H 
Name  Schema Table  Database  Description  Type  Length  Unit  Default Value  Unified Content Descriptor 
H 
twomass 
SIXDF 
H magnitude (HEXT) used for H selection 
real 
4 
mag 


h_1AperMag1 
vvvSource 
VVVDR5 
Point source H_1 aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
h_1AperMag1Err 
vvvSource 
VVVDR5 
Error in point source H_1 mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
h_1AperMag3 
vvvSource 
VVVDR5 
Default point source H_1 aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
h_1AperMag3Err 
vvvSource 
VVVDR5 
Error in default point source H_1 mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
h_1AperMag4 
vvvSource 
VVVDR5 
Point source H_1 aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
h_1AperMag4Err 
vvvSource 
VVVDR5 
Error in point source H_1 mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
h_1AverageConf 
vvvSource 
VVVDR5 
average confidence in 2 arcsec diameter default aperture (aper3) H_1 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.H 
h_1Class 
vvvSource 
VVVDR5 
discrete image classification flag in H_1 
smallint 
2 

9999 
src.class;em.IR.H 
h_1ClassStat 
vvvSource 
VVVDR5 
SExtractor classification statistic in H_1 
real 
4 

0.9999995e9 
stat;em.IR.H 
h_1Ell 
vvvSource 
VVVDR5 
1b/a, where a/b=semimajor/minor axes in H_1 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.H 
h_1eNum 
vvvMergeLog 
VVVDR5 
the extension number of this H_1 frame 
tinyint 
1 


meta.number;em.IR.H 
h_1eNum 
vvvPsfDophotZYJHKsMergeLog 
VVVDR5 
the extension number of this 1st epoch H frame 
tinyint 
1 


meta.number;em.IR.H 
h_1ErrBits 
vvvSource 
VVVDR5 
processing warning/error bitwise flags in H_1 
int 
4 

99999999 
meta.code;em.IR.H 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
h_1Eta 
vvvSource 
VVVDR5 
Offset of H_1 detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.H 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
h_1Gausig 
vvvSource 
VVVDR5 
RMS of axes of ellipse fit in H_1 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.IR.H 
h_1mfID 
vvvMergeLog 
VVVDR5 
the UID of the relevant H_1 multiframe 
bigint 
8 


meta.id;obs.field;em.IR.H 
h_1mfID 
vvvPsfDophotZYJHKsMergeLog 
VVVDR5 
the UID of the relevant 1st epoch H tile multiframe 
bigint 
8 


meta.id;obs.field;em.IR.H 
h_1Mjd 
vvvPsfDophotZYJHKsMergeLog 
VVVDR5 
the MJD of the 1st epoch H tile multiframe 
float 
8 


time;em.IR.H 
h_1Mjd 
vvvSource 
VVVDR5 
Modified Julian Day in H_1 band 
float 
8 
days 
0.9999995e9 
time.epoch;em.IR.H 
h_1mks_1Pnt 
vvvSource 
VVVDR5 
Point source colour H_1Ks_1 (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.IR.H;em.IR.K 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
h_1mks_1PntErr 
vvvSource 
VVVDR5 
Error on point source colour H_1Ks_1 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;em.IR.K 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
h_1PA 
vvvSource 
VVVDR5 
ellipse fit celestial orientation in H_1 
real 
4 
Degrees 
0.9999995e9 
pos.posAng;em.IR.H 
h_1ppErrBits 
vvvSource 
VVVDR5 
additional WFAU postprocessing error bits in H_1 
int 
4 

0 
meta.code;em.IR.H 
h_1SeqNum 
vvvSource 
VVVDR5 
the running number of the H_1 detection 
int 
4 

99999999 
meta.number;em.IR.H 
h_1Xi 
vvvSource 
VVVDR5 
Offset of H_1 detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff;em.IR.H 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
h_2AperMag1 
vvvSource 
VVVDR5 
Point source H_2 aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
h_2AperMag1Err 
vvvSource 
VVVDR5 
Error in point source H_2 mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
h_2AperMag3 
vvvSource 
VVVDR5 
Default point source H_2 aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
h_2AperMag3Err 
vvvSource 
VVVDR5 
Error in default point source H_2 mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
h_2AperMag4 
vvvSource 
VVVDR5 
Point source H_2 aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
h_2AperMag4Err 
vvvSource 
VVVDR5 
Error in point source H_2 mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
h_2AverageConf 
vvvSource 
VVVDR5 
average confidence in 2 arcsec diameter default aperture (aper3) H_2 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.H 
h_2Class 
vvvSource 
VVVDR5 
discrete image classification flag in H_2 
smallint 
2 

9999 
src.class;em.IR.H 
h_2ClassStat 
vvvSource 
VVVDR5 
SExtractor classification statistic in H_2 
real 
4 

0.9999995e9 
stat;em.IR.H 
h_2Ell 
vvvSource 
VVVDR5 
1b/a, where a/b=semimajor/minor axes in H_2 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.H 
h_2eNum 
vvvMergeLog 
VVVDR5 
the extension number of this H_2 frame 
tinyint 
1 


meta.number;em.IR.H 
h_2eNum 
vvvPsfDophotZYJHKsMergeLog 
VVVDR5 
the extension number of this 2nd epoch H frame 
tinyint 
1 


meta.number;em.IR.H 
h_2ErrBits 
vvvSource 
VVVDR5 
processing warning/error bitwise flags in H_2 
int 
4 

99999999 
meta.code;em.IR.H 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
h_2Eta 
vvvSource 
VVVDR5 
Offset of H_2 detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.H 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
h_2Gausig 
vvvSource 
VVVDR5 
RMS of axes of ellipse fit in H_2 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.IR.H 
h_2mfID 
vvvMergeLog 
VVVDR5 
the UID of the relevant H_2 multiframe 
bigint 
8 


meta.id;obs.field;em.IR.H 
h_2mfID 
vvvPsfDophotZYJHKsMergeLog 
VVVDR5 
the UID of the relevant 2nd epoch H tile multiframe 
bigint 
8 


meta.id;obs.field;em.IR.H 
h_2Mjd 
vvvPsfDophotZYJHKsMergeLog 
VVVDR5 
the MJD of the 2nd epoch H tile multiframe 
float 
8 


time;em.IR.H 
h_2Mjd 
vvvSource 
VVVDR5 
Modified Julian Day in H_2 band 
float 
8 
days 
0.9999995e9 
time.epoch;em.IR.H 
h_2mks_2Pnt 
vvvSource 
VVVDR5 
Point source colour H_2Ks_2 (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color;em.IR.H;em.IR.K 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
h_2mks_2PntErr 
vvvSource 
VVVDR5 
Error on point source colour H_2Ks_2 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;em.IR.K 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
h_2mrat 
twomass_scn 
TWOMASS 
Hband average 2nd image moment ratio. 
real 
4 


stat.fit.param 
h_2mrat 
twomass_sixx2_scn 
TWOMASS 
H band average 2nd image moment ratio for scan 
real 
4 



h_2PA 
vvvSource 
VVVDR5 
ellipse fit celestial orientation in H_2 
real 
4 
Degrees 
0.9999995e9 
pos.posAng;em.IR.H 
h_2ppErrBits 
vvvSource 
VVVDR5 
additional WFAU postprocessing error bits in H_2 
int 
4 

0 
meta.code;em.IR.H 
h_2SeqNum 
vvvSource 
VVVDR5 
the running number of the H_2 detection 
int 
4 

99999999 
meta.number;em.IR.H 
h_2Xi 
vvvSource 
VVVDR5 
Offset of H_2 detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff;em.IR.H 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
h_5sig_ba 
twomass_xsc 
TWOMASS 
H minor/major axis ratio fit to the 5sigma isophote. 
real 
4 


phys.size.axisRatio 
h_5sig_phi 
twomass_xsc 
TWOMASS 
H angle to 5sigma major axis (E of N). 
smallint 
2 
degrees 

stat.error 
h_5surf 
twomass_xsc 
TWOMASS 
H central surface brightness (r<=5). 
real 
4 
mag 

phot.mag.sb 
h_ba 
twomass_xsc 
TWOMASS 
H minor/major axis ratio fit to the 3sigma isophote. 
real 
4 


phys.size.axisRatio 
h_back 
twomass_xsc 
TWOMASS 
H coadd median background. 
real 
4 


meta.code 
h_bisym_chi 
twomass_xsc 
TWOMASS 
H bisymmetric crosscorrelation chi. 
real 
4 


stat.fit.param 
h_bisym_rat 
twomass_xsc 
TWOMASS 
H bisymmetric flux ratio. 
real 
4 


phot.flux;arith.ratio 
h_bndg_amp 
twomass_xsc 
TWOMASS 
H banding maximum FT amplitude on this side of coadd. 
real 
4 
DN 

stat.fit.param 
h_bndg_per 
twomass_xsc 
TWOMASS 
H banding Fourier Transf. period on this side of coadd. 
int 
4 
arcsec 

stat.fit.param 
h_cmsig 
twomass_psc 
TWOMASS 
Corrected photometric uncertainty for the default Hband magnitude. 
real 
4 
mag 
Hband 
phot.flux 
h_con_indx 
twomass_xsc 
TWOMASS 
H concentration index r_75%/r_25%. 
real 
4 


phys.size;arith.ratio 
h_d_area 
twomass_xsc 
TWOMASS 
H 5sigma to 3sigma differential area. 
smallint 
2 


stat.fit.residual 
h_flg_10 
twomass_xsc 
TWOMASS 
H confusion flag for 10 arcsec circular ap. mag. 
smallint 
2 


meta.code 
h_flg_15 
twomass_xsc 
TWOMASS 
H confusion flag for 15 arcsec circular ap. mag. 
smallint 
2 


meta.code 
h_flg_20 
twomass_xsc 
TWOMASS 
H confusion flag for 20 arcsec circular ap. mag. 
smallint 
2 


meta.code 
h_flg_25 
twomass_xsc 
TWOMASS 
H confusion flag for 25 arcsec circular ap. mag. 
smallint 
2 


meta.code 
h_flg_30 
twomass_xsc 
TWOMASS 
H confusion flag for 30 arcsec circular ap. mag. 
smallint 
2 


meta.code 
h_flg_40 
twomass_xsc 
TWOMASS 
H confusion flag for 40 arcsec circular ap. mag. 
smallint 
2 


meta.code 
h_flg_5 
twomass_xsc 
TWOMASS 
H confusion flag for 5 arcsec circular ap. mag. 
smallint 
2 


meta.code 
h_flg_50 
twomass_xsc 
TWOMASS 
H confusion flag for 50 arcsec circular ap. mag. 
smallint 
2 


meta.code 
h_flg_60 
twomass_xsc 
TWOMASS 
H confusion flag for 60 arcsec circular ap. mag. 
smallint 
2 


meta.code 
h_flg_7 
twomass_sixx2_xsc 
TWOMASS 
H confusion flag for 7 arcsec circular ap. mag 
smallint 
2 



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


meta.code 
h_flg_70 
twomass_xsc 
TWOMASS 
H confusion flag for 70 arcsec circular ap. mag. 
smallint 
2 


meta.code 
h_flg_c 
twomass_xsc 
TWOMASS 
H confusion flag for Kron circular mag. 
smallint 
2 


meta.code 
h_flg_e 
twomass_xsc 
TWOMASS 
H confusion flag for Kron elliptical mag. 
smallint 
2 


meta.code 
h_flg_fc 
twomass_xsc 
TWOMASS 
H confusion flag for fiducial Kron circ. mag. 
smallint 
2 


meta.code 
h_flg_fe 
twomass_xsc 
TWOMASS 
H confusion flag for fiducial Kron ell. mag. 
smallint 
2 


meta.code 
h_flg_i20c 
twomass_xsc 
TWOMASS 
H confusion flag for 20mag/sq." iso. circ. mag. 
smallint 
2 


meta.code 
h_flg_i20e 
twomass_xsc 
TWOMASS 
H confusion flag for 20mag/sq." iso. ell. mag. 
smallint 
2 


meta.code 
h_flg_i21c 
twomass_xsc 
TWOMASS 
H confusion flag for 21mag/sq." iso. circ. mag. 
smallint 
2 


meta.code 
h_flg_i21e 
twomass_xsc 
TWOMASS 
H confusion flag for 21mag/sq." iso. ell. mag. 
smallint 
2 


meta.code 
h_flg_j21fc 
twomass_xsc 
TWOMASS 
H confusion flag for 21mag/sq." iso. fid. circ. mag. 
smallint 
2 


meta.code 
h_flg_j21fe 
twomass_xsc 
TWOMASS 
H confusion flag for 21mag/sq." iso. fid. ell. mag. 
smallint 
2 


meta.code 
h_flg_k20fc 
twomass_xsc 
TWOMASS 
H confusion flag for 20mag/sq." iso. fid. circ. mag. 
smallint 
2 


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



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


meta.code 
h_k 
twomass_sixx2_psc 
TWOMASS 
The HKs color, computed from the Hband and Ksband magnitudes (h_m and k_m, respectively) of the source. In cases where the second or third digit in rd_flg is equal to either "0", "4", "6", or "9", no color is computed because the photometry in one or both bands is of lower quality or the source is not detected. 
real 
4 



h_m 
twomass_psc 
TWOMASS 
Default Hband magnitude 
real 
4 
mag 

phot.flux 
h_m 
twomass_sixx2_psc 
TWOMASS 
H selected "default" magnitude 
real 
4 
mag 


h_m_10 
twomass_xsc 
TWOMASS 
H 10 arcsec radius circular aperture magnitude. 
real 
4 
mag 

phot.flux 
h_m_15 
twomass_xsc 
TWOMASS 
H 15 arcsec radius circular aperture magnitude. 
real 
4 
mag 

phot.flux 
h_m_20 
twomass_xsc 
TWOMASS 
H 20 arcsec radius circular aperture magnitude. 
real 
4 
mag 

phot.flux 
h_m_25 
twomass_xsc 
TWOMASS 
H 25 arcsec radius circular aperture magnitude. 
real 
4 
mag 

phot.flux 
h_m_2mass 
allwise_sc 
WISE 
2MASS Hband magnitude or magnitude upper limit of the associated 2MASS PSC source. This column is "null" if there is no associated 2MASS PSC source or if the 2MASS PSC Hband magnitude entry is "null". 
float 
8 
mag 


h_m_2mass 
wise_allskysc 
WISE 
2MASS Hband magnitude or magnitude upper limit of the associated 2MASS PSC source. This column is default if there is no associated 2MASS PSC source or if the 2MASS PSC Hband magnitude entry is default. 
real 
4 
mag 
0.9999995e9 

h_m_2mass 
wise_prelimsc 
WISE 
2MASS Hband magnitude or magnitude upper limit of the associated 2MASS PSC source This column is default if there is no associated 2MASS PSC source or if the 2MASS PSC Hband magnitude entry is default 
real 
4 
mag 
0.9999995e9 

h_m_30 
twomass_xsc 
TWOMASS 
H 30 arcsec radius circular aperture magnitude. 
real 
4 
mag 

phot.flux 
h_m_40 
twomass_xsc 
TWOMASS 
H 40 arcsec radius circular aperture magnitude. 
real 
4 
mag 

phot.flux 
h_m_5 
twomass_xsc 
TWOMASS 
H 5 arcsec radius circular aperture magnitude. 
real 
4 
mag 

phot.flux 
h_m_50 
twomass_xsc 
TWOMASS 
H 50 arcsec radius circular aperture magnitude. 
real 
4 
mag 

phot.flux 
h_m_60 
twomass_xsc 
TWOMASS 
H 60 arcsec radius circular aperture magnitude. 
real 
4 
mag 

phot.flux 
h_m_7 
twomass_sixx2_xsc 
TWOMASS 
H 7 arcsec radius circular aperture magnitude 
real 
4 
mag 


h_m_7 
twomass_xsc 
TWOMASS 
H 7 arcsec radius circular aperture magnitude. 
real 
4 
mag 

phot.flux 
h_m_70 
twomass_xsc 
TWOMASS 
H 70 arcsec radius circular aperture magnitude. 
real 
4 
mag 

phot.flux 
h_m_c 
twomass_xsc 
TWOMASS 
H Kron circular aperture magnitude. 
real 
4 
mag 

phot.flux 
h_m_e 
twomass_xsc 
TWOMASS 
H Kron elliptical aperture magnitude. 
real 
4 
mag 

phot.flux 
h_m_ext 
twomass_sixx2_xsc 
TWOMASS 
H mag from fit extrapolation 
real 
4 
mag 


h_m_ext 
twomass_xsc 
TWOMASS 
H mag from fit extrapolation. 
real 
4 
mag 

phot.flux 
h_m_fc 
twomass_xsc 
TWOMASS 
H fiducial Kron circular magnitude. 
real 
4 
mag 

phot.flux 
h_m_fe 
twomass_xsc 
TWOMASS 
H fiducial Kron ell. mag aperture magnitude. 
real 
4 
mag 

phot.flux 
h_m_i20c 
twomass_xsc 
TWOMASS 
H 20mag/sq." isophotal circular ap. magnitude. 
real 
4 
mag 

phot.flux 
h_m_i20e 
twomass_xsc 
TWOMASS 
H 20mag/sq." isophotal elliptical ap. magnitude. 
real 
4 
mag 

phot.flux 
h_m_i21c 
twomass_xsc 
TWOMASS 
H 21mag/sq." isophotal circular ap. magnitude. 
real 
4 
mag 

phot.flux 
h_m_i21e 
twomass_xsc 
TWOMASS 
H 21mag/sq." isophotal elliptical ap. magnitude. 
real 
4 
mag 

phot.flux 
h_m_j21fc 
twomass_xsc 
TWOMASS 
H 21mag/sq." isophotal fiducial circ. ap. mag. 
real 
4 
mag 

phot.flux 
h_m_j21fe 
twomass_xsc 
TWOMASS 
H 21mag/sq." isophotal fiducial ell. ap. magnitude. 
real 
4 
mag 

phot.flux 
h_m_k20fc 
twomass_xsc 
TWOMASS 
H 20mag/sq." isophotal fiducial circ. ap. mag. 
real 
4 
mag 

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


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


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

phot.flux 
h_m_stdap 
twomass_psc 
TWOMASS 
Hband "standard" aperture magnitude. 
real 
4 
mag 

phot.flux 
h_m_sys 
twomass_xsc 
TWOMASS 
H system photometry magnitude. 
real 
4 
mag 

phot.flux 
h_mnsurfb_eff 
twomass_xsc 
TWOMASS 
H mean surface brightness at the halflight radius. 
real 
4 
mag 

phot.mag.sb 
h_msig 
twomass_sixx2_psc 
TWOMASS 
H "default" mag uncertainty 
real 
4 
mag 


h_msig_10 
twomass_xsc 
TWOMASS 
H 1sigma uncertainty in 10 arcsec circular ap. mag. 
real 
4 
mag 

stat.error 
h_msig_15 
twomass_xsc 
TWOMASS 
H 1sigma uncertainty in 15 arcsec circular ap. mag. 
real 
4 
mag 

stat.error 
h_msig_20 
twomass_xsc 
TWOMASS 
H 1sigma uncertainty in 20 arcsec circular ap. mag. 
real 
4 
mag 

stat.error 
h_msig_25 
twomass_xsc 
TWOMASS 
H 1sigma uncertainty in 25 arcsec circular ap. mag. 
real 
4 
mag 

stat.error 
h_msig_2mass 
allwise_sc 
WISE 
2MASS Hband corrected photometric uncertainty of the associated 2MASS PSC source. This column is "null" if there is no associated 2MASS PSC source or if the 2MASS PSC Hband uncertainty entry is "null". 
float 
8 
mag 


h_msig_2mass 
wise_allskysc 
WISE 
2MASS Hband corrected photometric uncertainty of the associated 2MASS PSC source. This column is default if there is no associated 2MASS PSC source or if the 2MASS PSC Hband uncertainty entry is default. 
real 
4 
mag 
0.9999995e9 

h_msig_2mass 
wise_prelimsc 
WISE 
2MASS Hband corrected photometric uncertainty of the associated 2MASS PSC source This column is default if there is no associated 2MASS PSC source or if the 2MASS PSC Hband uncertainty entry is default 
real 
4 
mag 
0.9999995e9 

h_msig_30 
twomass_xsc 
TWOMASS 
H 1sigma uncertainty in 30 arcsec circular ap. mag. 
real 
4 
mag 

stat.error 
h_msig_40 
twomass_xsc 
TWOMASS 
H 1sigma uncertainty in 40 arcsec circular ap. mag. 
real 
4 
mag 

stat.error 
h_msig_5 
twomass_xsc 
TWOMASS 
H 1sigma uncertainty in 5 arcsec circular ap. mag. 
real 
4 
mag 

stat.error 
h_msig_50 
twomass_xsc 
TWOMASS 
H 1sigma uncertainty in 50 arcsec circular ap. mag. 
real 
4 
mag 

stat.error 
h_msig_60 
twomass_xsc 
TWOMASS 
H 1sigma uncertainty in 60 arcsec circular ap. mag. 
real 
4 
mag 

stat.error 
h_msig_7 
twomass_sixx2_xsc 
TWOMASS 
H 1sigma uncertainty in 7 arcsec circular ap. mag 
real 
4 
mag 


h_msig_7 
twomass_xsc 
TWOMASS 
H 1sigma uncertainty in 7 arcsec circular ap. mag. 
real 
4 
mag 

stat.error 
h_msig_70 
twomass_xsc 
TWOMASS 
H 1sigma uncertainty in 70 arcsec circular ap. mag. 
real 
4 
mag 

stat.error 
h_msig_c 
twomass_xsc 
TWOMASS 
H 1sigma uncertainty in Kron circular mag. 
real 
4 
mag 

stat.error 
h_msig_e 
twomass_xsc 
TWOMASS 
H 1sigma uncertainty in Kron elliptical mag. 
real 
4 
mag 

stat.error 
h_msig_ext 
twomass_sixx2_xsc 
TWOMASS 
H 1sigma uncertainty in mag from fit extrapolation 
real 
4 
mag 


h_msig_ext 
twomass_xsc 
TWOMASS 
H 1sigma uncertainty in mag from fit extrapolation. 
real 
4 
mag 

stat.error 
h_msig_fc 
twomass_xsc 
TWOMASS 
H 1sigma uncertainty in fiducial Kron circ. mag. 
real 
4 
mag 

stat.error 
h_msig_fe 
twomass_xsc 
TWOMASS 
H 1sigma uncertainty in fiducial Kron ell. mag. 
real 
4 
mag 

stat.error 
h_msig_i20c 
twomass_xsc 
TWOMASS 
H 1sigma uncertainty in 20mag/sq." iso. circ. mag. 
real 
4 
mag 

stat.error 
h_msig_i20e 
twomass_xsc 
TWOMASS 
H 1sigma uncertainty in 20mag/sq." iso. ell. mag. 
real 
4 
mag 

stat.error 
h_msig_i21c 
twomass_xsc 
TWOMASS 
H 1sigma uncertainty in 21mag/sq." iso. circ. mag. 
real 
4 
mag 

stat.error 
h_msig_i21e 
twomass_xsc 
TWOMASS 
H 1sigma uncertainty in 21mag/sq." iso. ell. mag. 
real 
4 
mag 

stat.error 
h_msig_j21fc 
twomass_xsc 
TWOMASS 
H 1sigma uncertainty in 21mag/sq." iso.fid.circ.mag. 
real 
4 
mag 

stat.error 
h_msig_j21fe 
twomass_xsc 
TWOMASS 
H 1sigma uncertainty in 21mag/sq." iso.fid.ell.mag. 
real 
4 
mag 

stat.error 
h_msig_k20fc 
twomass_xsc 
TWOMASS 
H 1sigma uncertainty in 20mag/sq." iso.fid.circ. mag. 
real 
4 
mag 

stat.error 
h_msig_k20fe 
twomass_sixx2_xsc 
TWOMASS 
H 1sigma uncertainty in 20mag/sq.″ iso.fid.ell.mag 
real 
4 
mag 


h_msig_k20fe 
twomass_xsc 
TWOMASS 
H 1sigma uncertainty in 20mag/sq." iso.fid.ell.mag. 
real 
4 
mag 

stat.error 
h_msig_stdap 
twomass_psc 
TWOMASS 
Uncertainty in the Hband standard aperture magnitude. 
real 
4 
mag 

phot.flux 
h_msig_sys 
twomass_xsc 
TWOMASS 
H 1sigma uncertainty in system photometry mag. 
real 
4 
mag 

stat.error 
h_msigcom 
twomass_psc 
TWOMASS 
Combined, or total photometric uncertainty for the default Hband magnitude. 
real 
4 
mag 
Hband 
phot.flux 
h_msigcom 
twomass_sixx2_psc 
TWOMASS 
combined (total) H band photometric uncertainty 
real 
4 
mag 


h_msnr10 
twomass_scn 
TWOMASS 
The estimated Hband magnitude at which SNR=10 is achieved for this scan. 
real 
4 
mag 

phot.flux 
h_msnr10 
twomass_sixx2_scn 
TWOMASS 
H mag at which SNR=10 is achieved, from h_psp and h_zp_ap 
real 
4 
mag 


h_n_snr10 
twomass_scn 
TWOMASS 
Number of point sources at Hband with SNR>10 (instrumental mag <=15.1) 
int 
4 


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



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


stat.fit.param 
h_peak 
twomass_xsc 
TWOMASS 
H peak pixel brightness. 
real 
4 
mag 

phot.mag.sb 
h_perc_darea 
twomass_xsc 
TWOMASS 
H 5sigma to 3sigma percent area change. 
smallint 
2 


FIT_PARAM 
h_phi 
twomass_xsc 
TWOMASS 
H angle to 3sigma major axis (E of N). 
smallint 
2 
degrees 

pos.posAng 
h_psfchi 
twomass_psc 
TWOMASS 
Reduced chisquared goodnessoffit value for the Hband profilefit photometry made on the 1.3 s "Read_2" exposures. 
real 
4 


stat.fit.param 
h_psp 
twomass_scn 
TWOMASS 
Hband photometric sensitivity paramater (PSP). 
real 
4 


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



h_pts_noise 
twomass_scn 
TWOMASS 
Base10 logarithm of the mode of the noise distribution for all point source detections in the scan, where the noise is estimated from the measured Hband photometric errors and is expressed in units of mJy. 
real 
4 


instr.det.noise 
h_pts_noise 
twomass_sixx2_scn 
TWOMASS 
log10 of H band modal point src noise estimate 
real 
4 
logmJy 


h_r_c 
twomass_xsc 
TWOMASS 
H Kron circular aperture radius. 
real 
4 
arcsec 

phys.angSize;src 
h_r_e 
twomass_xsc 
TWOMASS 
H Kron elliptical aperture semimajor axis. 
real 
4 
arcsec 

phys.angSize;src 
h_r_eff 
twomass_xsc 
TWOMASS 
H halflight (integrated halfflux point) radius. 
real 
4 
arcsec 

phys.angSize;src 
h_r_i20c 
twomass_xsc 
TWOMASS 
H 20mag/sq." isophotal circular aperture radius. 
real 
4 
arcsec 

phys.angSize;src 
h_r_i20e 
twomass_xsc 
TWOMASS 
H 20mag/sq." isophotal elliptical ap. semimajor axis. 
real 
4 
arcsec 

phys.angSize;src 
h_r_i21c 
twomass_xsc 
TWOMASS 
H 21mag/sq." isophotal circular aperture radius. 
real 
4 
arcsec 

phys.angSize;src 
h_r_i21e 
twomass_xsc 
TWOMASS 
H 21mag/sq." isophotal elliptical ap. semimajor axis. 
real 
4 
arcsec 

phys.angSize;src 
h_resid_ann 
twomass_xsc 
TWOMASS 
H residual annulus background median. 
real 
4 
DN 

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


meta.code 
h_sc_2mm 
twomass_xsc 
TWOMASS 
H 2nd moment (score) (LCSB: SNRMAX  super SNR max). 
real 
4 


meta.code 
h_sc_msh 
twomass_xsc 
TWOMASS 
H median shape score. 
real 
4 


meta.code 
h_sc_mxdn 
twomass_xsc 
TWOMASS 
H mxdn (score) (LCSB: BSNR  block/smoothed SNR). 
real 
4 


meta.code 
h_sc_r1 
twomass_xsc 
TWOMASS 
H r1 (score). 
real 
4 


meta.code 
h_sc_r23 
twomass_xsc 
TWOMASS 
H r23 (score) (LCSB: TSNR  integrated SNR for r=15). 
real 
4 


meta.code 
h_sc_sh 
twomass_xsc 
TWOMASS 
H shape (score). 
real 
4 


meta.code 
h_sc_vint 
twomass_xsc 
TWOMASS 
H vint (score). 
real 
4 


meta.code 
h_sc_wsh 
twomass_xsc 
TWOMASS 
H wsh (score) (LCSB: PSNR  peak raw SNR). 
real 
4 


meta.code 
h_seetrack 
twomass_xsc 
TWOMASS 
H band seetracking score. 
real 
4 


meta.code 
h_sh0 
twomass_xsc 
TWOMASS 
H ridge shape (LCSB: BSNR limit). 
real 
4 


FIT_PARAM 
h_shape_avg 
twomass_scn 
TWOMASS 
Hband average seeing shape for scan. 
real 
4 


instr.obsty.seeing 
h_shape_avg 
twomass_sixx2_scn 
TWOMASS 
H band average seeing shape for scan 
real 
4 



h_shape_rms 
twomass_scn 
TWOMASS 
RMSerror of Hband average seeing shape. 
real 
4 


instr.obsty.seeing 
h_shape_rms 
twomass_sixx2_scn 
TWOMASS 
rms of H band avg seeing shape for scan 
real 
4 



h_sig_sh0 
twomass_xsc 
TWOMASS 
H ridge shape sigma (LCSB: B2SNR limit). 
real 
4 


FIT_PARAM 
h_snr 
twomass_psc 
TWOMASS 
Hband "scan" signaltonoise ratio. 
real 
4 
mag 

instr.det.noise 
h_snr 
twomass_sixx2_psc 
TWOMASS 
H band "scan" signaltonoise ratio 
real 
4 



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


meta.code 
h_zp_ap 
twomass_scn 
TWOMASS 
Photometric zeropoint for Hband aperture photometry. 
real 
4 
mag 

phot.mag;arith.zp 
h_zp_ap 
twomass_sixx2_scn 
TWOMASS 
H band ap. calibration photometric zeropoint for scan 
real 
4 
mag 


h_zperr_ap 
twomass_scn 
TWOMASS 
RMSerror of zeropoint for Hband aperture photometry 
real 
4 
mag 

stat.error 
h_zperr_ap 
twomass_sixx2_scn 
TWOMASS 
H band ap. calibration rms error of zeropoint for scan 
real 
4 
mag 


ha 
twomass_scn 
TWOMASS 
Hour angle at beginning of scan. 
float 
8 
hr 

pos.posAng 
ha 
twomass_sixx2_scn 
TWOMASS 
beginning hour angle of scan data 
float 
8 
hr 


halfFlux 
sharksDetection 
SHARKSv20210222 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
sharksDetection 
SHARKSv20210421 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
ultravistaDetection 
ULTRAVISTADR4 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation, not available in SE output {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vhsDetection 
VHSDR2 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count;em.opt 
halfFlux 
vhsDetection 
VHSDR3 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vhsDetection 
VHSDR4 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vhsDetection 
VHSDR5 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vhsDetection 
VHSDR6 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vhsDetection 
VHSv20120926 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vhsDetection 
VHSv20130417 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vhsDetection 
VHSv20140409 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vhsDetection 
VHSv20150108 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vhsDetection 
VHSv20160114 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vhsDetection 
VHSv20160507 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vhsDetection 
VHSv20170630 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vhsDetection 
VHSv20180419 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vhsDetection 
VHSv20201209 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vhsDetection, vhsListRemeasurement 
VHSDR1 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count;em.opt 
halfFlux 
videoDetection 
VIDEODR2 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation, not available in SE output {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count;em.opt 
halfFlux 
videoDetection 
VIDEODR3 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation, not available in SE output {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
videoDetection 
VIDEODR4 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation, not available in SE output {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
videoDetection 
VIDEODR5 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation, not available in SE output {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
videoDetection 
VIDEOv20100513 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation, not available in SE output {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count;em.opt 
halfFlux 
videoDetection 
VIDEOv20111208 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation, not available in SE output {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count;em.opt 
halfFlux 
videoListRemeasurement 
VIDEOv20100513 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count;em.opt 
halfFlux 
vikingDetection 
VIKINGDR2 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count;em.opt 
halfFlux 
vikingDetection 
VIKINGDR3 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vikingDetection 
VIKINGDR4 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vikingDetection 
VIKINGv20111019 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count;em.opt 
halfFlux 
vikingDetection 
VIKINGv20130417 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vikingDetection 
VIKINGv20140402 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vikingDetection 
VIKINGv20150421 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vikingDetection 
VIKINGv20151230 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vikingDetection 
VIKINGv20160406 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vikingDetection 
VIKINGv20161202 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vikingDetection 
VIKINGv20170715 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vikingDetection, vikingListRemeasurement 
VIKINGv20110714 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count;em.opt 
halfFlux 
vmcDetection 
VMCDR1 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count;em.opt 
halfFlux 
vmcDetection 
VMCDR2 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vmcDetection 
VMCDR3 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vmcDetection 
VMCDR4 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vmcDetection 
VMCDR5 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vmcDetection 
VMCv20110909 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count;em.opt 
halfFlux 
vmcDetection 
VMCv20120126 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count;em.opt 
halfFlux 
vmcDetection 
VMCv20121128 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vmcDetection 
VMCv20130304 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vmcDetection 
VMCv20130805 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vmcDetection 
VMCv20140428 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vmcDetection 
VMCv20140903 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vmcDetection 
VMCv20150309 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vmcDetection 
VMCv20151218 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vmcDetection 
VMCv20160311 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vmcDetection 
VMCv20160822 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vmcDetection 
VMCv20170109 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vmcDetection 
VMCv20170411 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vmcDetection 
VMCv20171101 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vmcDetection 
VMCv20180702 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vmcDetection 
VMCv20181120 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vmcDetection 
VMCv20191212 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vmcDetection 
VMCv20210708 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vmcDetection 
VMCv20230816 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vmcDetection, vmcListRemeasurement 
VMCv20110816 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count;em.opt 
halfFlux 
vmcdeepDetection 
VMCDEEPv20230713 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vvvDetection 
VVVDR1 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vvvDetection 
VVVDR2 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vvvDetection, vvvDetectionPawPrints, vvvDetectionTiles 
VVVDR5 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count 
halfFlux 
vvvDetection, vvvListRemeasurement 
VVVv20100531 
Half the total flux (max(isoFlux,aperFlux5), used in the halfRad calculation {catalogue TType keyword: Half_flux} 
real 
4 
ADU 
0.9999995e9 
phot.count;em.opt 
halfFluxErr 
sharksDetection 
SHARKSv20210222 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
sharksDetection 
SHARKSv20210421 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
ultravistaDetection 
ULTRAVISTADR4 
error on Half flux, not available in SE output {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vhsDetection 
VHSDR2 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vhsDetection 
VHSDR3 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vhsDetection 
VHSDR4 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vhsDetection 
VHSDR5 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vhsDetection 
VHSDR6 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vhsDetection 
VHSv20120926 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vhsDetection 
VHSv20130417 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vhsDetection 
VHSv20140409 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vhsDetection 
VHSv20150108 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vhsDetection 
VHSv20160114 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vhsDetection 
VHSv20160507 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vhsDetection 
VHSv20170630 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vhsDetection 
VHSv20180419 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vhsDetection 
VHSv20201209 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vhsDetection, vhsListRemeasurement 
VHSDR1 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
videoDetection 
VIDEODR2 
error on Half flux, not available in SE output {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
videoDetection 
VIDEODR3 
error on Half flux, not available in SE output {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
videoDetection 
VIDEODR4 
error on Half flux, not available in SE output {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
videoDetection 
VIDEODR5 
error on Half flux, not available in SE output {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
videoDetection 
VIDEOv20100513 
error on Half flux, not available in SE output {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
videoDetection 
VIDEOv20111208 
error on Half flux, not available in SE output {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
videoListRemeasurement 
VIDEOv20100513 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vikingDetection 
VIKINGDR2 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vikingDetection 
VIKINGDR3 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vikingDetection 
VIKINGDR4 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vikingDetection 
VIKINGv20111019 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vikingDetection 
VIKINGv20130417 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vikingDetection 
VIKINGv20140402 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vikingDetection 
VIKINGv20150421 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vikingDetection 
VIKINGv20151230 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vikingDetection 
VIKINGv20160406 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vikingDetection 
VIKINGv20161202 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vikingDetection 
VIKINGv20170715 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vikingDetection, vikingListRemeasurement 
VIKINGv20110714 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCDR1 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCDR2 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCDR3 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCDR4 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCDR5 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCv20110909 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCv20120126 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCv20121128 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCv20130304 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCv20130805 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCv20140428 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCv20140903 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCv20150309 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCv20151218 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCv20160311 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCv20160822 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCv20170109 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCv20170411 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCv20171101 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCv20180702 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCv20181120 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCv20191212 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCv20210708 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection 
VMCv20230816 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcDetection, vmcListRemeasurement 
VMCv20110816 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vmcdeepDetection 
VMCDEEPv20230713 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vvvDetection 
VVVDR1 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vvvDetection 
VVVDR2 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vvvDetection, vvvDetectionPawPrints, vvvDetectionTiles 
VVVDR5 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfFluxErr 
vvvDetection, vvvListRemeasurement 
VVVv20100531 
error on Half flux {catalogue TType keyword: Half_flux_err} 
real 
4 
ADU 
0.9999995e9 
stat.error 
halfMag 
sharksDetection 
SHARKSv20210222 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
sharksDetection 
SHARKSv20210421 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
ultravistaDetection 
ULTRAVISTADR4 
Calibrated magnitude within circular aperture halfRad, not available in SE output 
real 
4 
mag 

phot.mag 
halfMag 
vhsDetection 
VHSDR2 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vhsDetection 
VHSDR3 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vhsDetection 
VHSDR4 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vhsDetection 
VHSDR5 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vhsDetection 
VHSDR6 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vhsDetection 
VHSv20120926 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vhsDetection 
VHSv20130417 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vhsDetection 
VHSv20140409 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vhsDetection 
VHSv20150108 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vhsDetection 
VHSv20160114 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vhsDetection 
VHSv20160507 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vhsDetection 
VHSv20170630 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vhsDetection 
VHSv20180419 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vhsDetection 
VHSv20201209 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vhsDetection, vhsListRemeasurement 
VHSDR1 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
videoDetection 
VIDEODR2 
Calibrated magnitude within circular aperture halfRad, not available in SE output 
real 
4 
mag 

phot.mag 
halfMag 
videoDetection 
VIDEODR3 
Calibrated magnitude within circular aperture halfRad, not available in SE output 
real 
4 
mag 

phot.mag 
halfMag 
videoDetection 
VIDEODR4 
Calibrated magnitude within circular aperture halfRad, not available in SE output 
real 
4 
mag 

phot.mag 
halfMag 
videoDetection 
VIDEODR5 
Calibrated magnitude within circular aperture halfRad, not available in SE output 
real 
4 
mag 

phot.mag 
halfMag 
videoDetection 
VIDEOv20100513 
Calibrated magnitude within circular aperture halfRad, not available in SE output 
real 
4 
mag 

phot.mag 
halfMag 
videoDetection 
VIDEOv20111208 
Calibrated magnitude within circular aperture halfRad, not available in SE output 
real 
4 
mag 

phot.mag 
halfMag 
videoListRemeasurement 
VIDEOv20100513 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vikingDetection 
VIKINGDR2 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vikingDetection 
VIKINGDR3 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vikingDetection 
VIKINGDR4 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vikingDetection 
VIKINGv20111019 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vikingDetection 
VIKINGv20130417 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vikingDetection 
VIKINGv20140402 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vikingDetection 
VIKINGv20150421 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vikingDetection 
VIKINGv20151230 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vikingDetection 
VIKINGv20160406 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vikingDetection 
VIKINGv20161202 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vikingDetection 
VIKINGv20170715 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vikingDetection, vikingListRemeasurement 
VIKINGv20110714 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCDR1 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCDR2 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCDR3 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCDR4 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCDR5 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCv20110909 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCv20120126 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCv20121128 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCv20130304 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCv20130805 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCv20140428 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCv20140903 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCv20150309 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCv20151218 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCv20160311 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCv20160822 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCv20170109 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCv20170411 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCv20171101 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCv20180702 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCv20181120 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCv20191212 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCv20210708 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection 
VMCv20230816 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcDetection, vmcListRemeasurement 
VMCv20110816 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vmcdeepDetection 
VMCDEEPv20230713 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vvvDetection 
VVVDR1 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vvvDetection 
VVVDR2 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vvvDetection, vvvDetectionPawPrints, vvvDetectionTiles 
VVVDR5 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMag 
vvvDetection, vvvListRemeasurement 
VVVv20100531 
Calibrated magnitude within circular aperture halfRad 
real 
4 
mag 

phot.mag 
halfMagErr 
sharksDetection 
SHARKSv20210222 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
sharksDetection 
SHARKSv20210421 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
ultravistaDetection 
ULTRAVISTADR4 
Calibrated error on Half magnitude, not available in SE output 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vhsDetection 
VHSDR2 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vhsDetection 
VHSDR3 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vhsDetection 
VHSDR4 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vhsDetection 
VHSDR5 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vhsDetection 
VHSDR6 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vhsDetection 
VHSv20120926 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vhsDetection 
VHSv20130417 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vhsDetection 
VHSv20140409 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vhsDetection 
VHSv20150108 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vhsDetection 
VHSv20160114 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vhsDetection 
VHSv20160507 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vhsDetection 
VHSv20170630 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vhsDetection 
VHSv20180419 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vhsDetection 
VHSv20201209 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vhsDetection, vhsListRemeasurement 
VHSDR1 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
videoDetection 
VIDEODR2 
Calibrated error on Half magnitude, not available in SE output 
real 
4 
mag 

stat.error 
halfMagErr 
videoDetection 
VIDEODR3 
Calibrated error on Half magnitude, not available in SE output 
real 
4 
mag 

stat.error 
halfMagErr 
videoDetection 
VIDEODR4 
Calibrated error on Half magnitude, not available in SE output 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
videoDetection 
VIDEODR5 
Calibrated error on Half magnitude, not available in SE output 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
videoDetection 
VIDEOv20100513 
Calibrated error on Half magnitude, not available in SE output 
real 
4 
mag 

stat.error 
halfMagErr 
videoDetection 
VIDEOv20111208 
Calibrated error on Half magnitude, not available in SE output 
real 
4 
mag 

stat.error 
halfMagErr 
videoListRemeasurement 
VIDEOv20100513 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vikingDetection 
VIKINGDR2 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vikingDetection 
VIKINGDR3 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vikingDetection 
VIKINGDR4 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vikingDetection 
VIKINGv20111019 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vikingDetection 
VIKINGv20130417 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vikingDetection 
VIKINGv20140402 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vikingDetection 
VIKINGv20150421 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vikingDetection 
VIKINGv20151230 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vikingDetection 
VIKINGv20160406 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vikingDetection 
VIKINGv20161202 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vikingDetection 
VIKINGv20170715 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vikingDetection, vikingListRemeasurement 
VIKINGv20110714 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vmcDetection 
VMCDR1 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vmcDetection 
VMCDR2 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vmcDetection 
VMCDR3 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vmcDetection 
VMCDR4 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vmcDetection 
VMCDR5 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vmcDetection 
VMCv20110909 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vmcDetection 
VMCv20120126 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vmcDetection 
VMCv20121128 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vmcDetection 
VMCv20130304 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vmcDetection 
VMCv20130805 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vmcDetection 
VMCv20140428 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vmcDetection 
VMCv20140903 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vmcDetection 
VMCv20150309 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vmcDetection 
VMCv20151218 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vmcDetection 
VMCv20160311 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vmcDetection 
VMCv20160822 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vmcDetection 
VMCv20170109 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vmcDetection 
VMCv20170411 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vmcDetection 
VMCv20171101 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vmcDetection 
VMCv20180702 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vmcDetection 
VMCv20181120 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vmcDetection 
VMCv20191212 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vmcDetection 
VMCv20210708 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vmcDetection 
VMCv20230816 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vmcDetection, vmcListRemeasurement 
VMCv20110816 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vmcdeepDetection 
VMCDEEPv20230713 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vvvDetection 
VVVDR1 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vvvDetection 
VVVDR2 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfMagErr 
vvvDetection, vvvDetectionPawPrints, vvvDetectionTiles 
VVVDR5 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error;phot.mag 
halfMagErr 
vvvDetection, vvvListRemeasurement 
VVVv20100531 
Calibrated error on Half magnitude 
real 
4 
mag 

stat.error 
halfRad 
sharksDetection 
SHARKSv20210222 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
sharksDetection 
SHARKSv20210421 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
ultravistaDetection 
ULTRAVISTADR4 
SExtractor halflight radius (FRAC_RADIUS), calcuated assuming Kron flux is total flux {catalogue TType keyword: Half_radius} 
real 
4 
pixels 

phys.angSize 
halfRad 
ultravistaMapRemeasurement 
ULTRAVISTADR4 
Halflight radius (SE: FRAC_RADIUS, calcuated assuming Kron flux is total flux; CASU: default) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 

phys.angSize 
halfRad 
vhsDetection 
VHSDR2 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize;src 
halfRad 
vhsDetection 
VHSDR3 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vhsDetection 
VHSDR4 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vhsDetection 
VHSDR5 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vhsDetection 
VHSDR6 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vhsDetection 
VHSv20120926 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vhsDetection 
VHSv20130417 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vhsDetection 
VHSv20140409 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vhsDetection 
VHSv20150108 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vhsDetection 
VHSv20160114 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vhsDetection 
VHSv20160507 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vhsDetection 
VHSv20170630 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vhsDetection 
VHSv20180419 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vhsDetection 
VHSv20201209 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vhsDetection, vhsListRemeasurement 
VHSDR1 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize;src 
halfRad 
videoDetection 
VIDEODR2 
SExtractor halflight radius (FRAC_RADIUS), calcuated assuming Kron flux is total flux {catalogue TType keyword: Half_radius} 
real 
4 
pixels 

phys.angSize;src 
halfRad 
videoDetection 
VIDEODR3 
SExtractor halflight radius (FRAC_RADIUS), calcuated assuming Kron flux is total flux {catalogue TType keyword: Half_radius} 
real 
4 
pixels 

phys.angSize 
halfRad 
videoDetection 
VIDEODR4 
SExtractor halflight radius (FRAC_RADIUS), calcuated assuming Kron flux is total flux {catalogue TType keyword: Half_radius} 
real 
4 
pixels 

phys.angSize 
halfRad 
videoDetection 
VIDEODR5 
SExtractor halflight radius (FRAC_RADIUS), calcuated assuming Kron flux is total flux {catalogue TType keyword: Half_radius} 
real 
4 
pixels 

phys.angSize 
halfRad 
videoDetection 
VIDEOv20100513 
SExtractor halflight radius (FRAC_RADIUS), calcuated assuming Kron flux is total flux {catalogue TType keyword: Half_radius} 
real 
4 
pixels 

phys.angSize;src 
halfRad 
videoDetection 
VIDEOv20111208 
SExtractor halflight radius (FRAC_RADIUS), calcuated assuming Kron flux is total flux {catalogue TType keyword: Half_radius} 
real 
4 
pixels 

phys.angSize;src 
halfRad 
videoListRemeasurement 
VIDEOv20100513 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize;src 
halfRad 
vikingDetection 
VIKINGDR2 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize;src 
halfRad 
vikingDetection 
VIKINGDR3 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vikingDetection 
VIKINGDR4 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vikingDetection 
VIKINGv20111019 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize;src 
halfRad 
vikingDetection 
VIKINGv20130417 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vikingDetection 
VIKINGv20140402 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vikingDetection 
VIKINGv20150421 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vikingDetection 
VIKINGv20151230 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vikingDetection 
VIKINGv20160406 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vikingDetection 
VIKINGv20161202 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vikingDetection 
VIKINGv20170715 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vikingDetection, vikingListRemeasurement 
VIKINGv20110714 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize;src 
halfRad 
vikingMapRemeasurement 
VIKINGZYSELJv20160909 
Halflight radius (SE: FRAC_RADIUS, calcuated assuming Kron flux is total flux; CASU: default) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 

phys.angSize 
halfRad 
vikingMapRemeasurement 
VIKINGZYSELJv20170124 
Halflight radius (SE: FRAC_RADIUS, calcuated assuming Kron flux is total flux; CASU: default) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 

phys.angSize 
halfRad 
vmcDetection 
VMCDR1 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize;src 
halfRad 
vmcDetection 
VMCDR2 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vmcDetection 
VMCDR3 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vmcDetection 
VMCDR4 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vmcDetection 
VMCDR5 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vmcDetection 
VMCv20110909 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize;src 
halfRad 
vmcDetection 
VMCv20120126 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize;src 
halfRad 
vmcDetection 
VMCv20121128 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vmcDetection 
VMCv20130304 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vmcDetection 
VMCv20130805 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vmcDetection 
VMCv20140428 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vmcDetection 
VMCv20140903 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vmcDetection 
VMCv20150309 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vmcDetection 
VMCv20151218 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vmcDetection 
VMCv20160311 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vmcDetection 
VMCv20160822 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vmcDetection 
VMCv20170109 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vmcDetection 
VMCv20170411 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vmcDetection 
VMCv20171101 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vmcDetection 
VMCv20180702 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vmcDetection 
VMCv20181120 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vmcDetection 
VMCv20191212 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vmcDetection 
VMCv20210708 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vmcDetection 
VMCv20230816 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vmcDetection, vmcListRemeasurement 
VMCv20110816 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize;src 
halfRad 
vmcdeepDetection 
VMCDEEPv20230713 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vvvDetection 
VVVDR1 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vvvDetection 
VVVDR2 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vvvDetection, vvvDetectionPawPrints, vvvDetectionTiles 
VVVDR5 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize 
halfRad 
vvvDetection, vvvListRemeasurement 
VVVv20100531 
r_h halflight radius, calculated as the circular aperture that encloses half the total flux, which is specified as max(isoFlux,aperFlux5) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 
0.9999995e9 
phys.angSize;src 
hAperJky3 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Default point source H aperture corrected (2.0 arcsec aperture diameter) calibrated flux If in doubt use this flux estimator 
real 
4 
jansky 
0.9999995e9 
phot.flux 
hAperJky3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Default point source H aperture corrected (2.0 arcsec aperture diameter) calibrated flux If in doubt use this flux estimator 
real 
4 
jansky 
0.9999995e9 
phot.flux 
hAperJky3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Default point source H aperture corrected (2.0 arcsec aperture diameter) calibrated flux If in doubt use this flux estimator 
real 
4 
jansky 
0.9999995e9 
phot.flux 
hAperJky3Err 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Error in default point/extended source H (2.0 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
stat.error 
hAperJky3Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Error in default point/extended source H (2.0 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
stat.error 
hAperJky3Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Error in default point/extended source H (2.0 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
stat.error 
hAperJky4 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Point source H aperture corrected (2.8 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
hAperJky4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Point source H aperture corrected (2.8 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
hAperJky4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Point source H aperture corrected (2.8 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
hAperJky4Err 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Error in point/extended source H (2.8 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
stat.error 
hAperJky4Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Error in point/extended source H (2.8 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
stat.error 
hAperJky4Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Error in point/extended source H (2.8 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
stat.error 
hAperJky6 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Point source H aperture corrected (5.7 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
hAperJky6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Point source H aperture corrected (5.7 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
hAperJky6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Point source H aperture corrected (5.7 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
hAperJky6Err 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Error in point/extended source H (5.7 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
stat.error 
hAperJky6Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Error in point/extended source H (5.7 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
stat.error 
hAperJky6Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Error in point/extended source H (5.7 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
stat.error 
hAperJkyNoAperCorr3 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Default extended source H (2.0 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux If in doubt use this flux estimator 
real 
4 
jansky 
0.9999995e9 
phot.flux 
hAperJkyNoAperCorr3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Default extended source H (2.0 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux If in doubt use this flux estimator 
real 
4 
jansky 
0.9999995e9 
phot.flux 
hAperJkyNoAperCorr3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Default extended source H (2.0 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux If in doubt use this flux estimator 
real 
4 
jansky 
0.9999995e9 
phot.flux 
hAperJkyNoAperCorr4 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Extended source H (2.8 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
hAperJkyNoAperCorr4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Extended source H (2.8 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
hAperJkyNoAperCorr4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Extended source H (2.8 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
hAperJkyNoAperCorr6 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Extended source H (5.7 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
hAperJkyNoAperCorr6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Extended source H (5.7 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
hAperJkyNoAperCorr6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Extended source H (5.7 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
hAperLup3 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Default point source H aperture corrected (2.0 arcsec aperture diameter) luptitude If in doubt use this flux estimator 
real 
4 
lup 
0.9999995e9 
phot.lup 
hAperLup3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Default point source H aperture corrected (2.0 arcsec aperture diameter) luptitude If in doubt use this flux estimator 
real 
4 
lup 
0.9999995e9 
phot.lup 
hAperLup3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Default point source H aperture corrected (2.0 arcsec aperture diameter) luptitude If in doubt use this flux estimator 
real 
4 
lup 
0.9999995e9 
phot.lup 
hAperLup3Err 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Error in default point/extended source H (2.0 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
stat.error 
hAperLup3Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Error in default point/extended source H (2.0 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
stat.error 
hAperLup3Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Error in default point/extended source H (2.0 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
stat.error 
hAperLup4 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Point source H aperture corrected (2.8 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
hAperLup4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Point source H aperture corrected (2.8 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
hAperLup4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Point source H aperture corrected (2.8 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
hAperLup4Err 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Error in point/extended source H (2.8 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
stat.error 
hAperLup4Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Error in point/extended source H (2.8 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
stat.error 
hAperLup4Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Error in point/extended source H (2.8 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
stat.error 
hAperLup6 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Point source H aperture corrected (5.7 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
hAperLup6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Point source H aperture corrected (5.7 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
hAperLup6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Point source H aperture corrected (5.7 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
hAperLup6Err 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Error in point/extended source H (5.7 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
stat.error 
hAperLup6Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Error in point/extended source H (5.7 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
stat.error 
hAperLup6Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Error in point/extended source H (5.7 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
stat.error 
hAperLupNoAperCorr3 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Default extended source H (2.0 arcsec aperture diameter, but no aperture correction applied) aperture luptitude If in doubt use this flux estimator 
real 
4 
lup 
0.9999995e9 
phot.lup 
hAperLupNoAperCorr3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Default extended source H (2.0 arcsec aperture diameter, but no aperture correction applied) aperture luptitude If in doubt use this flux estimator 
real 
4 
lup 
0.9999995e9 
phot.lup 
hAperLupNoAperCorr3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Default extended source H (2.0 arcsec aperture diameter, but no aperture correction applied) aperture luptitude If in doubt use this flux estimator 
real 
4 
lup 
0.9999995e9 
phot.lup 
hAperLupNoAperCorr4 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Extended source H (2.8 arcsec aperture diameter, but no aperture correction applied) aperture luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
hAperLupNoAperCorr4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Extended source H (2.8 arcsec aperture diameter, but no aperture correction applied) aperture luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
hAperLupNoAperCorr4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Extended source H (2.8 arcsec aperture diameter, but no aperture correction applied) aperture luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
hAperLupNoAperCorr6 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Extended source H (5.7 arcsec aperture diameter, but no aperture correction applied) aperture luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
hAperLupNoAperCorr6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Extended source H (5.7 arcsec aperture diameter, but no aperture correction applied) aperture luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
hAperLupNoAperCorr6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Extended source H (5.7 arcsec aperture diameter, but no aperture correction applied) aperture luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
hAperMag1 
vvvSource 
VVVDR1 
Extended source H aperture corrected mag (0.7 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag1 
vvvSource 
VVVDR5 
Point source H aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag1 
vvvSource 
VVVv20100531 
Extended source H aperture corrected mag (0.7 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag1 
vvvSource 
VVVv20110718 
Extended source H aperture corrected mag (0.7 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag1 
vvvSource, vvvSynopticSource 
VVVDR2 
Extended source H aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag1Err 
vvvSource 
VVVDR1 
Error in extended source H mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag1Err 
vvvSource 
VVVDR5 
Error in point source H mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag1Err 
vvvSource 
VVVv20100531 
Error in extended source H mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag1Err 
vvvSource 
VVVv20110718 
Error in extended source H mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag1Err 
vvvSource, vvvSynopticSource 
VVVDR2 
Error in extended source H mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag2 
vvvSynopticSource 
VVVDR1 
Extended source H aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag2 
vvvSynopticSource 
VVVDR2 
Extended source H aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag2Err 
vvvSynopticSource 
VVVDR1 
Error in extended source H mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag2Err 
vvvSynopticSource 
VVVDR2 
Error in extended source H mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3 
ultravistaSource 
ULTRAVISTADR4 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag3 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Default point source H aperture corrected (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
vhsSource 
VHSDR1 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
vhsSource 
VHSDR2 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
vhsSource 
VHSDR3 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag3 
vhsSource 
VHSDR4 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag3 
vhsSource 
VHSDR5 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag3 
vhsSource 
VHSDR6 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag3 
vhsSource 
VHSv20120926 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
vhsSource 
VHSv20130417 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
vhsSource 
VHSv20140409 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag3 
vhsSource 
VHSv20150108 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag3 
vhsSource 
VHSv20160114 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag3 
vhsSource 
VHSv20160507 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag3 
vhsSource 
VHSv20170630 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag3 
vhsSource 
VHSv20180419 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag3 
vhsSource 
VHSv20201209 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag3 
videoSource 
VIDEODR2 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
videoSource 
VIDEODR3 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
videoSource 
VIDEODR4 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag3 
videoSource 
VIDEODR5 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag3 
videoSource 
VIDEOv20100513 
Default point/extended source H mag, no aperture correction applied If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
videoSource 
VIDEOv20111208 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
vikingSource 
VIKINGDR2 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
vikingSource 
VIKINGDR3 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
vikingSource 
VIKINGDR4 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag3 
vikingSource 
VIKINGv20110714 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
vikingSource 
VIKINGv20111019 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
vikingSource 
VIKINGv20130417 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
vikingSource 
VIKINGv20140402 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag3 
vikingSource 
VIKINGv20150421 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag3 
vikingSource 
VIKINGv20151230 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag3 
vikingSource 
VIKINGv20160406 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag3 
vikingSource 
VIKINGv20161202 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag3 
vikingSource 
VIKINGv20170715 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Default point source H aperture corrected (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Default point source H aperture corrected (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
vvvSource 
VVVDR1 
Default point/extended source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
vvvSource 
VVVDR2 
Default point/extended source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag3 
vvvSource 
VVVDR5 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag3 
vvvSource 
VVVv20100531 
Default point/extended source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
vvvSource 
VVVv20110718 
Default point/extended source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
vvvSynopticSource 
VVVDR1 
Default point/extended source H aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag3 
vvvSynopticSource 
VVVDR2 
Default point/extended source H aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag3 
vvvVivaCatalogue 
VVVDR5 
H magnitude using aperture corrected mag (2.0 arcsec aperture diameter, from VVVDR4 1st epoch JHKs contemporaneous OB) {catalogue TType keyword: hAperMag3} 
real 
4 
mag 
9.999995e8 

hAperMag3Err 
ultravistaSource 
ULTRAVISTADR4 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag3Err 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Error in default point/extended source H (2.0 arcsec aperture diameter) magnitude 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
vhsSource 
VHSDR1 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
vhsSource 
VHSDR2 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
vhsSource 
VHSDR3 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
hAperMag3Err 
vhsSource 
VHSDR4 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;phot.mag 
hAperMag3Err 
vhsSource 
VHSDR5 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag3Err 
vhsSource 
VHSDR6 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag3Err 
vhsSource 
VHSv20120926 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
vhsSource 
VHSv20130417 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
vhsSource 
VHSv20140409 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
hAperMag3Err 
vhsSource 
VHSv20150108 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;phot.mag 
hAperMag3Err 
vhsSource 
VHSv20160114 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag3Err 
vhsSource 
VHSv20160507 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag3Err 
vhsSource 
VHSv20170630 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag3Err 
vhsSource 
VHSv20180419 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag3Err 
vhsSource 
VHSv20201209 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag3Err 
videoSource 
VIDEODR2 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
videoSource 
VIDEODR3 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
videoSource 
VIDEODR4 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;phot.mag 
hAperMag3Err 
videoSource 
VIDEODR5 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;phot.mag 
hAperMag3Err 
videoSource 
VIDEOv20100513 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
videoSource 
VIDEOv20111208 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
vikingSource 
VIKINGDR2 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
vikingSource 
VIKINGDR3 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
vikingSource 
VIKINGDR4 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
hAperMag3Err 
vikingSource 
VIKINGv20110714 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
vikingSource 
VIKINGv20111019 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
vikingSource 
VIKINGv20130417 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
vikingSource 
VIKINGv20140402 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
vikingSource 
VIKINGv20150421 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;phot.mag 
hAperMag3Err 
vikingSource 
VIKINGv20151230 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag3Err 
vikingSource 
VIKINGv20160406 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag3Err 
vikingSource 
VIKINGv20161202 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag3Err 
vikingSource 
VIKINGv20170715 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag3Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Error in default point/extended source H (2.0 arcsec aperture diameter) magnitude 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Error in default point/extended source H (2.0 arcsec aperture diameter) magnitude 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
vvvSource 
VVVDR2 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
vvvSource 
VVVDR5 
Error in default point source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag3Err 
vvvSource 
VVVv20100531 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
vvvSource 
VVVv20110718 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
vvvSource, vvvSynopticSource 
VVVDR1 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag3Err 
vvvVivaCatalogue 
VVVDR5 
Error in default point source H mag, from VVVDR4 {catalogue TType keyword: hAperMag3Err} 
real 
4 
mag 
9.999995e8 

hAperMag4 
ultravistaSource 
ULTRAVISTADR4 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag4 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Point source H aperture corrected (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
vhsSource 
VHSDR1 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
vhsSource 
VHSDR2 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
vhsSource 
VHSDR3 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag4 
vhsSource 
VHSDR4 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag4 
vhsSource 
VHSDR5 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag4 
vhsSource 
VHSDR6 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag4 
vhsSource 
VHSv20120926 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
vhsSource 
VHSv20130417 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
vhsSource 
VHSv20140409 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag4 
vhsSource 
VHSv20150108 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag4 
vhsSource 
VHSv20160114 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag4 
vhsSource 
VHSv20160507 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag4 
vhsSource 
VHSv20170630 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag4 
vhsSource 
VHSv20180419 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag4 
vhsSource 
VHSv20201209 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag4 
videoSource 
VIDEODR2 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
videoSource 
VIDEODR3 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
videoSource 
VIDEODR4 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag4 
videoSource 
VIDEODR5 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag4 
videoSource 
VIDEOv20100513 
Extended source H mag, no aperture correction applied 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
videoSource 
VIDEOv20111208 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
vikingSource 
VIKINGDR2 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
vikingSource 
VIKINGDR3 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
vikingSource 
VIKINGDR4 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag4 
vikingSource 
VIKINGv20110714 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
vikingSource 
VIKINGv20111019 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
vikingSource 
VIKINGv20130417 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
vikingSource 
VIKINGv20140402 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag4 
vikingSource 
VIKINGv20150421 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag4 
vikingSource 
VIKINGv20151230 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag4 
vikingSource 
VIKINGv20160406 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag4 
vikingSource 
VIKINGv20161202 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag4 
vikingSource 
VIKINGv20170715 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Point source H aperture corrected (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Point source H aperture corrected (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
vvvSource 
VVVDR2 
Extended source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag4 
vvvSource 
VVVDR5 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag4 
vvvSource 
VVVv20100531 
Extended source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
vvvSource 
VVVv20110718 
Extended source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4 
vvvSource, vvvSynopticSource 
VVVDR1 
Extended source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag4Err 
ultravistaSource 
ULTRAVISTADR4 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag4Err 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Error in point/extended source H (2.8 arcsec aperture diameter) magnitude 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
vhsSource 
VHSDR1 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
vhsSource 
VHSDR2 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
vhsSource 
VHSDR3 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
hAperMag4Err 
vhsSource 
VHSDR4 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;phot.mag 
hAperMag4Err 
vhsSource 
VHSDR5 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag4Err 
vhsSource 
VHSDR6 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag4Err 
vhsSource 
VHSv20120926 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
vhsSource 
VHSv20130417 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
vhsSource 
VHSv20140409 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
hAperMag4Err 
vhsSource 
VHSv20150108 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;phot.mag 
hAperMag4Err 
vhsSource 
VHSv20160114 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag4Err 
vhsSource 
VHSv20160507 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag4Err 
vhsSource 
VHSv20170630 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag4Err 
vhsSource 
VHSv20180419 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag4Err 
vhsSource 
VHSv20201209 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag4Err 
videoSource 
VIDEODR2 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
videoSource 
VIDEODR3 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
videoSource 
VIDEODR4 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;phot.mag 
hAperMag4Err 
videoSource 
VIDEODR5 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;phot.mag 
hAperMag4Err 
videoSource 
VIDEOv20100513 
Error in extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
videoSource 
VIDEOv20111208 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
vikingSource 
VIKINGDR2 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
vikingSource 
VIKINGDR3 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
vikingSource 
VIKINGDR4 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
hAperMag4Err 
vikingSource 
VIKINGv20110714 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
vikingSource 
VIKINGv20111019 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
vikingSource 
VIKINGv20130417 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
vikingSource 
VIKINGv20140402 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
vikingSource 
VIKINGv20150421 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;phot.mag 
hAperMag4Err 
vikingSource 
VIKINGv20151230 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag4Err 
vikingSource 
VIKINGv20160406 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag4Err 
vikingSource 
VIKINGv20161202 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag4Err 
vikingSource 
VIKINGv20170715 
Error in point/extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag4Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Error in point/extended source H (2.8 arcsec aperture diameter) magnitude 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Error in point/extended source H (2.8 arcsec aperture diameter) magnitude 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
vvvSource 
VVVDR2 
Error in extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
vvvSource 
VVVDR5 
Error in point source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag4Err 
vvvSource 
VVVv20100531 
Error in extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
vvvSource 
VVVv20110718 
Error in extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag4Err 
vvvSource, vvvSynopticSource 
VVVDR1 
Error in extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag5 
vvvSynopticSource 
VVVDR1 
Extended source H aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag5 
vvvSynopticSource 
VVVDR2 
Extended source H aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag5Err 
vvvSynopticSource 
VVVDR1 
Error in extended source H mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag5Err 
vvvSynopticSource 
VVVDR2 
Error in extended source H mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6 
ultravistaSource 
ULTRAVISTADR4 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag6 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Point source H aperture corrected (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag6 
vhsSource 
VHSDR1 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag6 
vhsSource 
VHSDR2 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag6 
vhsSource 
VHSDR3 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag6 
vhsSource 
VHSDR4 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag6 
vhsSource 
VHSDR5 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag6 
vhsSource 
VHSDR6 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag6 
vhsSource 
VHSv20120926 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag6 
vhsSource 
VHSv20130417 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag6 
vhsSource 
VHSv20140409 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag6 
vhsSource 
VHSv20150108 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag6 
vhsSource 
VHSv20160114 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag6 
vhsSource 
VHSv20160507 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag6 
vhsSource 
VHSv20170630 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag6 
vhsSource 
VHSv20180419 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag6 
vhsSource 
VHSv20201209 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag6 
videoSource 
VIDEODR2 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag6 
videoSource 
VIDEODR3 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag6 
videoSource 
VIDEODR4 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag6 
videoSource 
VIDEODR5 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag6 
videoSource 
VIDEOv20100513 
Extended source H mag, no aperture correction applied 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag6 
videoSource 
VIDEOv20111208 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag6 
vikingSource 
VIKINGDR2 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag6 
vikingSource 
VIKINGDR3 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag6 
vikingSource 
VIKINGDR4 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag6 
vikingSource 
VIKINGv20110714 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag6 
vikingSource 
VIKINGv20111019 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag6 
vikingSource 
VIKINGv20130417 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag6 
vikingSource 
VIKINGv20140402 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag6 
vikingSource 
VIKINGv20150421 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag6 
vikingSource 
VIKINGv20151230 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag6 
vikingSource 
VIKINGv20160406 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag6 
vikingSource 
VIKINGv20161202 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag6 
vikingSource 
VIKINGv20170715 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMag6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Point source H aperture corrected (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Point source H aperture corrected (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMag6Err 
ultravistaSource 
ULTRAVISTADR4 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag6Err 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Error in point/extended source H (5.7 arcsec aperture diameter) magnitude 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6Err 
vhsSource 
VHSDR1 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6Err 
vhsSource 
VHSDR2 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6Err 
vhsSource 
VHSDR3 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
hAperMag6Err 
vhsSource 
VHSDR4 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;phot.mag 
hAperMag6Err 
vhsSource 
VHSDR5 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag6Err 
vhsSource 
VHSDR6 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag6Err 
vhsSource 
VHSv20120926 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6Err 
vhsSource 
VHSv20130417 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6Err 
vhsSource 
VHSv20140409 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
hAperMag6Err 
vhsSource 
VHSv20150108 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;phot.mag 
hAperMag6Err 
vhsSource 
VHSv20160114 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag6Err 
vhsSource 
VHSv20160507 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag6Err 
vhsSource 
VHSv20170630 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag6Err 
vhsSource 
VHSv20180419 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag6Err 
vhsSource 
VHSv20201209 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag6Err 
videoSource 
VIDEODR2 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6Err 
videoSource 
VIDEODR3 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6Err 
videoSource 
VIDEODR4 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;phot.mag 
hAperMag6Err 
videoSource 
VIDEODR5 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;phot.mag 
hAperMag6Err 
videoSource 
VIDEOv20100513 
Error in extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6Err 
videoSource 
VIDEOv20111208 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6Err 
vikingSource 
VIKINGDR2 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6Err 
vikingSource 
VIKINGDR3 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6Err 
vikingSource 
VIKINGDR4 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
hAperMag6Err 
vikingSource 
VIKINGv20110714 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6Err 
vikingSource 
VIKINGv20111019 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6Err 
vikingSource 
VIKINGv20130417 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6Err 
vikingSource 
VIKINGv20140402 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6Err 
vikingSource 
VIKINGv20150421 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;phot.mag 
hAperMag6Err 
vikingSource 
VIKINGv20151230 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag6Err 
vikingSource 
VIKINGv20160406 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag6Err 
vikingSource 
VIKINGv20161202 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag6Err 
vikingSource 
VIKINGv20170715 
Error in point/extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hAperMag6Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Error in point/extended source H (5.7 arcsec aperture diameter) magnitude 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMag6Err 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Error in point/extended source H (5.7 arcsec aperture diameter) magnitude 
real 
4 
mag 
0.9999995e9 
stat.error 
hAperMagNoAperCorr3 
ultravistaSource 
ULTRAVISTADR4 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr3 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Default extended source H (2.0 arcsec aperture diameter, but no aperture correction applied) aperture magnitude If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr3 
vhsSource 
VHSDR1 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr3 
vhsSource 
VHSDR2 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr3 
vhsSource 
VHSDR3 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr3 
vhsSource 
VHSDR4 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr3 
vhsSource 
VHSDR5 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr3 
vhsSource 
VHSDR6 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr3 
vhsSource 
VHSv20120926 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr3 
vhsSource 
VHSv20130417 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr3 
vhsSource 
VHSv20140409 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr3 
vhsSource 
VHSv20150108 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr3 
vhsSource 
VHSv20160114 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr3 
vhsSource 
VHSv20160507 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr3 
vhsSource 
VHSv20170630 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr3 
vhsSource 
VHSv20180419 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr3 
vhsSource 
VHSv20201209 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr3 
videoSource 
VIDEODR2 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr3 
videoSource 
VIDEODR3 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr3 
videoSource 
VIDEODR4 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr3 
videoSource 
VIDEODR5 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr3 
videoSource 
VIDEOv20111208 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr3 
vikingSource 
VIKINGDR2 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr3 
vikingSource 
VIKINGDR3 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr3 
vikingSource 
VIKINGDR4 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr3 
vikingSource 
VIKINGv20110714 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr3 
vikingSource 
VIKINGv20111019 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr3 
vikingSource 
VIKINGv20130417 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr3 
vikingSource 
VIKINGv20140402 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr3 
vikingSource 
VIKINGv20150421 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr3 
vikingSource 
VIKINGv20151230 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr3 
vikingSource 
VIKINGv20160406 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr3 
vikingSource 
VIKINGv20161202 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr3 
vikingSource 
VIKINGv20170715 
Default extended source H aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Default extended source H (2.0 arcsec aperture diameter, but no aperture correction applied) aperture magnitude If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr3 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Default extended source H (2.0 arcsec aperture diameter, but no aperture correction applied) aperture magnitude If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr4 
ultravistaSource 
ULTRAVISTADR4 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr4 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Extended source H (2.8 arcsec aperture diameter, but no aperture correction applied) aperture magnitude 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr4 
vhsSource 
VHSDR1 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr4 
vhsSource 
VHSDR2 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr4 
vhsSource 
VHSDR3 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr4 
vhsSource 
VHSDR4 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr4 
vhsSource 
VHSDR5 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr4 
vhsSource 
VHSDR6 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr4 
vhsSource 
VHSv20120926 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr4 
vhsSource 
VHSv20130417 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr4 
vhsSource 
VHSv20140409 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr4 
vhsSource 
VHSv20150108 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr4 
vhsSource 
VHSv20160114 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr4 
vhsSource 
VHSv20160507 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr4 
vhsSource 
VHSv20170630 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr4 
vhsSource 
VHSv20180419 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr4 
vhsSource 
VHSv20201209 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr4 
videoSource 
VIDEODR2 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr4 
videoSource 
VIDEODR3 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr4 
videoSource 
VIDEODR4 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr4 
videoSource 
VIDEODR5 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr4 
videoSource 
VIDEOv20111208 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr4 
vikingSource 
VIKINGDR2 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr4 
vikingSource 
VIKINGDR3 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr4 
vikingSource 
VIKINGDR4 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr4 
vikingSource 
VIKINGv20110714 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr4 
vikingSource 
VIKINGv20111019 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr4 
vikingSource 
VIKINGv20130417 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr4 
vikingSource 
VIKINGv20140402 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr4 
vikingSource 
VIKINGv20150421 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr4 
vikingSource 
VIKINGv20151230 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr4 
vikingSource 
VIKINGv20160406 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr4 
vikingSource 
VIKINGv20161202 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr4 
vikingSource 
VIKINGv20170715 
Extended source H aperture mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Extended source H (2.8 arcsec aperture diameter, but no aperture correction applied) aperture magnitude 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr4 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Extended source H (2.8 arcsec aperture diameter, but no aperture correction applied) aperture magnitude 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr6 
ultravistaSource 
ULTRAVISTADR4 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr6 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Extended source H (5.7 arcsec aperture diameter, but no aperture correction applied) aperture magnitude 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr6 
vhsSource 
VHSDR1 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr6 
vhsSource 
VHSDR2 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr6 
vhsSource 
VHSDR3 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr6 
vhsSource 
VHSDR4 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr6 
vhsSource 
VHSDR5 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr6 
vhsSource 
VHSDR6 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr6 
vhsSource 
VHSv20120926 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr6 
vhsSource 
VHSv20130417 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr6 
vhsSource 
VHSv20140409 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr6 
vhsSource 
VHSv20150108 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr6 
vhsSource 
VHSv20160114 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr6 
vhsSource 
VHSv20160507 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr6 
vhsSource 
VHSv20170630 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr6 
vhsSource 
VHSv20180419 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr6 
vhsSource 
VHSv20201209 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr6 
videoSource 
VIDEODR2 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr6 
videoSource 
VIDEODR3 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr6 
videoSource 
VIDEODR4 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr6 
videoSource 
VIDEODR5 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr6 
videoSource 
VIDEOv20111208 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr6 
vikingSource 
VIKINGDR2 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr6 
vikingSource 
VIKINGDR3 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr6 
vikingSource 
VIKINGDR4 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr6 
vikingSource 
VIKINGv20110714 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr6 
vikingSource 
VIKINGv20111019 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr6 
vikingSource 
VIKINGv20130417 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr6 
vikingSource 
VIKINGv20140402 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr6 
vikingSource 
VIKINGv20150421 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr6 
vikingSource 
VIKINGv20151230 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr6 
vikingSource 
VIKINGv20160406 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr6 
vikingSource 
VIKINGv20161202 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr6 
vikingSource 
VIKINGv20170715 
Extended source H aperture mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hAperMagNoAperCorr6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Extended source H (5.7 arcsec aperture diameter, but no aperture correction applied) aperture magnitude 
real 
4 
mag 
0.9999995e9 
phot.mag 
hAperMagNoAperCorr6 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Extended source H (5.7 arcsec aperture diameter, but no aperture correction applied) aperture magnitude 
real 
4 
mag 
0.9999995e9 
phot.mag 
haStratAst 
ultravistaVarFrameSetInfo 
ULTRAVISTADR4 
Parameter, c0 from FerreiraLopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in H band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
haStratAst 
videoVarFrameSetInfo 
VIDEODR2 
Strateva parameter, a, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
haStratAst 
videoVarFrameSetInfo 
VIDEODR3 
Strateva parameter, a, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
haStratAst 
videoVarFrameSetInfo 
VIDEODR4 
Strateva parameter, a, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
haStratAst 
videoVarFrameSetInfo 
VIDEODR5 
Strateva parameter, a, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
haStratAst 
videoVarFrameSetInfo 
VIDEOv20100513 
Strateva parameter, a, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
haStratAst 
videoVarFrameSetInfo 
VIDEOv20111208 
Strateva parameter, a, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
haStratAst 
vikingVarFrameSetInfo 
VIKINGDR2 
Strateva parameter, a, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
haStratAst 
vikingVarFrameSetInfo 
VIKINGv20110714 
Strateva parameter, a, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
haStratAst 
vikingVarFrameSetInfo 
VIKINGv20111019 
Strateva parameter, a, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
haStratAst 
vvvVarFrameSetInfo 
VVVDR5 
Parameter, c0 from FerreiraLopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in H band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
haStratAst 
vvvVarFrameSetInfo 
VVVv20100531 
Strateva parameter, a, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
haStratPht 
ultravistaMapLcVarFrameSetInfo 
ULTRAVISTADR4 
Strateva parameter, a, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
haStratPht 
ultravistaVarFrameSetInfo 
ULTRAVISTADR4 
Parameter, c0 from FerreiraLopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in H band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
haStratPht 
videoVarFrameSetInfo 
VIDEODR2 
Strateva parameter, a, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
haStratPht 
videoVarFrameSetInfo 
VIDEODR3 
Strateva parameter, a, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
haStratPht 
videoVarFrameSetInfo 
VIDEODR4 
Strateva parameter, a, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
haStratPht 
videoVarFrameSetInfo 
VIDEODR5 
Strateva parameter, a, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
haStratPht 
videoVarFrameSetInfo 
VIDEOv20100513 
Strateva parameter, a, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
haStratPht 
videoVarFrameSetInfo 
VIDEOv20111208 
Strateva parameter, a, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
haStratPht 
vikingVarFrameSetInfo 
VIKINGDR2 
Strateva parameter, a, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
haStratPht 
vikingVarFrameSetInfo 
VIKINGv20110714 
Strateva parameter, a, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
haStratPht 
vikingVarFrameSetInfo 
VIKINGv20111019 
Strateva parameter, a, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
haStratPht 
vvvVarFrameSetInfo 
VVVDR5 
Parameter, c0 from FerreiraLopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in H band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
haStratPht 
vvvVarFrameSetInfo 
VVVv20100531 
Strateva parameter, a, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hAverageConf 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.NIR 
hAverageConf 
vhsSource 
VHSDR1 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

99999999 
meta.code 
hAverageConf 
vhsSource 
VHSDR2 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

99999999 
meta.code 
hAverageConf 
vhsSource 
VHSDR3 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.H 
hAverageConf 
vhsSource 
VHSDR4 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.H 
hAverageConf 
vhsSource 
VHSDR5 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.H 
hAverageConf 
vhsSource 
VHSDR6 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.H 
hAverageConf 
vhsSource 
VHSv20120926 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

99999999 
stat.likelihood;em.IR.NIR 
hAverageConf 
vhsSource 
VHSv20130417 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.NIR 
hAverageConf 
vhsSource 
VHSv20140409 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.H 
hAverageConf 
vhsSource 
VHSv20150108 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.H 
hAverageConf 
vhsSource 
VHSv20160114 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.H 
hAverageConf 
vhsSource 
VHSv20160507 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.H 
hAverageConf 
vhsSource 
VHSv20170630 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.H 
hAverageConf 
vhsSource 
VHSv20180419 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.H 
hAverageConf 
vhsSource 
VHSv20201209 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.H 
hAverageConf 
vikingSource 
VIKINGDR2 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

99999999 
meta.code 
hAverageConf 
vikingSource 
VIKINGDR3 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

99999999 
stat.likelihood;em.IR.NIR 
hAverageConf 
vikingSource 
VIKINGDR4 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.H 
hAverageConf 
vikingSource 
VIKINGv20110714 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

99999999 
meta.code 
hAverageConf 
vikingSource 
VIKINGv20111019 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

99999999 
meta.code 
hAverageConf 
vikingSource 
VIKINGv20130417 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.NIR 
hAverageConf 
vikingSource 
VIKINGv20140402 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.NIR 
hAverageConf 
vikingSource 
VIKINGv20150421 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.H 
hAverageConf 
vikingSource 
VIKINGv20151230 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.H 
hAverageConf 
vikingSource 
VIKINGv20160406 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.H 
hAverageConf 
vikingSource 
VIKINGv20161202 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.H 
hAverageConf 
vikingSource 
VIKINGv20170715 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.H 
hAverageConf 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.NIR 
hAverageConf 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.NIR 
hAverageConf 
vvvSource 
VVVDR2 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.NIR 
hAverageConf 
vvvSource 
VVVDR5 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.H 
hAverageConf 
vvvSource, vvvSynopticSource 
VVVDR1 
average confidence in 2 arcsec diameter default aperture (aper3) H 
real 
4 

99999999 
stat.likelihood;em.IR.NIR 
hbestAper 
ultravistaMapLcVariability 
ULTRAVISTADR4 
Best aperture (13) for photometric statistics in the H band 
int 
4 

9999 

Aperture magnitude (16) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) 
hbestAper 
ultravistaVariability 
ULTRAVISTADR4 
Best aperture (16) for photometric statistics in the H band 
int 
4 

9999 
meta.code.class;em.IR.H 
Aperture magnitude (16) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) 
hbestAper 
videoVariability 
VIDEODR2 
Best aperture (16) for photometric statistics in the H band 
int 
4 

9999 

Aperture magnitude (16) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) 
hbestAper 
videoVariability 
VIDEODR3 
Best aperture (16) for photometric statistics in the H band 
int 
4 

9999 
meta.code.class;em.IR.NIR 
Aperture magnitude (16) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) 
hbestAper 
videoVariability 
VIDEODR4 
Best aperture (16) for photometric statistics in the H band 
int 
4 

9999 
meta.code.class;em.IR.H 
Aperture magnitude (16) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) 
hbestAper 
videoVariability 
VIDEODR5 
Best aperture (16) for photometric statistics in the H band 
int 
4 

9999 
meta.code.class;em.IR.H 
Aperture magnitude (16) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) 
hbestAper 
videoVariability 
VIDEOv20100513 
Best aperture (16) for photometric statistics in the H band 
int 
4 

9999 

Aperture magnitude (16) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) 
hbestAper 
videoVariability 
VIDEOv20111208 
Best aperture (16) for photometric statistics in the H band 
int 
4 

9999 

Aperture magnitude (16) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) 
hbestAper 
vikingVariability 
VIKINGDR2 
Best aperture (16) for photometric statistics in the H band 
int 
4 

9999 

Aperture magnitude (16) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) 
hbestAper 
vikingVariability 
VIKINGv20110714 
Best aperture (16) for photometric statistics in the H band 
int 
4 

9999 

Aperture magnitude (16) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) 
hbestAper 
vikingVariability 
VIKINGv20111019 
Best aperture (16) for photometric statistics in the H band 
int 
4 

9999 

Aperture magnitude (16) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) 
hbestAper 
vvvVariability 
VVVDR5 
Best aperture (16) for photometric statistics in the H band 
int 
4 

9999 
meta.code.class;em.IR.H 
Aperture magnitude (16) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) 
hbestAper 
vvvVariability 
VVVv20100531 
Best aperture (16) for photometric statistics in the H band 
int 
4 

9999 

Aperture magnitude (16) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) 
hbStratAst 
ultravistaVarFrameSetInfo 
ULTRAVISTADR4 
Parameter, c1 from FerreiraLopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in H band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hbStratAst 
videoVarFrameSetInfo 
VIDEODR2 
Strateva parameter, b, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hbStratAst 
videoVarFrameSetInfo 
VIDEODR3 
Strateva parameter, b, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hbStratAst 
videoVarFrameSetInfo 
VIDEODR4 
Strateva parameter, b, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hbStratAst 
videoVarFrameSetInfo 
VIDEODR5 
Strateva parameter, b, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hbStratAst 
videoVarFrameSetInfo 
VIDEOv20100513 
Strateva parameter, b, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hbStratAst 
videoVarFrameSetInfo 
VIDEOv20111208 
Strateva parameter, b, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hbStratAst 
vikingVarFrameSetInfo 
VIKINGDR2 
Strateva parameter, b, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hbStratAst 
vikingVarFrameSetInfo 
VIKINGv20110714 
Strateva parameter, b, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hbStratAst 
vikingVarFrameSetInfo 
VIKINGv20111019 
Strateva parameter, b, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hbStratAst 
vvvVarFrameSetInfo 
VVVDR5 
Parameter, c1 from FerreiraLopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in H band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hbStratAst 
vvvVarFrameSetInfo 
VVVv20100531 
Strateva parameter, b, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hbStratPht 
ultravistaMapLcVarFrameSetInfo 
ULTRAVISTADR4 
Strateva parameter, b, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hbStratPht 
ultravistaVarFrameSetInfo 
ULTRAVISTADR4 
Parameter, c1 from FerreiraLopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in H band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hbStratPht 
videoVarFrameSetInfo 
VIDEODR2 
Strateva parameter, b, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hbStratPht 
videoVarFrameSetInfo 
VIDEODR3 
Strateva parameter, b, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hbStratPht 
videoVarFrameSetInfo 
VIDEODR4 
Strateva parameter, b, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hbStratPht 
videoVarFrameSetInfo 
VIDEODR5 
Strateva parameter, b, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hbStratPht 
videoVarFrameSetInfo 
VIDEOv20100513 
Strateva parameter, b, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hbStratPht 
videoVarFrameSetInfo 
VIDEOv20111208 
Strateva parameter, b, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hbStratPht 
vikingVarFrameSetInfo 
VIKINGDR2 
Strateva parameter, b, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hbStratPht 
vikingVarFrameSetInfo 
VIKINGv20110714 
Strateva parameter, b, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hbStratPht 
vikingVarFrameSetInfo 
VIKINGv20111019 
Strateva parameter, b, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hbStratPht 
vvvVarFrameSetInfo 
VVVDR5 
Parameter, c1 from FerreiraLopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in H band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hbStratPht 
vvvVarFrameSetInfo 
VVVv20100531 
Strateva parameter, b, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hchiSqAst 
ultravistaVarFrameSetInfo 
ULTRAVISTADR4 
Goodness of fit of Strateva function to astrometric data in H band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hchiSqAst 
videoVarFrameSetInfo 
VIDEODR2 
Goodness of fit of Strateva function to astrometric data in H band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hchiSqAst 
videoVarFrameSetInfo 
VIDEODR3 
Goodness of fit of Strateva function to astrometric data in H band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hchiSqAst 
videoVarFrameSetInfo 
VIDEODR4 
Goodness of fit of Strateva function to astrometric data in H band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hchiSqAst 
videoVarFrameSetInfo 
VIDEODR5 
Goodness of fit of Strateva function to astrometric data in H band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hchiSqAst 
videoVarFrameSetInfo 
VIDEOv20100513 
Goodness of fit of Strateva function to astrometric data in H band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hchiSqAst 
videoVarFrameSetInfo 
VIDEOv20111208 
Goodness of fit of Strateva function to astrometric data in H band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hchiSqAst 
vikingVarFrameSetInfo 
VIKINGDR2 
Goodness of fit of Strateva function to astrometric data in H band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hchiSqAst 
vikingVarFrameSetInfo 
VIKINGv20110714 
Goodness of fit of Strateva function to astrometric data in H band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hchiSqAst 
vikingVarFrameSetInfo 
VIKINGv20111019 
Goodness of fit of Strateva function to astrometric data in H band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hchiSqAst 
vvvVarFrameSetInfo 
VVVDR5 
Goodness of fit of Strateva function to astrometric data in H band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hchiSqAst 
vvvVarFrameSetInfo 
VVVv20100531 
Goodness of fit of Strateva function to astrometric data in H band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hchiSqpd 
ultravistaMapLcVariability 
ULTRAVISTADR4 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hchiSqpd 
ultravistaVariability 
ULTRAVISTADR4 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2;em.IR.H 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hchiSqpd 
videoVariability 
VIDEODR2 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hchiSqpd 
videoVariability 
VIDEODR3 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hchiSqpd 
videoVariability 
VIDEODR4 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2;em.IR.H 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hchiSqpd 
videoVariability 
VIDEODR5 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2;em.IR.H 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hchiSqpd 
videoVariability 
VIDEOv20100513 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hchiSqpd 
videoVariability 
VIDEOv20111208 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hchiSqpd 
vikingVariability 
VIKINGDR2 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hchiSqpd 
vikingVariability 
VIKINGv20110714 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hchiSqpd 
vikingVariability 
VIKINGv20111019 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hchiSqpd 
vvvVariability 
VVVDR5 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 
stat.fit.chi2;em.IR.H 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hchiSqpd 
vvvVariability 
VVVv20100531 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hchiSqPht 
ultravistaMapLcVarFrameSetInfo, ultravistaVarFrameSetInfo 
ULTRAVISTADR4 
Goodness of fit of Strateva function to photometric data in H band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hchiSqPht 
videoVarFrameSetInfo 
VIDEODR2 
Goodness of fit of Strateva function to photometric data in H band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hchiSqPht 
videoVarFrameSetInfo 
VIDEODR3 
Goodness of fit of Strateva function to photometric data in H band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hchiSqPht 
videoVarFrameSetInfo 
VIDEODR4 
Goodness of fit of Strateva function to photometric data in H band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hchiSqPht 
videoVarFrameSetInfo 
VIDEODR5 
Goodness of fit of Strateva function to photometric data in H band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hchiSqPht 
videoVarFrameSetInfo 
VIDEOv20100513 
Goodness of fit of Strateva function to photometric data in H band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hchiSqPht 
videoVarFrameSetInfo 
VIDEOv20111208 
Goodness of fit of Strateva function to photometric data in H band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hchiSqPht 
vikingVarFrameSetInfo 
VIKINGDR2 
Goodness of fit of Strateva function to photometric data in H band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hchiSqPht 
vikingVarFrameSetInfo 
VIKINGv20110714 
Goodness of fit of Strateva function to photometric data in H band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hchiSqPht 
vikingVarFrameSetInfo 
VIKINGv20111019 
Goodness of fit of Strateva function to photometric data in H band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hchiSqPht 
vvvVarFrameSetInfo 
VVVDR5 
Goodness of fit of Strateva function to photometric data in H band 
real 
4 

0.9999995e9 
stat.fit.goodness;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hchiSqPht 
vvvVarFrameSetInfo 
VVVv20100531 
Goodness of fit of Strateva function to photometric data in H band 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
Hclass 
vvvParallaxCatalogue, vvvProperMotionCatalogue 
VVVDR5 
VVV DR4 H morphological classification. 1 = galaxy,0 = noise,1 = stellar,2 = probably stellar,3 = probable galaxy,7 = bad pixel within 2" aperture,9 = saturated {catalogue TType keyword: Hclass} 
int 
4 

99999999 

hClass 
ultravistaSource 
ULTRAVISTADR4 
discrete image classification flag in H 
smallint 
2 

9999 
src.class;em.IR.H 
hClass 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
vhsSource 
VHSDR2 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
vhsSource 
VHSDR3 
discrete image classification flag in H 
smallint 
2 

9999 
src.class;em.IR.H 
hClass 
vhsSource 
VHSDR4 
discrete image classification flag in H 
smallint 
2 

9999 
src.class;em.IR.H 
hClass 
vhsSource 
VHSDR5 
discrete image classification flag in H 
smallint 
2 

9999 
src.class;em.IR.H 
hClass 
vhsSource 
VHSDR6 
discrete image classification flag in H 
smallint 
2 

9999 
src.class;em.IR.H 
hClass 
vhsSource 
VHSv20120926 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
vhsSource 
VHSv20130417 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
vhsSource 
VHSv20140409 
discrete image classification flag in H 
smallint 
2 

9999 
src.class;em.IR.H 
hClass 
vhsSource 
VHSv20150108 
discrete image classification flag in H 
smallint 
2 

9999 
src.class;em.IR.H 
hClass 
vhsSource 
VHSv20160114 
discrete image classification flag in H 
smallint 
2 

9999 
src.class;em.IR.H 
hClass 
vhsSource 
VHSv20160507 
discrete image classification flag in H 
smallint 
2 

9999 
src.class;em.IR.H 
hClass 
vhsSource 
VHSv20170630 
discrete image classification flag in H 
smallint 
2 

9999 
src.class;em.IR.H 
hClass 
vhsSource 
VHSv20180419 
discrete image classification flag in H 
smallint 
2 

9999 
src.class;em.IR.H 
hClass 
vhsSource 
VHSv20201209 
discrete image classification flag in H 
smallint 
2 

9999 
src.class;em.IR.H 
hClass 
vhsSource, vhsSourceRemeasurement 
VHSDR1 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
videoSource 
VIDEODR2 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
videoSource 
VIDEODR3 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
videoSource 
VIDEODR4 
discrete image classification flag in H 
smallint 
2 

9999 
src.class;em.IR.H 
hClass 
videoSource 
VIDEODR5 
discrete image classification flag in H 
smallint 
2 

9999 
src.class;em.IR.H 
hClass 
videoSource 
VIDEOv20111208 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
videoSource, videoSourceRemeasurement 
VIDEOv20100513 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
vikingSource 
VIKINGDR2 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
vikingSource 
VIKINGDR3 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
vikingSource 
VIKINGDR4 
discrete image classification flag in H 
smallint 
2 

9999 
src.class;em.IR.H 
hClass 
vikingSource 
VIKINGv20111019 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
vikingSource 
VIKINGv20130417 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
vikingSource 
VIKINGv20140402 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
vikingSource 
VIKINGv20150421 
discrete image classification flag in H 
smallint 
2 

9999 
src.class;em.IR.H 
hClass 
vikingSource 
VIKINGv20151230 
discrete image classification flag in H 
smallint 
2 

9999 
src.class;em.IR.H 
hClass 
vikingSource 
VIKINGv20160406 
discrete image classification flag in H 
smallint 
2 

9999 
src.class;em.IR.H 
hClass 
vikingSource 
VIKINGv20161202 
discrete image classification flag in H 
smallint 
2 

9999 
src.class;em.IR.H 
hClass 
vikingSource 
VIKINGv20170715 
discrete image classification flag in H 
smallint 
2 

9999 
src.class;em.IR.H 
hClass 
vikingSource, vikingSourceRemeasurement 
VIKINGv20110714 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
vvvSource 
VVVDR2 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
vvvSource 
VVVDR5 
discrete image classification flag in H 
smallint 
2 

9999 
src.class;em.IR.H 
hClass 
vvvSource 
VVVv20110718 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
vvvSource, vvvSourceRemeasurement 
VVVv20100531 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClass 
vvvSource, vvvSynopticSource 
VVVDR1 
discrete image classification flag in H 
smallint 
2 

9999 
src.class 
hClassStat 
ultravistaSource 
ULTRAVISTADR4 
SExtractor classification statistic in H 
real 
4 

0.9999995e9 
stat;em.IR.H 
hClassStat 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat 
hClassStat 
vhsSource 
VHSDR2 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat 
hClassStat 
vhsSource 
VHSDR3 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat;em.IR.H 
hClassStat 
vhsSource 
VHSDR4 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat;em.IR.H 
hClassStat 
vhsSource 
VHSDR5 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat;em.IR.H 
hClassStat 
vhsSource 
VHSDR6 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat;em.IR.H 
hClassStat 
vhsSource 
VHSv20120926 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat 
hClassStat 
vhsSource 
VHSv20130417 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat 
hClassStat 
vhsSource 
VHSv20140409 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat;em.IR.H 
hClassStat 
vhsSource 
VHSv20150108 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat;em.IR.H 
hClassStat 
vhsSource 
VHSv20160114 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat;em.IR.H 
hClassStat 
vhsSource 
VHSv20160507 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat;em.IR.H 
hClassStat 
vhsSource 
VHSv20170630 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat;em.IR.H 
hClassStat 
vhsSource 
VHSv20180419 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat;em.IR.H 
hClassStat 
vhsSource 
VHSv20201209 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat;em.IR.H 
hClassStat 
vhsSource, vhsSourceRemeasurement 
VHSDR1 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat 
hClassStat 
videoSource 
VIDEODR2 
SExtractor classification statistic in H 
real 
4 

0.9999995e9 
stat 
hClassStat 
videoSource 
VIDEODR3 
SExtractor classification statistic in H 
real 
4 

0.9999995e9 
stat 
hClassStat 
videoSource 
VIDEODR4 
SExtractor classification statistic in H 
real 
4 

0.9999995e9 
stat;em.IR.H 
hClassStat 
videoSource 
VIDEODR5 
SExtractor classification statistic in H 
real 
4 

0.9999995e9 
stat;em.IR.H 
hClassStat 
videoSource 
VIDEOv20100513 
SExtractor classification statistic in H 
real 
4 

0.9999995e9 
stat 
hClassStat 
videoSource 
VIDEOv20111208 
SExtractor classification statistic in H 
real 
4 

0.9999995e9 
stat 
hClassStat 
videoSourceRemeasurement 
VIDEOv20100513 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat 
hClassStat 
vikingSource 
VIKINGDR2 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat 
hClassStat 
vikingSource 
VIKINGDR3 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat 
hClassStat 
vikingSource 
VIKINGDR4 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat;em.IR.H 
hClassStat 
vikingSource 
VIKINGv20111019 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat 
hClassStat 
vikingSource 
VIKINGv20130417 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat 
hClassStat 
vikingSource 
VIKINGv20140402 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat 
hClassStat 
vikingSource 
VIKINGv20150421 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat;em.IR.H 
hClassStat 
vikingSource 
VIKINGv20151230 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat;em.IR.H 
hClassStat 
vikingSource 
VIKINGv20160406 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat;em.IR.H 
hClassStat 
vikingSource 
VIKINGv20161202 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat;em.IR.H 
hClassStat 
vikingSource 
VIKINGv20170715 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat;em.IR.H 
hClassStat 
vikingSource, vikingSourceRemeasurement 
VIKINGv20110714 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat 
hClassStat 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat 
hClassStat 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat 
hClassStat 
vvvSource 
VVVDR1 
SExtractor classification statistic in H 
real 
4 

0.9999995e9 
stat 
hClassStat 
vvvSource 
VVVDR2 
SExtractor classification statistic in H 
real 
4 

0.9999995e9 
stat 
hClassStat 
vvvSource 
VVVDR5 
SExtractor classification statistic in H 
real 
4 

0.9999995e9 
stat;em.IR.H 
hClassStat 
vvvSource 
VVVv20100531 
SExtractor classification statistic in H 
real 
4 

0.9999995e9 
stat 
hClassStat 
vvvSource 
VVVv20110718 
SExtractor classification statistic in H 
real 
4 

0.9999995e9 
stat 
hClassStat 
vvvSourceRemeasurement 
VVVv20100531 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat 
hClassStat 
vvvSourceRemeasurement 
VVVv20110718 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat 
hClassStat 
vvvSynopticSource 
VVVDR1 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat 
hClassStat 
vvvSynopticSource 
VVVDR2 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
stat 
hCorr 
twompzPhotoz 
TWOMPZ 
H 20mag/sq." isophotal fiducial ell. ap. magnitude with Galactic dust correction {image primary HDU keyword: Hcorr} 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hCorrErr 
twompzPhotoz 
TWOMPZ 
H 1sigma uncertainty in 20mag/sq." aperture {image primary HDU keyword: h_msig_k20fe} 
real 
4 
mag 
0.9999995e9 

hcStratAst 
ultravistaVarFrameSetInfo 
ULTRAVISTADR4 
Parameter, c2 from FerreiraLopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in H band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hcStratAst 
videoVarFrameSetInfo 
VIDEODR2 
Strateva parameter, c, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hcStratAst 
videoVarFrameSetInfo 
VIDEODR3 
Strateva parameter, c, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hcStratAst 
videoVarFrameSetInfo 
VIDEODR4 
Strateva parameter, c, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hcStratAst 
videoVarFrameSetInfo 
VIDEODR5 
Strateva parameter, c, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hcStratAst 
videoVarFrameSetInfo 
VIDEOv20100513 
Strateva parameter, c, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hcStratAst 
videoVarFrameSetInfo 
VIDEOv20111208 
Strateva parameter, c, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hcStratAst 
vikingVarFrameSetInfo 
VIKINGDR2 
Strateva parameter, c, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hcStratAst 
vikingVarFrameSetInfo 
VIKINGv20110714 
Strateva parameter, c, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hcStratAst 
vikingVarFrameSetInfo 
VIKINGv20111019 
Strateva parameter, c, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hcStratAst 
vvvVarFrameSetInfo 
VVVDR5 
Parameter, c2 from FerreiraLopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in H band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hcStratAst 
vvvVarFrameSetInfo 
VVVv20100531 
Strateva parameter, c, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hcStratPht 
ultravistaMapLcVarFrameSetInfo 
ULTRAVISTADR4 
Strateva parameter, c, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hcStratPht 
ultravistaVarFrameSetInfo 
ULTRAVISTADR4 
Parameter, c2 from FerreiraLopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in H band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hcStratPht 
videoVarFrameSetInfo 
VIDEODR2 
Strateva parameter, c, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hcStratPht 
videoVarFrameSetInfo 
VIDEODR3 
Strateva parameter, c, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.NIR 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hcStratPht 
videoVarFrameSetInfo 
VIDEODR4 
Strateva parameter, c, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hcStratPht 
videoVarFrameSetInfo 
VIDEODR5 
Strateva parameter, c, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hcStratPht 
videoVarFrameSetInfo 
VIDEOv20100513 
Strateva parameter, c, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hcStratPht 
videoVarFrameSetInfo 
VIDEOv20111208 
Strateva parameter, c, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hcStratPht 
vikingVarFrameSetInfo 
VIKINGDR2 
Strateva parameter, c, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hcStratPht 
vikingVarFrameSetInfo 
VIKINGv20110714 
Strateva parameter, c, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hcStratPht 
vikingVarFrameSetInfo 
VIKINGv20111019 
Strateva parameter, c, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hcStratPht 
vvvVarFrameSetInfo 
VVVDR5 
Parameter, c2 from FerreiraLopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in H band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hcStratPht 
vvvVarFrameSetInfo 
VVVv20100531 
Strateva parameter, c, in fit to photometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hDeblend 
vhsSourceRemeasurement 
VHSDR1 
placeholder flag indicating parent/child relation in H 
int 
4 

99999999 
meta.code 
hDeblend 
videoSource, videoSourceRemeasurement 
VIDEOv20100513 
placeholder flag indicating parent/child relation in H 
int 
4 

99999999 
meta.code 
hDeblend 
vikingSourceRemeasurement 
VIKINGv20110714 
placeholder flag indicating parent/child relation in H 
int 
4 

99999999 
meta.code 
hDeblend 
vikingSourceRemeasurement 
VIKINGv20111019 
placeholder flag indicating parent/child relation in H 
int 
4 

99999999 
meta.code 
hDeblend 
vvvSource 
VVVv20110718 
placeholder flag indicating parent/child relation in H 
int 
4 

99999999 
meta.code 
hDeblend 
vvvSource, vvvSourceRemeasurement 
VVVv20100531 
placeholder flag indicating parent/child relation in H 
int 
4 

99999999 
meta.code 
HEALPix 
ravedr5Source 
RAVE 
Hierarchical EqualArea isoLatitude Pixelisation value (N_side = 4096) 
bigint 
8 


meta.code 
HeightLSG 
vvvVivaCatalogue 
VVVDR5 
Height of FreqLSG considering LSG method {catalogue TType keyword: HeightLSG} 
float 
8 
?? 
9.999995e8 

HeightPDM 
vvvVivaCatalogue 
VVVDR5 
Height of FreqPDM considering PDM method {catalogue TType keyword: HeightPDM} 
float 
8 
?? 
9.999995e8 

HeightPKfi2 
vvvVivaCatalogue 
VVVDR5 
Height of FreqPKfi2 using PK method {catalogue TType keyword: HeightPKfi2} 
float 
8 
?? 
9.999995e8 

HeightPLfi2 
vvvVivaCatalogue 
VVVDR5 
Height of FreqPLfi2 considering PL method {catalogue TType keyword: HeightPLfi2} 
float 
8 
?? 
9.999995e8 

HeightSTR 
vvvVivaCatalogue 
VVVDR5 
Height of FreqSTR considering STR method {catalogue TType keyword: HeightSTR} 
float 
8 
?? 
9.999995e8 

Hell 
vvvParallaxCatalogue, vvvProperMotionCatalogue 
VVVDR5 
Ellipticity of the DR4 H detection. {catalogue TType keyword: Hell} 
real 
4 

999999500.0 

hEll 
ultravistaSource 
ULTRAVISTADR4 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.H 
hEll 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticty 
hEll 
vhsSource 
VHSDR2 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity 
hEll 
vhsSource 
VHSDR3 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.H 
hEll 
vhsSource 
VHSDR4 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.H 
hEll 
vhsSource 
VHSDR5 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.H 
hEll 
vhsSource 
VHSDR6 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.H 
hEll 
vhsSource 
VHSv20120926 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity 
hEll 
vhsSource 
VHSv20130417 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity 
hEll 
vhsSource 
VHSv20140409 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.H 
hEll 
vhsSource 
VHSv20150108 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.H 
hEll 
vhsSource 
VHSv20160114 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.H 
hEll 
vhsSource 
VHSv20160507 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.H 
hEll 
vhsSource 
VHSv20170630 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.H 
hEll 
vhsSource 
VHSv20180419 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.H 
hEll 
vhsSource 
VHSv20201209 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.H 
hEll 
vhsSource, vhsSourceRemeasurement 
VHSDR1 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity 
hEll 
videoSource 
VIDEODR2 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity 
hEll 
videoSource 
VIDEODR3 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity 
hEll 
videoSource 
VIDEODR4 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.H 
hEll 
videoSource 
VIDEODR5 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.H 
hEll 
videoSource 
VIDEOv20111208 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity 
hEll 
videoSource, videoSourceRemeasurement 
VIDEOv20100513 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity 
hEll 
vikingSource 
VIKINGDR2 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity 
hEll 
vikingSource 
VIKINGDR3 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity 
hEll 
vikingSource 
VIKINGDR4 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.H 
hEll 
vikingSource 
VIKINGv20111019 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity 
hEll 
vikingSource 
VIKINGv20130417 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity 
hEll 
vikingSource 
VIKINGv20140402 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity 
hEll 
vikingSource 
VIKINGv20150421 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.H 
hEll 
vikingSource 
VIKINGv20151230 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.H 
hEll 
vikingSource 
VIKINGv20160406 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.H 
hEll 
vikingSource 
VIKINGv20161202 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.H 
hEll 
vikingSource 
VIKINGv20170715 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.H 
hEll 
vikingSource, vikingSourceRemeasurement 
VIKINGv20110714 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity 
hEll 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity 
hEll 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity 
hEll 
vvvSource 
VVVDR2 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity 
hEll 
vvvSource 
VVVDR5 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity;em.IR.H 
hEll 
vvvSource 
VVVv20110718 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity 
hEll 
vvvSource, vvvSourceRemeasurement 
VVVv20100531 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity 
hEll 
vvvSource, vvvSynopticSource 
VVVDR1 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
src.ellipticity 
hemis 
twomass_psc 
TWOMASS 
Hemisphere code for the TWOMASS Observatory from which this source was observed. 
varchar 
1 


meta.code;obs 
hemis 
twomass_scn 
TWOMASS 
Observatory from which data were obtained: "n" = north = Mt. Hopkins, "s" = south = Cerro Tololo. 
varchar 
1 


meta.code;obs 
hemis 
twomass_sixx2_scn 
TWOMASS 
hemisphere (N/S) of observation 
varchar 
1 



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


meta.code;obs 
heNum 
ultravistaMergeLog, ultravistaRemeasMergeLog 
ULTRAVISTADR4 
the extension number of this H frame 
tinyint 
1 


meta.number;em.IR.H 
heNum 
vhsMergeLog 
VHSDR1 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
vhsMergeLog 
VHSDR2 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
vhsMergeLog 
VHSDR3 
the extension number of this H frame 
tinyint 
1 


meta.number;em.IR.H 
heNum 
vhsMergeLog 
VHSDR4 
the extension number of this H frame 
tinyint 
1 


meta.number;em.IR.H 
heNum 
vhsMergeLog 
VHSDR5 
the extension number of this H frame 
tinyint 
1 


meta.number;em.IR.H 
heNum 
vhsMergeLog 
VHSDR6 
the extension number of this H frame 
tinyint 
1 


meta.number;em.IR.H 
heNum 
vhsMergeLog 
VHSv20120926 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
vhsMergeLog 
VHSv20130417 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
vhsMergeLog 
VHSv20140409 
the extension number of this H frame 
tinyint 
1 


meta.number;em.IR.H 
heNum 
vhsMergeLog 
VHSv20150108 
the extension number of this H frame 
tinyint 
1 


meta.number;em.IR.H 
heNum 
vhsMergeLog 
VHSv20160114 
the extension number of this H frame 
tinyint 
1 


meta.number;em.IR.H 
heNum 
vhsMergeLog 
VHSv20160507 
the extension number of this H frame 
tinyint 
1 


meta.number;em.IR.H 
heNum 
vhsMergeLog 
VHSv20170630 
the extension number of this H frame 
tinyint 
1 


meta.number;em.IR.H 
heNum 
vhsMergeLog 
VHSv20180419 
the extension number of this H frame 
tinyint 
1 


meta.number;em.IR.H 
heNum 
vhsMergeLog 
VHSv20201209 
the extension number of this H frame 
tinyint 
1 


meta.id;em.IR.H 
heNum 
videoMergeLog 
VIDEODR2 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
videoMergeLog 
VIDEODR3 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
videoMergeLog 
VIDEODR4 
the extension number of this H frame 
tinyint 
1 


meta.number;em.IR.H 
heNum 
videoMergeLog 
VIDEODR5 
the extension number of this H frame 
tinyint 
1 


meta.number;em.IR.H 
heNum 
videoMergeLog 
VIDEOv20100513 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
videoMergeLog 
VIDEOv20111208 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
vikingMergeLog 
VIKINGDR2 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
vikingMergeLog 
VIKINGDR3 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
vikingMergeLog 
VIKINGDR4 
the extension number of this H frame 
tinyint 
1 


meta.number;em.IR.H 
heNum 
vikingMergeLog 
VIKINGv20110714 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
vikingMergeLog 
VIKINGv20111019 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
vikingMergeLog 
VIKINGv20130417 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
vikingMergeLog 
VIKINGv20140402 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
vikingMergeLog 
VIKINGv20150421 
the extension number of this H frame 
tinyint 
1 


meta.number;em.IR.H 
heNum 
vikingMergeLog 
VIKINGv20151230 
the extension number of this H frame 
tinyint 
1 


meta.number;em.IR.H 
heNum 
vikingMergeLog 
VIKINGv20160406 
the extension number of this H frame 
tinyint 
1 


meta.number;em.IR.H 
heNum 
vikingMergeLog 
VIKINGv20161202 
the extension number of this H frame 
tinyint 
1 


meta.number;em.IR.H 
heNum 
vikingMergeLog 
VIKINGv20170715 
the extension number of this H frame 
tinyint 
1 


meta.number;em.IR.H 
heNum 
vikingZY_selJ_RemeasMergeLog 
VIKINGZYSELJv20160909 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
vikingZY_selJ_RemeasMergeLog 
VIKINGZYSELJv20170124 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
vvvMergeLog 
VVVDR2 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
vvvMergeLog 
VVVDR5 
the extension number of this H frame 
tinyint 
1 


meta.number;em.IR.H 
heNum 
vvvMergeLog 
VVVv20100531 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
vvvMergeLog 
VVVv20110718 
the extension number of this H frame 
tinyint 
1 


meta.number 
heNum 
vvvMergeLog, vvvSynopticMergeLog 
VVVDR1 
the extension number of this H frame 
tinyint 
1 


meta.number 
hErrBits 
ultravistaSource 
ULTRAVISTADR4 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code;em.IR.H 
This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows: Bit Flag  Meaning   1  The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected).   2  The object was originally blended with another   4  At least one pixel is saturated (or very close to)   8  The object is truncated (too close to an image boundary)   16  Object's aperture data are incomplete or corrupted   32  Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters.   64  Memory overflow occurred during deblending   128  Memory overflow occurred during extraction  

hErrBits 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vhsSource 
VHSDR1 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vhsSource 
VHSDR2 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vhsSource 
VHSDR3 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code;em.IR.H 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vhsSource 
VHSDR4 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code;em.IR.H 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vhsSource 
VHSDR5 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code;em.IR.H 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vhsSource 
VHSDR6 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code;em.IR.H 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vhsSource 
VHSv20120926 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vhsSource 
VHSv20130417 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vhsSource 
VHSv20140409 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code;em.IR.H 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vhsSource 
VHSv20150108 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code;em.IR.H 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vhsSource 
VHSv20160114 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code;em.IR.H 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vhsSource 
VHSv20160507 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code;em.IR.H 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vhsSource 
VHSv20170630 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code;em.IR.H 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vhsSource 
VHSv20180419 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code;em.IR.H 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vhsSource 
VHSv20201209 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code;em.IR.H 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vhsSourceRemeasurement 
VHSDR1 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code 
hErrBits 
videoSource 
VIDEODR2 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code 
This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows: Bit Flag  Meaning   1  The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected).   2  The object was originally blended with another   4  At least one pixel is saturated (or very close to)   8  The object is truncated (too close to an image boundary)   16  Object's aperture data are incomplete or corrupted   32  Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters.   64  Memory overflow occurred during deblending   128  Memory overflow occurred during extraction  

hErrBits 
videoSource 
VIDEODR3 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code 
This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows: Bit Flag  Meaning   1  The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected).   2  The object was originally blended with another   4  At least one pixel is saturated (or very close to)   8  The object is truncated (too close to an image boundary)   16  Object's aperture data are incomplete or corrupted   32  Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters.   64  Memory overflow occurred during deblending   128  Memory overflow occurred during extraction  

hErrBits 
videoSource 
VIDEODR4 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code;em.IR.H 
This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows: Bit Flag  Meaning   1  The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected).   2  The object was originally blended with another   4  At least one pixel is saturated (or very close to)   8  The object is truncated (too close to an image boundary)   16  Object's aperture data are incomplete or corrupted   32  Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters.   64  Memory overflow occurred during deblending   128  Memory overflow occurred during extraction  

hErrBits 
videoSource 
VIDEODR5 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code;em.IR.H 
This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows: Bit Flag  Meaning   1  The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected).   2  The object was originally blended with another   4  At least one pixel is saturated (or very close to)   8  The object is truncated (too close to an image boundary)   16  Object's aperture data are incomplete or corrupted   32  Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters.   64  Memory overflow occurred during deblending   128  Memory overflow occurred during extraction  

hErrBits 
videoSource 
VIDEOv20100513 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code 
This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows: Bit Flag  Meaning   1  The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected).   2  The object was originally blended with another   4  At least one pixel is saturated (or very close to)   8  The object is truncated (too close to an image boundary)   16  Object's aperture data are incomplete or corrupted   32  Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters.   64  Memory overflow occurred during deblending   128  Memory overflow occurred during extraction  

hErrBits 
videoSource 
VIDEOv20111208 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code 
This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows: Bit Flag  Meaning   1  The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected).   2  The object was originally blended with another   4  At least one pixel is saturated (or very close to)   8  The object is truncated (too close to an image boundary)   16  Object's aperture data are incomplete or corrupted   32  Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters.   64  Memory overflow occurred during deblending   128  Memory overflow occurred during extraction  

hErrBits 
videoSourceRemeasurement 
VIDEOv20100513 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code 
hErrBits 
vikingSource 
VIKINGDR2 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vikingSource 
VIKINGDR3 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vikingSource 
VIKINGDR4 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code;em.IR.H 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vikingSource 
VIKINGv20110714 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vikingSource 
VIKINGv20111019 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vikingSource 
VIKINGv20130417 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vikingSource 
VIKINGv20140402 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vikingSource 
VIKINGv20150421 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code;em.IR.H 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vikingSource 
VIKINGv20151230 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code;em.IR.H 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vikingSource 
VIKINGv20160406 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code;em.IR.H 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vikingSource 
VIKINGv20161202 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code;em.IR.H 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vikingSource 
VIKINGv20170715 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code;em.IR.H 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vikingSourceRemeasurement 
VIKINGv20110714 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code 
hErrBits 
vikingSourceRemeasurement 
VIKINGv20111019 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code 
hErrBits 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vvvSource 
VVVDR2 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vvvSource 
VVVDR5 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code;em.IR.H 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vvvSource 
VVVv20100531 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vvvSource 
VVVv20110718 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vvvSource, vvvSynopticSource 
VVVDR1 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
hErrBits 
vvvSourceRemeasurement 
VVVv20100531 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code 
hErrBits 
vvvSourceRemeasurement 
VVVv20110718 
processing warning/error bitwise flags in H 
int 
4 

99999999 
meta.code 
hEta 
ultravistaSource 
ULTRAVISTADR4 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.H 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
vhsSource 
VHSDR1 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
vhsSource 
VHSDR2 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
vhsSource 
VHSDR3 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.H 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
vhsSource 
VHSDR4 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.H 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
vhsSource 
VHSDR5 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.H 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
vhsSource 
VHSDR6 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.H 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
vhsSource 
VHSv20120926 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
vhsSource 
VHSv20130417 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
vhsSource 
VHSv20140409 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.H 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
vhsSource 
VHSv20150108 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.H 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
vhsSource 
VHSv20160114 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.H 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
vhsSource 
VHSv20160507 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.H 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
vhsSource 
VHSv20170630 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.H 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
vhsSource 
VHSv20180419 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.H 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
vhsSource 
VHSv20201209 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.H 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
videoSource 
VIDEODR2 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
videoSource 
VIDEODR3 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
videoSource 
VIDEODR4 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.H 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
videoSource 
VIDEODR5 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.H 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
videoSource 
VIDEOv20100513 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
videoSource 
VIDEOv20111208 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
vikingSource 
VIKINGDR2 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
vikingSource 
VIKINGDR3 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
vikingSource 
VIKINGDR4 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.H 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
vikingSource 
VIKINGv20110714 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
vikingSource 
VIKINGv20111019 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
vikingSource 
VIKINGv20130417 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
vikingSource 
VIKINGv20140402 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
vikingSource 
VIKINGv20150421 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.H 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
vikingSource 
VIKINGv20151230 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.H 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
vikingSource 
VIKINGv20160406 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.H 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
vikingSource 
VIKINGv20161202 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.H 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
vikingSource 
VIKINGv20170715 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.H 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
vvvSource 
VVVDR2 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
vvvSource 
VVVDR5 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff;em.IR.H 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
vvvSource 
VVVv20100531 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
vvvSource 
VVVv20110718 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hEta 
vvvSource, vvvSynopticSource 
VVVDR1 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. 
hexpML 
ultravistaMapLcVarFrameSetInfo, ultravistaVarFrameSetInfo 
ULTRAVISTADR4 
Expected magnitude limit of frameSet in this in H band. 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H;stat.max 
hexpML 
videoVarFrameSetInfo 
VIDEODR2 
Expected magnitude limit of frameSet in this in H band. 
real 
4 

0.9999995e9 

hexpML 
videoVarFrameSetInfo 
VIDEODR3 
Expected magnitude limit of frameSet in this in H band. 
real 
4 

0.9999995e9 
phot.mag;stat.max;em.IR.NIR 
hexpML 
videoVarFrameSetInfo 
VIDEODR4 
Expected magnitude limit of frameSet in this in H band. 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H;stat.max 
hexpML 
videoVarFrameSetInfo 
VIDEODR5 
Expected magnitude limit of frameSet in this in H band. 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H;stat.max 
hexpML 
videoVarFrameSetInfo 
VIDEOv20100513 
Expected magnitude limit of frameSet in this in H band. 
real 
4 

0.9999995e9 

hexpML 
videoVarFrameSetInfo 
VIDEOv20111208 
Expected magnitude limit of frameSet in this in H band. 
real 
4 

0.9999995e9 

hexpML 
vikingVarFrameSetInfo 
VIKINGDR2 
Expected magnitude limit of frameSet in this in H band. 
real 
4 

0.9999995e9 

hexpML 
vikingVarFrameSetInfo 
VIKINGv20110714 
Expected magnitude limit of frameSet in this in H band. 
real 
4 

0.9999995e9 

hexpML 
vikingVarFrameSetInfo 
VIKINGv20111019 
Expected magnitude limit of frameSet in this in H band. 
real 
4 

0.9999995e9 

hexpML 
vvvVarFrameSetInfo 
VVVDR5 
Expected magnitude limit of frameSet in this in H band. 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H;stat.max 
hexpML 
vvvVarFrameSetInfo 
VVVv20100531 
Expected magnitude limit of frameSet in this in H band. 
real 
4 

0.9999995e9 

hExpRms 
ultravistaMapLcVariability 
ULTRAVISTADR4 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in H band 
real 
4 
mag 
0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hExpRms 
ultravistaVariability 
ULTRAVISTADR4 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in H band 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hExpRms 
videoVariability 
VIDEODR2 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in H band 
real 
4 
mag 
0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hExpRms 
videoVariability 
VIDEODR3 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in H band 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.NIR 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hExpRms 
videoVariability 
VIDEODR4 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in H band 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hExpRms 
videoVariability 
VIDEODR5 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in H band 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hExpRms 
videoVariability 
VIDEOv20100513 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in H band 
real 
4 
mag 
0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hExpRms 
videoVariability 
VIDEOv20111208 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in H band 
real 
4 
mag 
0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hExpRms 
vikingVariability 
VIKINGDR2 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in H band 
real 
4 
mag 
0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hExpRms 
vikingVariability 
VIKINGv20110714 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in H band 
real 
4 
mag 
0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hExpRms 
vikingVariability 
VIKINGv20111019 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in H band 
real 
4 
mag 
0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hExpRms 
vvvVariability 
VVVDR5 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in H band 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hExpRms 
vvvVariability 
VVVv20100531 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in H band 
real 
4 
mag 
0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hGausig 
ultravistaSource 
ULTRAVISTADR4 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.IR.H 
hGausig 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
vhsSource 
VHSDR2 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
vhsSource 
VHSDR3 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.IR.H 
hGausig 
vhsSource 
VHSDR4 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.IR.H 
hGausig 
vhsSource 
VHSDR5 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.IR.H 
hGausig 
vhsSource 
VHSDR6 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.IR.H 
hGausig 
vhsSource 
VHSv20120926 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
vhsSource 
VHSv20130417 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
vhsSource 
VHSv20140409 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.IR.H 
hGausig 
vhsSource 
VHSv20150108 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.IR.H 
hGausig 
vhsSource 
VHSv20160114 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.IR.H 
hGausig 
vhsSource 
VHSv20160507 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.IR.H 
hGausig 
vhsSource 
VHSv20170630 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.IR.H 
hGausig 
vhsSource 
VHSv20180419 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.IR.H 
hGausig 
vhsSource 
VHSv20201209 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.IR.H 
hGausig 
vhsSource, vhsSourceRemeasurement 
VHSDR1 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
videoSource 
VIDEODR2 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
videoSource 
VIDEODR3 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
videoSource 
VIDEODR4 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.IR.H 
hGausig 
videoSource 
VIDEODR5 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.IR.H 
hGausig 
videoSource 
VIDEOv20111208 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
videoSource, videoSourceRemeasurement 
VIDEOv20100513 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
vikingSource 
VIKINGDR2 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
vikingSource 
VIKINGDR3 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
vikingSource 
VIKINGDR4 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.IR.H 
hGausig 
vikingSource 
VIKINGv20111019 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
vikingSource 
VIKINGv20130417 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
vikingSource 
VIKINGv20140402 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
vikingSource 
VIKINGv20150421 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.IR.H 
hGausig 
vikingSource 
VIKINGv20151230 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.IR.H 
hGausig 
vikingSource 
VIKINGv20160406 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.IR.H 
hGausig 
vikingSource 
VIKINGv20161202 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.IR.H 
hGausig 
vikingSource 
VIKINGv20170715 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.IR.H 
hGausig 
vikingSource, vikingSourceRemeasurement 
VIKINGv20110714 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
vvvSource 
VVVDR2 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
vvvSource 
VVVDR5 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param;em.IR.H 
hGausig 
vvvSource 
VVVv20110718 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
vvvSource, vvvSourceRemeasurement 
VVVv20100531 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hGausig 
vvvSource, vvvSynopticSource 
VVVDR1 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
hgl 
twomass_scn 
TWOMASS 
Special flag indicating whether or not this scan has a singleframe Hband electronic glitch. 
smallint 
2 


meta.code 
hgl 
twomass_sixx2_scn 
TWOMASS 
singleframe Hband glitch flag (0:not found1:found) 
smallint 
2 



hHalfRad 
ultravistaSource 
ULTRAVISTADR4 
SExtractor halflight radius in H band 
real 
4 
pixels 
0.9999995e9 
phys.angSize;em.IR.H 
hHalfRad 
videoSource 
VIDEODR4 
SExtractor halflight radius in H band 
real 
4 
pixels 
0.9999995e9 
phys.angSize;em.IR.H 
hHalfRad 
videoSource 
VIDEODR5 
SExtractor halflight radius in H band 
real 
4 
pixels 
0.9999995e9 
phys.angSize;em.IR.H 
hHlCorSMjRadAs 
ultravistaSource 
ULTRAVISTADR4 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.IR.H 
hHlCorSMjRadAs 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hHlCorSMjRadAs 
vhsSource 
VHSDR1 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hHlCorSMjRadAs 
vhsSource 
VHSDR2 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hHlCorSMjRadAs 
vhsSource 
VHSDR3 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.IR.H 
hHlCorSMjRadAs 
vhsSource 
VHSDR4 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.IR.H 
hHlCorSMjRadAs 
vhsSource 
VHSDR5 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.IR.H 
hHlCorSMjRadAs 
vhsSource 
VHSDR6 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.IR.H 
hHlCorSMjRadAs 
vhsSource 
VHSv20120926 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hHlCorSMjRadAs 
vhsSource 
VHSv20130417 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hHlCorSMjRadAs 
vhsSource 
VHSv20140409 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.IR.H 
hHlCorSMjRadAs 
vhsSource 
VHSv20150108 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.IR.H 
hHlCorSMjRadAs 
vhsSource 
VHSv20160114 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.IR.H 
hHlCorSMjRadAs 
vhsSource 
VHSv20160507 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.IR.H 
hHlCorSMjRadAs 
vhsSource 
VHSv20170630 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.IR.H 
hHlCorSMjRadAs 
vhsSource 
VHSv20180419 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.IR.H 
hHlCorSMjRadAs 
vhsSource 
VHSv20201209 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.IR.H 
hHlCorSMjRadAs 
videoSource 
VIDEODR2 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hHlCorSMjRadAs 
videoSource 
VIDEODR3 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hHlCorSMjRadAs 
videoSource 
VIDEODR4 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.IR.H 
hHlCorSMjRadAs 
videoSource 
VIDEODR5 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.IR.H 
hHlCorSMjRadAs 
videoSource 
VIDEOv20100513 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hHlCorSMjRadAs 
videoSource 
VIDEOv20111208 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hHlCorSMjRadAs 
vikingSource 
VIKINGDR2 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hHlCorSMjRadAs 
vikingSource 
VIKINGDR3 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hHlCorSMjRadAs 
vikingSource 
VIKINGDR4 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.IR.H 
hHlCorSMjRadAs 
vikingSource 
VIKINGv20110714 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hHlCorSMjRadAs 
vikingSource 
VIKINGv20111019 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hHlCorSMjRadAs 
vikingSource 
VIKINGv20130417 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hHlCorSMjRadAs 
vikingSource 
VIKINGv20140402 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hHlCorSMjRadAs 
vikingSource 
VIKINGv20150421 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.IR.H 
hHlCorSMjRadAs 
vikingSource 
VIKINGv20151230 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.IR.H 
hHlCorSMjRadAs 
vikingSource 
VIKINGv20160406 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.IR.H 
hHlCorSMjRadAs 
vikingSource 
VIKINGv20161202 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.IR.H 
hHlCorSMjRadAs 
vikingSource 
VIKINGv20170715 
Seeing corrected halflight, semimajor axis in H band 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;em.IR.H 
HIGH_BACKGROUND 
xmm3dr4 
XMM 
The flag is set to 1 (= True) if this detection comes from a field which, during manual screening, was considered to have a high background level which notably impacted on source detection. 
bit 
1 



hIntRms 
ultravistaMapLcVariability 
ULTRAVISTADR4 
Intrinsic rms in Hband 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hIntRms 
ultravistaVariability 
ULTRAVISTADR4 
Intrinsic rms in Hband 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hIntRms 
videoVariability 
VIDEODR2 
Intrinsic rms in Hband 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hIntRms 
videoVariability 
VIDEODR3 
Intrinsic rms in Hband 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.NIR 
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hIntRms 
videoVariability 
VIDEODR4 
Intrinsic rms in Hband 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hIntRms 
videoVariability 
VIDEODR5 
Intrinsic rms in Hband 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hIntRms 
videoVariability 
VIDEOv20100513 
Intrinsic rms in Hband 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hIntRms 
videoVariability 
VIDEOv20111208 
Intrinsic rms in Hband 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hIntRms 
vikingVariability 
VIKINGDR2 
Intrinsic rms in Hband 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hIntRms 
vikingVariability 
VIKINGv20110714 
Intrinsic rms in Hband 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hIntRms 
vikingVariability 
VIKINGv20111019 
Intrinsic rms in Hband 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hIntRms 
vvvVariability 
VVVDR5 
Intrinsic rms in Hband 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hIntRms 
vvvVariability 
VVVv20100531 
Intrinsic rms in Hband 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hip 
hipparcos_new_reduction 
GAIADR1 
Hipparcos identifier 
int 
4 


meta.main;meta.id 
hip 
tgas_source 
GAIADR1 
Hipparcos identifier 
int 
4 


id.cross 
hip 
tycho2 
GAIADR1 
Hipparcos number 
varchar 
16 


meta.id.cross 
hip_tyc_oid 
gaia_hip_tycho2_match 
GAIADR1 
Initial Gaia Source List identifier for Hipparcos/Tycho2 
bigint 
8 


id.cross 
hisDefAst 
ultravistaVarFrameSetInfo 
ULTRAVISTADR4 
Use a default model for the astrometric noise in H band. 
tinyint 
1 

0 
meta.code;em.IR.H 
hisDefAst 
videoVarFrameSetInfo 
VIDEODR2 
Use a default model for the astrometric noise in H band. 
tinyint 
1 

0 

hisDefAst 
videoVarFrameSetInfo 
VIDEODR3 
Use a default model for the astrometric noise in H band. 
tinyint 
1 

0 
meta.code;em.IR.NIR 
hisDefAst 
videoVarFrameSetInfo 
VIDEODR4 
Use a default model for the astrometric noise in H band. 
tinyint 
1 

0 
meta.code;em.IR.H 
hisDefAst 
videoVarFrameSetInfo 
VIDEODR5 
Use a default model for the astrometric noise in H band. 
tinyint 
1 

0 
meta.code;em.IR.H 
hisDefAst 
videoVarFrameSetInfo 
VIDEOv20111208 
Use a default model for the astrometric noise in H band. 
tinyint 
1 

0 

hisDefAst 
vikingVarFrameSetInfo 
VIKINGDR2 
Use a default model for the astrometric noise in H band. 
tinyint 
1 

0 

hisDefAst 
vikingVarFrameSetInfo 
VIKINGv20111019 
Use a default model for the astrometric noise in H band. 
tinyint 
1 

0 

hisDefAst 
vvvVarFrameSetInfo 
VVVDR5 
Use a default model for the astrometric noise in H band. 
tinyint 
1 

0 
meta.code;em.IR.H 
hisDefPht 
ultravistaMapLcVarFrameSetInfo, ultravistaVarFrameSetInfo 
ULTRAVISTADR4 
Use a default model for the photometric noise in H band. 
tinyint 
1 

0 
meta.code;em.IR.H 
hisDefPht 
videoVarFrameSetInfo 
VIDEODR2 
Use a default model for the photometric noise in H band. 
tinyint 
1 

0 

hisDefPht 
videoVarFrameSetInfo 
VIDEODR3 
Use a default model for the photometric noise in H band. 
tinyint 
1 

0 
meta.code;em.IR.NIR 
hisDefPht 
videoVarFrameSetInfo 
VIDEODR4 
Use a default model for the photometric noise in H band. 
tinyint 
1 

0 
meta.code;em.IR.H 
hisDefPht 
videoVarFrameSetInfo 
VIDEODR5 
Use a default model for the photometric noise in H band. 
tinyint 
1 

0 
meta.code;em.IR.H 
hisDefPht 
videoVarFrameSetInfo 
VIDEOv20111208 
Use a default model for the photometric noise in H band. 
tinyint 
1 

0 

hisDefPht 
vikingVarFrameSetInfo 
VIKINGDR2 
Use a default model for the photometric noise in H band. 
tinyint 
1 

0 

hisDefPht 
vikingVarFrameSetInfo 
VIKINGv20111019 
Use a default model for the photometric noise in H band. 
tinyint 
1 

0 

hisDefPht 
vvvVarFrameSetInfo 
VVVDR5 
Use a default model for the photometric noise in H band. 
tinyint 
1 

0 
meta.code;em.IR.H 
hIsMeas 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Is pass band H measured? 0 no, 1 yes 
tinyint 
1 

0 
meta.code 
hIsMeas 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20160909 
Is pass band H measured? 0 no, 1 yes 
tinyint 
1 

0 
meta.code 
hIsMeas 
vikingZY_selJ_SourceRemeasurement 
VIKINGZYSELJv20170124 
Is pass band H measured? 0 no, 1 yes 
tinyint 
1 

0 
meta.code 
hKronJky 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Extended source H calibrated flux (Kron) 
real 
4 
jansky 
0.9999995e9 
phot.flux 
hKronJkyErr 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Error in extended source H calibrated flux (Kron) 
real 
4 
janksy 
0.9999995e9 
stat.error 
hKronLup 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Extended source H luptitude (Kron) 
real 
4 
lup 
0.9999995e9 
phot.lup 
hKronLupErr 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Error in extended source H luptitude (Kron) 
real 
4 
lup 
0.9999995e9 
stat.error 
hKronMag 
ultravistaSource 
ULTRAVISTADR4 
Extended source H mag (Kron  SExtractor MAG_AUTO) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hKronMag 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Extended source H magnitude (Kron) 
real 
4 
mag 
0.9999995e9 
phot.mag 
hKronMag 
videoSource 
VIDEODR4 
Extended source H mag (Kron  SExtractor MAG_AUTO) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hKronMag 
videoSource 
VIDEODR5 
Extended source H mag (Kron  SExtractor MAG_AUTO) 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H 
hKronMagErr 
ultravistaSource 
ULTRAVISTADR4 
Extended source H mag error (Kron  SExtractor MAG_AUTO) 
real 
4 
mag 
0.9999995e9 
stat.error;phot.mag;em.IR.H 
hKronMagErr 
ultravistaSourceRemeasurement 
ULTRAVISTADR4 
Error in extended source H magnitude (Kron) 
real 
4 
mag 
0.9999995e9 
stat.error 
hKronMagErr 
videoSource 
VIDEODR4 
Extended source H mag error (Kron  SExtractor MAG_AUTO) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;phot.mag 
hKronMagErr 
videoSource 
VIDEODR5 
Extended source H mag error (Kron  SExtractor MAG_AUTO) 
real 
4 
mag 
0.9999995e9 
stat.error;em.IR.H;phot.mag 
hlCircRadAs 
sharksDetection 
SHARKSv20210222 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
sharksDetection 
SHARKSv20210421 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
ultravistaDetection 
ULTRAVISTADR4 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
ultravistaMapRemeasurement 
ULTRAVISTADR4 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total (CASU: default) 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vhsDetection 
VHSDR1 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vhsDetection 
VHSDR2 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vhsDetection 
VHSDR3 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vhsDetection 
VHSDR4 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vhsDetection 
VHSDR5 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vhsDetection 
VHSDR6 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vhsDetection 
VHSv20120926 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vhsDetection 
VHSv20130417 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vhsDetection 
VHSv20140409 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vhsDetection 
VHSv20150108 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vhsDetection 
VHSv20160114 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vhsDetection 
VHSv20160507 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vhsDetection 
VHSv20170630 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vhsDetection 
VHSv20180419 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vhsDetection 
VHSv20201209 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vhsListRemeasurement 
VHSDR1 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total flux 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
videoDetection 
VIDEODR2 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
videoDetection 
VIDEODR3 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
videoDetection 
VIDEODR4 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
videoDetection 
VIDEODR5 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
videoDetection 
VIDEOv20100513 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
videoDetection 
VIDEOv20111208 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
videoListRemeasurement 
VIDEOv20100513 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total flux 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vikingDetection 
VIKINGDR2 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vikingDetection 
VIKINGDR3 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vikingDetection 
VIKINGDR4 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vikingDetection 
VIKINGv20110714 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vikingDetection 
VIKINGv20111019 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vikingDetection 
VIKINGv20130417 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vikingDetection 
VIKINGv20140402 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vikingDetection 
VIKINGv20150421 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vikingDetection 
VIKINGv20151230 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vikingDetection 
VIKINGv20160406 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vikingDetection 
VIKINGv20161202 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vikingDetection 
VIKINGv20170715 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vikingListRemeasurement 
VIKINGv20110714 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total flux 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vikingListRemeasurement 
VIKINGv20111019 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total flux 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vikingMapRemeasurement 
VIKINGZYSELJv20160909 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total (CASU: default) 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vikingMapRemeasurement 
VIKINGZYSELJv20170124 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total (CASU: default) 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadAs 
vmcdeepDetection 
VMCDEEPv20230713 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
sharksDetection 
SHARKSv20210222 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
sharksDetection 
SHARKSv20210421 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
ultravistaDetection 
ULTRAVISTADR4 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
ultravistaMapRemeasurement 
ULTRAVISTADR4 
Error in hlCircRadAs (CASU: default) 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vhsDetection 
VHSDR2 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vhsDetection 
VHSDR3 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vhsDetection 
VHSDR4 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vhsDetection 
VHSDR5 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vhsDetection 
VHSDR6 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vhsDetection 
VHSv20120926 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vhsDetection 
VHSv20130417 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vhsDetection 
VHSv20140409 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vhsDetection 
VHSv20150108 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vhsDetection 
VHSv20160114 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vhsDetection 
VHSv20160507 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vhsDetection 
VHSv20170630 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vhsDetection 
VHSv20180419 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vhsDetection 
VHSv20201209 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vhsDetection, vhsListRemeasurement 
VHSDR1 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
videoDetection 
VIDEODR2 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
videoDetection 
VIDEODR3 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
videoDetection 
VIDEODR4 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
videoDetection 
VIDEODR5 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
videoDetection 
VIDEOv20111208 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
videoDetection, videoListRemeasurement 
VIDEOv20100513 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vikingDetection 
VIKINGDR2 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vikingDetection 
VIKINGDR3 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vikingDetection 
VIKINGDR4 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vikingDetection 
VIKINGv20111019 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vikingDetection 
VIKINGv20130417 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vikingDetection 
VIKINGv20140402 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vikingDetection 
VIKINGv20150421 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vikingDetection 
VIKINGv20151230 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vikingDetection 
VIKINGv20160406 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vikingDetection 
VIKINGv20161202 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vikingDetection 
VIKINGv20170715 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vikingDetection, vikingListRemeasurement 
VIKINGv20110714 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vikingMapRemeasurement 
VIKINGZYSELJv20160909 
Error in hlCircRadAs (CASU: default) 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vikingMapRemeasurement 
VIKINGZYSELJv20170124 
Error in hlCircRadAs (CASU: default) 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
vmcdeepDetection 
VMCDEEPv20230713 
Error in hlCircRadAs 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMjRadAs 
sharksDetection 
SHARKSv20210222 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
sharksDetection 
SHARKSv20210421 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
ultravistaDetection 
ULTRAVISTADR4 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
ultravistaMapRemeasurement 
ULTRAVISTADR4 
Seeing corrected Halflight semimajor axis (CASU: default) 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
vhsDetection 
VHSDR1 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCorSMjRadAs 
vhsDetection 
VHSDR2 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCorSMjRadAs 
vhsDetection 
VHSDR3 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
vhsDetection 
VHSDR4 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
vhsDetection 
VHSDR5 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
vhsDetection 
VHSDR6 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
vhsDetection 
VHSv20120926 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
vhsDetection 
VHSv20130417 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
vhsDetection 
VHSv20140409 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
vhsDetection 
VHSv20150108 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
vhsDetection 
VHSv20160114 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
vhsDetection 
VHSv20160507 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
vhsDetection 
VHSv20170630 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
vhsDetection 
VHSv20180419 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
vhsDetection 
VHSv20201209 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
vhsListRemeasurement 
VHSDR1 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMjRadAs 
videoDetection 
VIDEODR2 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCorSMjRadAs 
videoDetection 
VIDEODR3 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
videoDetection 
VIDEODR4 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
videoDetection 
VIDEODR5 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
videoDetection 
VIDEOv20100513 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCorSMjRadAs 
videoDetection 
VIDEOv20111208 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCorSMjRadAs 
videoListRemeasurement 
VIDEOv20100513 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMjRadAs 
vikingDetection 
VIKINGDR2 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCorSMjRadAs 
vikingDetection 
VIKINGDR3 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
vikingDetection 
VIKINGDR4 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
vikingDetection 
VIKINGv20110714 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCorSMjRadAs 
vikingDetection 
VIKINGv20111019 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCorSMjRadAs 
vikingDetection 
VIKINGv20130417 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
vikingDetection 
VIKINGv20140402 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
vikingDetection 
VIKINGv20150421 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
vikingDetection 
VIKINGv20151230 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
vikingDetection 
VIKINGv20160406 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
vikingDetection 
VIKINGv20161202 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
vikingDetection 
VIKINGv20170715 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
vikingListRemeasurement 
VIKINGv20110714 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMjRadAs 
vikingListRemeasurement 
VIKINGv20111019 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMjRadAs 
vikingMapRemeasurement 
VIKINGZYSELJv20160909 
Seeing corrected Halflight semimajor axis (CASU: default) 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
vikingMapRemeasurement 
VIKINGZYSELJv20170124 
Seeing corrected Halflight semimajor axis (CASU: default) 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMjRadAs 
vmcdeepDetection 
VMCDEEPv20230713 
Seeing corrected Halflight semimajor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMnRadAs 
sharksDetection 
SHARKSv20210222 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
sharksDetection 
SHARKSv20210421 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
ultravistaDetection 
ULTRAVISTADR4 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
ultravistaMapRemeasurement 
ULTRAVISTADR4 
Seeing corrected Halflight semiminor axis (CASU: default) 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vhsDetection 
VHSDR2 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vhsDetection 
VHSDR3 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vhsDetection 
VHSDR4 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vhsDetection 
VHSDR5 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vhsDetection 
VHSDR6 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vhsDetection 
VHSv20120926 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vhsDetection 
VHSv20130417 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vhsDetection 
VHSv20140409 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vhsDetection 
VHSv20150108 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vhsDetection 
VHSv20160114 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vhsDetection 
VHSv20160507 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vhsDetection 
VHSv20170630 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vhsDetection 
VHSv20180419 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vhsDetection 
VHSv20201209 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vhsDetection, vhsListRemeasurement 
VHSDR1 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
videoDetection 
VIDEODR2 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
videoDetection 
VIDEODR3 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
videoDetection 
VIDEODR4 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
videoDetection 
VIDEODR5 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
videoDetection 
VIDEOv20111208 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
videoDetection, videoListRemeasurement 
VIDEOv20100513 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vikingDetection 
VIKINGDR2 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vikingDetection 
VIKINGDR3 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vikingDetection 
VIKINGDR4 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vikingDetection 
VIKINGv20111019 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vikingDetection 
VIKINGv20130417 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vikingDetection 
VIKINGv20140402 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vikingDetection 
VIKINGv20150421 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vikingDetection 
VIKINGv20151230 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vikingDetection 
VIKINGv20160406 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vikingDetection 
VIKINGv20161202 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vikingDetection 
VIKINGv20170715 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vikingDetection, vikingListRemeasurement 
VIKINGv20110714 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 

hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vikingMapRemeasurement 
VIKINGZYSELJv20160909 
Seeing corrected Halflight semiminor axis (CASU: default) 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vikingMapRemeasurement 
VIKINGZYSELJv20170124 
Seeing corrected Halflight semiminor axis (CASU: default) 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMnRadAs 
vmcdeepDetection 
VMCDEEPv20230713 
Seeing corrected Halflight semiminor axis 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
sharksDetection 
SHARKSv20210222 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
sharksDetection 
SHARKSv20210421 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
ultravistaDetection 
ULTRAVISTADR4 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
ultravistaMapRemeasurement 
ULTRAVISTADR4 
Geometric halflight radius (CASU: default) 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
vhsDetection 
VHSDR2 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize;src 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
vhsDetection 
VHSDR3 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
vhsDetection 
VHSDR4 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
vhsDetection 
VHSDR5 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
vhsDetection 
VHSDR6 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
vhsDetection 
VHSv20120926 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
vhsDetection 
VHSv20130417 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
vhsDetection 
VHSv20140409 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
vhsDetection 
VHSv20150108 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
vhsDetection 
VHSv20160114 
Geometric halflight radius 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A q 