vmcSynopticSource	VSAQC	Error in extended source Ks mag (4.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	ERROR
ksAperMag5Err	vmcSynopticSource	VSAVMC	Error in extended source Ks mag (4.0 arcsec aperture diameter)	real	4	mag	-0.9999995e9	ERROR
ksAperMag6	svNgc253Source	VSASVNGC253	Extended source Ks aperture corrected mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	PHOT_MAG
ksAperMag6	svOrionSource	VSASVORION	Extended source Ks aperture corrected mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	PHOT_MAG
ksAperMag6	ultravistaSource	VSAUltraVISTA	Extended source Ks mag, no aperture correction applied	real	4	mag	-0.9999995e9	PHOT_MAG
ksAperMag6	ultravistaSource, videoSource	VSAQC	Extended source Ks mag, no aperture correction applied	real	4	mag	-0.9999995e9	PHOT_MAG
ksAperMag6	vhsSource	VSAVHS	Point source Ks aperture corrected mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	PHOT_MAG
ksAperMag6	vhsSource, vikingSource, vmcSource	VSAQC	Point source Ks aperture corrected mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	PHOT_MAG
ksAperMag6Err	svNgc253Source	VSASVNGC253	Error in extended source Ks mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	ERROR
ksAperMag6Err	svOrionSource	VSASVORION	Error in extended source Ks mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	ERROR
ksAperMag6Err	ultravistaSource	VSAUltraVISTA	Error in extended source Ks mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	ERROR
ksAperMag6Err	ultravistaSource, videoSource	VSAQC	Error in extended source Ks mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	ERROR
ksAperMag6Err	vhsSource	VSAVHS	Error in point/extended source Ks mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	ERROR
ksAperMag6Err	vhsSource, vikingSource, vmcSource	VSAQC	Error in point/extended source Ks mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	ERROR
ksAperMagNoAperCorr3	vhsSource	VSAVHS	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, vikingSource, vmcSource	VSAQC	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
ksAperMagNoAperCorr4	vhsSource	VSAVHS	Extended source Ks aperture mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	PHOT_MAG
ksAperMagNoAperCorr4	vhsSource, vikingSource, vmcSource	VSAQC	Extended source Ks aperture mag (2.8 arcsec aperture diameter)	real	4	mag	-0.9999995e9	PHOT_MAG
ksAperMagNoAperCorr6	vhsSource	VSAVHS	Extended source Ks aperture mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	PHOT_MAG
ksAperMagNoAperCorr6	vhsSource, vikingSource, vmcSource	VSAQC	Extended source Ks aperture mag (5.7 arcsec aperture diameter)	real	4	mag	-0.9999995e9	PHOT_MAG
ksaStratAst	videoVarFrameSetInfo	VSAVIDEO	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, vikingVarFrameSetInfo, vmcVarFrameSetInfo, vvvVarFrameSetInfo	VSAQC	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.
ksaStratPht	videoVarFrameSetInfo	VSAVIDEO	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, vikingVarFrameSetInfo, vmcVarFrameSetInfo, vvvVarFrameSetInfo	VSAQC	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.
ksAverageConf	svNgc253Source	VSASVNGC253	average confidence in 2 arcsec diameter default aperture (aper3) Ks	real	4		-99999999	CODE_MISC
ksAverageConf	svOrionSource	VSASVORION	average confidence in 2 arcsec diameter default aperture (aper3) Ks	real	4		-99999999	CODE_MISC
ksAverageConf	vhsSource	VSAVHS	average confidence in 2 arcsec diameter default aperture (aper3) Ks	real	4		-99999999	CODE_MISC
ksAverageConf	vhsSource, vikingSource, vmcSource, vmcSynopticSource	VSAQC	average confidence in 2 arcsec diameter default aperture (aper3) Ks	real	4		-99999999	CODE_MISC
ksbestAper	videoVariability	VSAVIDEO	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, vikingVariability, vmcVariability, vvvVariability	VSAQC	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)
ksbStratAst	videoVarFrameSetInfo	VSAVIDEO	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, vikingVarFrameSetInfo, vmcVarFrameSetInfo, vvvVarFrameSetInfo	VSAQC	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.
ksbStratPht	videoVarFrameSetInfo	VSAVIDEO	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, vikingVarFrameSetInfo, vmcVarFrameSetInfo, vvvVarFrameSetInfo	VSAQC	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.
kschiSqAst	videoVarFrameSetInfo	VSAVIDEO	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, vikingVarFrameSetInfo, vmcVarFrameSetInfo, vvvVarFrameSetInfo	VSAQC	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.
kschiSqpd	videoVariability	VSAVIDEO	Chi square (per degree of freedom) fit to data (mean and expected rms)	real	4		-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
kschiSqpd	videoVariability, vikingVariability, vmcVariability, vvvVariability	VSAQC	Chi square (per degree of freedom) fit to data (mean and expected rms)	real	4		-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
kschiSqPht	videoVarFrameSetInfo	VSAVIDEO	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, vikingVarFrameSetInfo, vmcVarFrameSetInfo, vvvVarFrameSetInfo	VSAQC	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.
ksClass	svNgc253Source	VSASVNGC253	discrete image classification flag in Ks	smallint	2		-9999	CLASS_MISC
ksClass	svOrionSource	VSASVORION	discrete image classification flag in Ks	smallint	2		-9999	CLASS_MISC
ksClass	ultravistaSource	VSAUltraVISTA	discrete image classification flag in Ks	smallint	2		-9999	CLASS_MISC
ksClass	ultravistaSource, ultravistaSourceRemeasurement, vhsSource, vhsSourceRemeasurement, videoSource, videoSourceRemeasurement, vikingSource, vikingSourceRemeasurement, vmcSource, vmcSourceRemeasurement, vmcSynopticSource, vvvSource, vvvSourceRemeasurement	VSAQC	discrete image classification flag in Ks	smallint	2		-9999	CLASS_MISC
ksClassStat	svNgc253Source	VSASVNGC253	N(0,1) stellarness-of-profile statistic in Ks	real	4		-0.9999995e9	STAT_PROP
ksClassStat	svOrionSource	VSASVORION	N(0,1) stellarness-of-profile statistic in Ks	real	4		-0.9999995e9	STAT_PROP
ksClassStat	ultravistaSource	VSAUltraVISTA	S-Extractor classification statistic in Ks	real	4		-0.9999995e9	STAT_PROP
ksClassStat	ultravistaSource, videoSource, vvvSource	VSAQC	S-Extractor classification statistic in Ks	real	4		-0.9999995e9	STAT_PROP
ksClassStat	ultravistaSourceRemeasurement	VSAUltraVISTA	N(0,1) stellarness-of-profile statistic in Ks	real	4		-0.9999995e9	STAT_PROP
ksClassStat	ultravistaSourceRemeasurement, vhsSource, vhsSourceRemeasurement, videoSourceRemeasurement, vikingSource, vikingSourceRemeasurement, vmcSource, vmcSourceRemeasurement, vmcSynopticSource, vvvSourceRemeasurement	VSAQC	N(0,1) stellarness-of-profile statistic in Ks	real	4		-0.9999995e9	STAT_PROP
kscStratAst	videoVarFrameSetInfo	VSAVIDEO	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, vikingVarFrameSetInfo, vmcVarFrameSetInfo, vvvVarFrameSetInfo	VSAQC	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.
kscStratPht	videoVarFrameSetInfo	VSAVIDEO	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, vikingVarFrameSetInfo, vmcVarFrameSetInfo, vvvVarFrameSetInfo	VSAQC	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.
ksDeblend	ultravistaSource	VSAUltraVISTA	placeholder flag indicating parent/child relation in Ks	int	4		-99999999	CODE_MISC
ksDeblend	ultravistaSource, ultravistaSourceRemeasurement, vhsSourceRemeasurement, videoSource, videoSourceRemeasurement, vikingSourceRemeasurement, vmcSourceRemeasurement, vvvSource, vvvSourceRemeasurement	VSAQC	placeholder flag indicating parent/child relation in Ks	int	4		-99999999	CODE_MISC
ksEll	svNgc253Source	VSASVNGC253	1-b/a, where a/b=semi-major/minor axes in Ks	real	4		-0.9999995e9	PHYS_ELLIPTICITY
ksEll	svOrionSource	VSASVORION	1-b/a, where a/b=semi-major/minor axes in Ks	real	4		-0.9999995e9	PHYS_ELLIPTICITY
ksEll	ultravistaSource	VSAUltraVISTA	1-b/a, where a/b=semi-major/minor axes in Ks	real	4		-0.9999995e9	PHYS_ELLIPTICITY
ksEll	ultravistaSource, ultravistaSourceRemeasurement, vhsSource, vhsSourceRemeasurement, videoSource, videoSourceRemeasurement, vikingSource, vikingSourceRemeasurement, vmcSource, vmcSourceRemeasurement, vmcSynopticSource, vvvSource, vvvSourceRemeasurement	VSAQC	1-b/a, where a/b=semi-major/minor axes in Ks	real	4		-0.9999995e9	PHYS_ELLIPTICITY
kseNum	svNgc253MergeLog	VSASVNGC253	the extension number of this Ks frame	tinyint	1			NUMBER
kseNum	svOrionMergeLog	VSASVORION	the extension number of this Ks frame	tinyint	1			NUMBER
kseNum	ultravistaMergeLog	VSAUltraVISTA	the extension number of this Ks frame	tinyint	1			NUMBER
kseNum	ultravistaMergeLog, vhsMergeLog, videoMergeLog, vikingMergeLog, vmcMergeLog, vmcSynopticMergeLog, vvvMergeLog	VSAQC	the extension number of this Ks frame	tinyint	1			NUMBER
ksErrBits	svNgc253Source	VSASVNGC253	processing warning/error bitwise flags in Ks	int	4		-99999999	CODE_MISC
			Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits	svOrionSource	VSASVORION	processing warning/error bitwise flags in Ks	int	4		-99999999	CODE_MISC
			Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits	ultravistaSource	VSAUltraVISTA	processing warning/error bitwise flags in Ks	int	4		-99999999	CODE_MISC
			This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows: Bit Flag Meaning 1 The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected). 2 The object was originally blended with another 4 At least one pixel is saturated (or very close to) 8 The object is truncated (too close to an image boundary) 16 Object's aperture data are incomplete or corrupted 32 Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters. 64 Memory overflow occurred during deblending 128 Memory overflow occurred during extraction
ksErrBits	ultravistaSource, videoSource	VSAQC	processing warning/error bitwise flags in Ks	int	4		-99999999	CODE_MISC
			This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows: Bit Flag Meaning 1 The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected). 2 The object was originally blended with another 4 At least one pixel is saturated (or very close to) 8 The object is truncated (too close to an image boundary) 16 Object's aperture data are incomplete or corrupted 32 Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters. 64 Memory overflow occurred during deblending 128 Memory overflow occurred during extraction
ksErrBits	ultravistaSourceRemeasurement	VSAUltraVISTA	processing warning/error bitwise flags in Ks	int	4		-99999999	CODE_MISC
ksErrBits	ultravistaSourceRemeasurement, vhsSourceRemeasurement, videoSourceRemeasurement, vikingSourceRemeasurement, vmcSourceRemeasurement, vvvSourceRemeasurement	VSAQC	processing warning/error bitwise flags in Ks	int	4		-99999999	CODE_MISC
ksErrBits	vhsSource	VSAVHS	processing warning/error bitwise flags in Ks	int	4		-99999999	CODE_MISC
			Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksErrBits	vhsSource, vikingSource, vmcSource, vmcSynopticSource, vvvSource	VSAQC	processing warning/error bitwise flags in Ks	int	4		-99999999	CODE_MISC
			Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
ksEta	svNgc253Source	VSASVNGC253	Offset of Ks detection from master position (+north/-south)	real	4	arcsec	-0.9999995e9	POS_EQ_DEC_OFF
			When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want.
ksEta	svOrionSource	VSASVORION	Offset of Ks detection from master position (+north/-south)	real	4	arcsec	-0.9999995e9	POS_EQ_DEC_OFF
			When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want.
ksEta	ultravistaSource	VSAUltraVISTA	Offset of Ks detection from master position (+north/-south)	real	4	arcsec	-0.9999995e9	POS_EQ_DEC_OFF
			When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want.
ksEta	ultravistaSource, vhsSource, videoSource, vikingSource, vmcSource, vmcSynopticSource, vvvSource	VSAQC	Offset of Ks detection from master position (+north/-south)	real	4	arcsec	-0.9999995e9	POS_EQ_DEC_OFF
			When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want.
ksexpML	videoVarFrameSetInfo	VSAVIDEO	Expected magnitude limit of frameSet in this in Ks band.	real	4		-0.9999995e9
ksexpML	videoVarFrameSetInfo, vikingVarFrameSetInfo, vmcVarFrameSetInfo, vvvVarFrameSetInfo	VSAQC	Expected magnitude limit of frameSet in this in Ks band.	real	4		-0.9999995e9
ksExpRms	videoVariability	VSAVIDEO	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, vikingVariability, vmcVariability, vvvVariability	VSAQC	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.
ksGausig	svNgc253Source	VSASVNGC253	RMS of axes of ellipse fit in Ks	real	4	pixels	-0.9999995e9	MORPH_PARAM
ksGausig	svOrionSource	VSASVORION	RMS of axes of ellipse fit in Ks	real	4	pixels	-0.9999995e9	MORPH_PARAM
ksGausig	ultravistaSource	VSAUltraVISTA	RMS of axes of ellipse fit in Ks	real	4	pixels	-0.9999995e9	MORPH_PARAM
ksGausig	ultravistaSource, ultravistaSourceRemeasurement, vhsSource, vhsSourceRemeasurement, videoSource, videoSourceRemeasurement, vikingSource, vikingSourceRemeasurement, vmcSource, vmcSourceRemeasurement, vmcSynopticSource, vvvSource, vvvSourceRemeasurement	VSAQC	RMS of axes of ellipse fit in Ks	real	4	pixels	-0.9999995e9	MORPH_PARAM
ksHlCorSMjRadAs	svNgc253Source	VSASVNGC253	Seeing corrected half-light, semi-major axis in Ks band	real	4	arcsec	-0.9999995e9	EXTENSION_RAD
ksHlCorSMjRadAs	ultravistaSource	VSAUltraVISTA	Seeing corrected half-light, semi-major axis in Ks band	real	4	arcsec	-0.9999995e9	EXTENSION_RAD
ksHlCorSMjRadAs	ultravistaSource, vhsSource, videoSource, vikingSource	VSAQC	Seeing corrected half-light, semi-major axis in Ks band	real	4	arcsec	-0.9999995e9	EXTENSION_RAD
ksIntRms	videoVariability	VSAVIDEO	Intrinsic rms 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.
ksIntRms	videoVariability, vikingVariability, vmcVariability, vvvVariability	VSAQC	Intrinsic rms 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.
ksMag	ultravistaSourceRemeasurement	VSAUltraVISTA	Ks mag (as appropriate for this merged source)	real	4	mag	-0.9999995e9	PHOT_MAG
ksMag	ultravistaSourceRemeasurement, vhsSourceRemeasurement, videoSourceRemeasurement, vikingSourceRemeasurement, vmcSourceRemeasurement, vvvSourceRemeasurement	VSAQC	Ks mag (as appropriate for this merged source)	real	4	mag	-0.9999995e9	PHOT_MAG
ksMagErr	ultravistaSourceRemeasurement	VSAUltraVISTA	Error in Ks mag	real	4	mag	-0.9999995e9	ERROR
ksMagErr	ultravistaSourceRemeasurement, vhsSourceRemeasurement, videoSourceRemeasurement, vikingSourceRemeasurement, vmcSourceRemeasurement, vvvSourceRemeasurement	VSAQC	Error in Ks mag	real	4	mag	-0.9999995e9	ERROR
ksMagMAD	videoVariability	VSAVIDEO	Median Absolute Deviation of Ks magnitude	real	4	mag	-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
ksMagMAD	videoVariability, vikingVariability, vmcVariability, vvvVariability	VSAQC	Median Absolute Deviation of Ks magnitude	real	4	mag	-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
ksMagRms	videoVariability	VSAVIDEO	rms of Ks magnitude	real	4	mag	-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
ksMagRms	videoVariability, vikingVariability, vmcVariability, vvvVariability	VSAQC	rms of Ks magnitude	real	4	mag	-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
ksmaxCadence	videoVariability	VSAVIDEO	maximum gap between observations	real	4	days	-0.9999995e9
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
ksmaxCadence	videoVariability, vikingVariability, vmcVariability, vvvVariability	VSAQC	maximum gap between observations	real	4	days	-0.9999995e9
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
ksMaxMag	videoVariability	VSAVIDEO	Maximum magnitude in Ks band, of good detections	real	4		-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
ksMaxMag	videoVariability, vikingVariability, vmcVariability, vvvVariability	VSAQC	Maximum magnitude in Ks band, of good detections	real	4		-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
ksmeanMag	videoVariability	VSAVIDEO	Mean Ks magnitude	real	4	mag	-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
ksmeanMag	videoVariability, vikingVariability, vmcVariability, vvvVariability	VSAQC	Mean Ks magnitude	real	4	mag	-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
ksmedCadence	videoVariability	VSAVIDEO	median gap between observations	real	4	days	-0.9999995e9
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
ksmedCadence	videoVariability, vikingVariability, vmcVariability, vvvVariability	VSAQC	median gap between observations	real	4	days	-0.9999995e9
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
ksmedianMag	videoVariability	VSAVIDEO	Median Ks magnitude	real	4	mag	-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
ksmedianMag	videoVariability, vikingVariability, vmcVariability, vvvVariability	VSAQC	Median Ks magnitude	real	4	mag	-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
ksmfID	svNgc253MergeLog	VSASVNGC253	the UID of the relevant Ks multiframe	bigint	8			ID_FRAME
ksmfID	svOrionMergeLog	VSASVORION	the UID of the relevant Ks multiframe	bigint	8			ID_FRAME
ksmfID	ultravistaMergeLog	VSAUltraVISTA	the UID of the relevant Ks multiframe	bigint	8			ID_FRAME
ksmfID	ultravistaMergeLog, vhsMergeLog, videoMergeLog, vikingMergeLog, vmcMergeLog, vmcSynopticMergeLog, vvvMergeLog	VSAQC	the UID of the relevant Ks multiframe	bigint	8			ID_FRAME
ksminCadence	videoVariability	VSAVIDEO	minimum gap between observations	real	4	days	-0.9999995e9
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
ksminCadence	videoVariability, vikingVariability, vmcVariability, vvvVariability	VSAQC	minimum gap between observations	real	4	days	-0.9999995e9
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
ksMinMag	videoVariability	VSAVIDEO	Minimum magnitude in Ks band, of good detections	real	4		-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
ksMinMag	videoVariability, vikingVariability, vmcVariability, vvvVariability	VSAQC	Minimum magnitude in Ks band, of good detections	real	4		-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
ksndof	videoVariability	VSAVIDEO	Number of degrees of freedom for chisquare	smallint	2		-9999
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
ksndof	videoVariability, vikingVariability, vmcVariability, vvvVariability	VSAQC	Number of degrees of freedom for chisquare	smallint	2		-9999
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
ksnDofAst	videoVarFrameSetInfo	VSAVIDEO	Number of degrees of freedom of astrometric fit in Ks band.	smallint	2		-9999
			The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
ksnDofAst	videoVarFrameSetInfo, vikingVarFrameSetInfo, vmcVarFrameSetInfo, vvvVarFrameSetInfo	VSAQC	Number of degrees of freedom of astrometric fit in Ks band.	smallint	2		-9999
			The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
ksnDofPht	videoVarFrameSetInfo	VSAVIDEO	Number of degrees of freedom of photometric fit in Ks band.	smallint	2		-9999
			The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
ksnDofPht	videoVarFrameSetInfo, vikingVarFrameSetInfo, vmcVarFrameSetInfo, vvvVarFrameSetInfo	VSAQC	Number of degrees of freedom of photometric fit in Ks band.	smallint	2		-9999
			The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
ksnFlaggedObs	videoVariability	VSAQC	Number of detections in Ks band flagged as potentially spurious by videoDetection.ppErrBits	int	4		0
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
ksnFlaggedObs	videoVariability	VSAVIDEO	Number of detections in Ks band flagged as potentially spurious by videoDetection.ppErrBits	int	4		0
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
ksnFlaggedObs	vikingVariability	VSAQC	Number of detections in Ks band flagged as potentially spurious by vikingDetection.ppErrBits	int	4		0
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
ksnFlaggedObs	vikingVariability	VSAVIKING	Number of detections in Ks band flagged as potentially spurious by vikingDetection.ppErrBits	int	4		0
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
ksnFlaggedObs	vmcVariability	VSAQC	Number of detections in Ks band flagged as potentially spurious by vmcDetection.ppErrBits	int	4		0
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
ksnFlaggedObs	vmcVariability	VSAVMC	Number of detections in Ks band flagged as potentially spurious by vmcDetection.ppErrBits	int	4		0
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
ksnFlaggedObs	vvvVariability	VSAQC	Number of detections in Ks band flagged as potentially spurious by vvvDetection.ppErrBits	int	4		0
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
ksnFlaggedObs	vvvVariability	VSAVVV	Number of detections in Ks band flagged as potentially spurious by vvvDetection.ppErrBits	int	4		0
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
ksnGoodObs	videoVariability	VSAVIDEO	Number of good detections in Ks band	int	4		0
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
ksnGoodObs	videoVariability, vikingVariability, vmcVariability, vvvVariability	VSAQC	Number of good detections in Ks band	int	4		0
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
ksNgt3sig	videoVariability	VSAVIDEO	Number of good detections in Ks-band that are more than 3 sigma deviations	smallint	2		-9999
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
ksNgt3sig	videoVariability, vikingVariability, vmcVariability, vvvVariability	VSAQC	Number of good detections in Ks-band that are more than 3 sigma deviations	smallint	2		-9999
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
ksnMissingObs	videoVariability	VSAVIDEO	Number of Ks band frames that this object should have been detected on and was not	int	4		0
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
ksnMissingObs	videoVariability, vikingVariability, vmcVariability, vvvVariability	VSAQC	Number of Ks band frames that this object should have been detected on and was not	int	4		0
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
ksPA	svNgc253Source	VSASVNGC253	ellipse fit celestial orientation in Ks	real	4	Degrees	-0.9999995e9	POS_POS-ANG
ksPA	svOrionSource	VSASVORION	ellipse fit celestial orientation in Ks	real	4	Degrees	-0.9999995e9	POS_POS-ANG
ksPA	ultravistaSource	VSAUltraVISTA	ellipse fit celestial orientation in Ks	real	4	Degrees	-0.9999995e9	POS_POS-ANG
ksPA	ultravistaSource, ultravistaSourceRemeasurement, vhsSource, vhsSourceRemeasurement, videoSource, videoSourceRemeasurement, vikingSource, vikingSourceRemeasurement, vmcSource, vmcSourceRemeasurement, vmcSynopticSource, vvvSource, vvvSourceRemeasurement	VSAQC	ellipse fit celestial orientation in Ks	real	4	Degrees	-0.9999995e9	POS_POS-ANG
ksPetroMag	svNgc253Source	VSASVNGC253	Extended source Ks mag (Petrosian)	real	4	mag	-0.9999995e9	PHOT_MAG
ksPetroMag	svOrionSource	VSASVORION	Extended source Ks mag (Petrosian)	real	4	mag	-0.9999995e9	PHOT_MAG
ksPetroMag	ultravistaSource	VSAUltraVISTA	Extended source Ks mag (Petrosian)	real	4	mag	-0.9999995e9	PHOT_MAG
ksPetroMag	ultravistaSource, vhsSource, videoSource, vikingSource, vmcSource	VSAQC	Extended source Ks mag (Petrosian)	real	4	mag	-0.9999995e9	PHOT_MAG
ksPetroMagErr	svNgc253Source	VSASVNGC253	Error in extended source Ks mag (Petrosian)	real	4	mag	-0.9999995e9	ERROR
ksPetroMagErr	svOrionSource	VSASVORION	Error in extended source Ks mag (Petrosian)	real	4	mag	-0.9999995e9	ERROR
ksPetroMagErr	ultravistaSource	VSAUltraVISTA	Error in extended source Ks mag (Petrosian)	real	4	mag	-0.9999995e9	ERROR
ksPetroMagErr	ultravistaSource, vhsSource, videoSource, vikingSource, vmcSource	VSAQC	Error in extended source Ks mag (Petrosian)	real	4	mag	-0.9999995e9	ERROR
ksppErrBits	svNgc253Source	VSASVNGC253	additional WFAU post-processing error bits in Ks	int	4		0	CODE_MISC
			Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings: Byte Bit Detection quality issue Threshold or bit mask Applies to Decimal Hexadecimal 0 4 Deblended 16 0x00000010 All VDFS catalogues 0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues 2 16 Close to saturated 65536 0x00010000 All VDFS catalogues 2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only 2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues 2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.
ksppErrBits	svOrionSource	VSASVORION	additional WFAU post-processing error bits in Ks	int	4		0	CODE_MISC
			Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings: Byte Bit Detection quality issue Threshold or bit mask Applies to Decimal Hexadecimal 0 4 Deblended 16 0x00000010 All VDFS catalogues 0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues 2 16 Close to saturated 65536 0x00010000 All VDFS catalogues 2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only 2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues 2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.
ksppErrBits	ultravistaSource	VSAUltraVISTA	additional WFAU post-processing error bits in Ks	int	4		0	CODE_MISC
ksppErrBits	ultravistaSource, ultravistaSourceRemeasurement, vhsSourceRemeasurement, videoSource, videoSourceRemeasurement, vikingSourceRemeasurement, vmcSourceRemeasurement, vvvSource, vvvSourceRemeasurement	VSAQC	additional WFAU post-processing error bits in Ks	int	4		0	CODE_MISC
ksppErrBits	vhsSource	VSAVHS	additional WFAU post-processing error bits in Ks	int	4		0	CODE_MISC
			Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings: Byte Bit Detection quality issue Threshold or bit mask Applies to Decimal Hexadecimal 0 4 Deblended 16 0x00000010 All VDFS catalogues 0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues 2 16 Close to saturated 65536 0x00010000 All VDFS catalogues 2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only 2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues 2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.
ksppErrBits	vhsSource, vikingSource, vmcSource, vmcSynopticSource	VSAQC	additional WFAU post-processing error bits in Ks	int	4		0	CODE_MISC
			Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings: Byte Bit Detection quality issue Threshold or bit mask Applies to Decimal Hexadecimal 0 4 Deblended 16 0x00000010 All VDFS catalogues 0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues 2 16 Close to saturated 65536 0x00010000 All VDFS catalogues 2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only 2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues 2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.
ksprobVar	videoVariability	VSAVIDEO	Probability of variable from chi-square (and other data)	real	4		-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
ksprobVar	videoVariability, vikingVariability, vmcVariability, vvvVariability	VSAQC	Probability of variable from chi-square (and other data)	real	4		-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
ksPsfMag	svNgc253Source	VSASVNGC253	Point source profile-fitted Ks mag	real	4	mag	-0.9999995e9	PHOT_MAG
ksPsfMag	svOrionSource	VSASVORION	Point source profile-fitted Ks mag	real	4	mag	-0.9999995e9	PHOT_MAG
ksPsfMag	ultravistaSource	VSAUltraVISTA	Not available in SE output	real	4	mag	-0.9999995e9	PHOT_MAG
ksPsfMag	ultravistaSource, videoSource	VSAQC	Not available in SE output	real	4	mag	-0.9999995e9	PHOT_MAG
ksPsfMag	vhsSource	VSAVHS	Point source profile-fitted Ks mag	real	4	mag	-0.9999995e9	PHOT_MAG
ksPsfMag	vhsSource, vikingSource, vmcSource	VSAQC	Point source profile-fitted Ks mag	real	4	mag	-0.9999995e9	PHOT_MAG
ksPsfMagErr	svNgc253Source	VSASVNGC253	Error in point source profile-fitted Ks mag	real	4	mag	-0.9999995e9	ERROR
ksPsfMagErr	svOrionSource	VSASVORION	Error in point source profile-fitted Ks mag	real	4	mag	-0.9999995e9	ERROR
ksPsfMagErr	ultravistaSource	VSAUltraVISTA	Not available in SE output	real	4	mag	-0.9999995e9	ERROR
ksPsfMagErr	ultravistaSource, videoSource	VSAQC	Not available in SE output	real	4	mag	-0.9999995e9	ERROR
ksPsfMagErr	vhsSource	VSAVHS	Error in point source profile-fitted Ks mag	real	4	mag	-0.9999995e9	ERROR
ksPsfMagErr	vhsSource, vikingSource, vmcSource	VSAQC	Error in point source profile-fitted Ks mag	real	4	mag	-0.9999995e9	ERROR
ksSeqNum	svNgc253Source	VSASVNGC253	the running number of the Ks detection	int	4		-99999999	ID_NUMBER
ksSeqNum	svOrionSource	VSASVORION	the running number of the Ks detection	int	4		-99999999	ID_NUMBER
ksSeqNum	ultravistaSource	VSAUltraVISTA	the running number of the Ks detection	int	4		-99999999	ID_NUMBER
ksSeqNum	ultravistaSource, vhsSource, videoSource, vikingSource, vmcSource, vmcSynopticSource, vvvSource	VSAQC	the running number of the Ks detection	int	4		-99999999	ID_NUMBER
ksSeqNum	ultravistaSourceRemeasurement	VSAUltraVISTA	the running number of the Ks remeasurement	int	4		-99999999	ID_NUMBER
ksSeqNum	ultravistaSourceRemeasurement, vhsSourceRemeasurement, videoSourceRemeasurement, vikingSourceRemeasurement, vmcSourceRemeasurement, vvvSourceRemeasurement	VSAQC	the running number of the Ks remeasurement	int	4		-99999999	ID_NUMBER
ksSerMag2D	svNgc253Source	VSASVNGC253	Extended source Ks mag (profile-fitted)	real	4	mag	-0.9999995e9	PHOT_MAG
ksSerMag2D	svOrionSource	VSASVORION	Extended source Ks mag (profile-fitted)	real	4	mag	-0.9999995e9	PHOT_MAG
ksSerMag2D	ultravistaSource	VSAUltraVISTA	Not available in SE output	real	4	mag	-0.9999995e9	PHOT_MAG
ksSerMag2D	ultravistaSource, videoSource	VSAQC	Not available in SE output	real	4	mag	-0.9999995e9	PHOT_MAG
ksSerMag2D	vhsSource	VSAVHS	Extended source Ks mag (profile-fitted)	real	4	mag	-0.9999995e9	PHOT_MAG
ksSerMag2D	vhsSource, vikingSource, vmcSource	VSAQC	Extended source Ks mag (profile-fitted)	real	4	mag	-0.9999995e9	PHOT_MAG
ksSerMag2DErr	svNgc253Source	VSASVNGC253	Error in extended source Ks mag (profile-fitted)	real	4	mag	-0.9999995e9	ERROR
ksSerMag2DErr	svOrionSource	VSASVORION	Error in extended source Ks mag (profile-fitted)	real	4	mag	-0.9999995e9	ERROR
ksSerMag2DErr	ultravistaSource	VSAUltraVISTA	Not available in SE output	real	4	mag	-0.9999995e9	ERROR
ksSerMag2DErr	ultravistaSource, videoSource	VSAQC	Not available in SE output	real	4	mag	-0.9999995e9	ERROR
ksSerMag2DErr	vhsSource	VSAVHS	Error in extended source Ks mag (profile-fitted)	real	4	mag	-0.9999995e9	ERROR
ksSerMag2DErr	vhsSource, vikingSource, vmcSource	VSAQC	Error in extended source Ks mag (profile-fitted)	real	4	mag	-0.9999995e9	ERROR
ksskewness	videoVariability	VSAVIDEO	Skewness in Ks band (see Sesar et al. 2007)	real	4		-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
ksskewness	videoVariability, vikingVariability, vmcVariability, vvvVariability	VSAQC	Skewness in Ks band (see Sesar et al. 2007)	real	4		-0.9999995e9
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
kstotalPeriod	videoVariability	VSAVIDEO	total period of observations (last obs-first obs)	real	4	days	-0.9999995e9
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
kstotalPeriod	videoVariability, vikingVariability, vmcVariability, vvvVariability	VSAQC	total period of observations (last obs-first obs)	real	4	days	-0.9999995e9
			The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable.
ksVarClass	videoVariability	VSAVIDEO	Classification of variability in this band	smallint	2		-9999
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
ksVarClass	videoVariability, vikingVariability, vmcVariability, vvvVariability	VSAQC	Classification of variability in this band	smallint	2		-9999
			The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
ksXi	svNgc253Source	VSASVNGC253	Offset of Ks detection from master position (+east/-west)	real	4	arcsec	-0.9999995e9	POS_EQ_RA_OFF
			When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want.
ksXi	svOrionSource	VSASVORION	Offset of Ks detection from master position (+east/-west)	real	4	arcsec	-0.9999995e9	POS_EQ_RA_OFF
			When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want.
ksXi	ultravistaSource	VSAUltraVISTA	Offset of Ks detection from master position (+east/-west)	real	4	arcsec	-0.9999995e9	POS_EQ_RA_OFF
			When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want.
ksXi	ultravistaSource, vhsSource, videoSource, vikingSource, vmcSource, vmcSynopticSource, vvvSource	VSAQC	Offset of Ks detection from master position (+east/-west)	real	4	arcsec	-0.9999995e9	POS_EQ_RA_OFF
			When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want.