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### Glossary of VSA attributes

##### This Glossary alphabetically lists all attributes used in the VSAv20190128 database(s) held in the VSA. If you would like to have more information about the schema tables please use the VSAv20190128Schema Browser (other Browser versions).
 A B C D E F G H I J K L M N O P Q R S T U V W X Y Z

### J

NameSchema TableDatabaseDescriptionTypeLengthUnitDefault ValueUnified Content Descriptor
J twomass SIXDF J magnitude (JEXT) used for J selection real 4 mag
j_1AperMag3 vikingSource VIKINGv20151230 Default point source J_1 aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
j_1AperMag3 vikingSource VIKINGv20160406 Default point source J_1 aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
j_1AperMag3 vikingSource VIKINGv20161202 Default point source J_1 aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
j_1AperMag3 vikingSource VIKINGv20170715 Default point source J_1 aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
j_1AperMag3 vikingSource VIKINGv20181012 Default point source J_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.J
j_1AperMag3Err vikingSource VIKINGv20151230 Error in default point/extended source J_1 mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag
j_1AperMag3Err vikingSource VIKINGv20160406 Error in default point/extended source J_1 mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag
j_1AperMag3Err vikingSource VIKINGv20161202 Error in default point/extended source J_1 mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag
j_1AperMag3Err vikingSource VIKINGv20170715 Error in default point/extended source J_1 mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag
j_1AperMag3Err vikingSource VIKINGv20181012 Error in default point/extended source J_1 mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
j_1AperMag4 vikingSource VIKINGv20151230 Point source J_1 aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
j_1AperMag4 vikingSource VIKINGv20160406 Point source J_1 aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
j_1AperMag4 vikingSource VIKINGv20161202 Point source J_1 aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
j_1AperMag4 vikingSource VIKINGv20170715 Point source J_1 aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
j_1AperMag4 vikingSource VIKINGv20181012 Point source J_1 aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
j_1AperMag4Err vikingSource VIKINGv20151230 Error in point/extended source J_1 mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag
j_1AperMag4Err vikingSource VIKINGv20160406 Error in point/extended source J_1 mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag
j_1AperMag4Err vikingSource VIKINGv20161202 Error in point/extended source J_1 mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag
j_1AperMag4Err vikingSource VIKINGv20170715 Error in point/extended source J_1 mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag
j_1AperMag4Err vikingSource VIKINGv20181012 Error in point/extended source J_1 mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
j_1AperMag6 vikingSource VIKINGv20151230 Point source J_1 aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
j_1AperMag6 vikingSource VIKINGv20160406 Point source J_1 aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
j_1AperMag6 vikingSource VIKINGv20161202 Point source J_1 aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
j_1AperMag6 vikingSource VIKINGv20170715 Point source J_1 aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
j_1AperMag6 vikingSource VIKINGv20181012 Point source J_1 aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
j_1AperMag6Err vikingSource VIKINGv20151230 Error in point/extended source J_1 mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag
j_1AperMag6Err vikingSource VIKINGv20160406 Error in point/extended source J_1 mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag
j_1AperMag6Err vikingSource VIKINGv20161202 Error in point/extended source J_1 mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag
j_1AperMag6Err vikingSource VIKINGv20170715 Error in point/extended source J_1 mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag
j_1AperMag6Err vikingSource VIKINGv20181012 Error in point/extended source J_1 mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
j_1AperMagNoAperCorr3 vikingSource VIKINGv20151230 Default extended source J_1 aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
j_1AperMagNoAperCorr3 vikingSource VIKINGv20160406 Default extended source J_1 aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
j_1AperMagNoAperCorr3 vikingSource VIKINGv20161202 Default extended source J_1 aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
j_1AperMagNoAperCorr3 vikingSource VIKINGv20170715 Default extended source J_1 aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
j_1AperMagNoAperCorr3 vikingSource VIKINGv20181012 Default extended source J_1 aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
j_1AperMagNoAperCorr4 vikingSource VIKINGv20151230 Extended source J_1 aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
j_1AperMagNoAperCorr4 vikingSource VIKINGv20160406 Extended source J_1 aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
j_1AperMagNoAperCorr4 vikingSource VIKINGv20161202 Extended source J_1 aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
j_1AperMagNoAperCorr4 vikingSource VIKINGv20170715 Extended source J_1 aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
j_1AperMagNoAperCorr4 vikingSource VIKINGv20181012 Extended source J_1 aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
j_1AperMagNoAperCorr6 vikingSource VIKINGv20151230 Extended source J_1 aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
j_1AperMagNoAperCorr6 vikingSource VIKINGv20160406 Extended source J_1 aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
j_1AperMagNoAperCorr6 vikingSource VIKINGv20161202 Extended source J_1 aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
j_1AperMagNoAperCorr6 vikingSource VIKINGv20170715 Extended source J_1 aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
j_1AperMagNoAperCorr6 vikingSource VIKINGv20181012 Extended source J_1 aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
j_1AverageConf vikingSource VIKINGv20151230 average confidence in 2 arcsec diameter default aperture (aper3) J_1 real 4   -0.9999995e9 stat.likelihood
j_1AverageConf vikingSource VIKINGv20160406 average confidence in 2 arcsec diameter default aperture (aper3) J_1 real 4   -0.9999995e9 stat.likelihood
j_1AverageConf vikingSource VIKINGv20161202 average confidence in 2 arcsec diameter default aperture (aper3) J_1 real 4   -0.9999995e9 stat.likelihood
j_1AverageConf vikingSource VIKINGv20170715 average confidence in 2 arcsec diameter default aperture (aper3) J_1 real 4   -0.9999995e9 stat.likelihood
j_1AverageConf vikingSource VIKINGv20181012 average confidence in 2 arcsec diameter default aperture (aper3) J_1 real 4   -0.9999995e9 stat.likelihood;em.IR.J
j_1Class vikingSource VIKINGv20151230 discrete image classification flag in J_1 smallint 2   -9999 src.class
j_1Class vikingSource VIKINGv20160406 discrete image classification flag in J_1 smallint 2   -9999 src.class
j_1Class vikingSource VIKINGv20161202 discrete image classification flag in J_1 smallint 2   -9999 src.class
j_1Class vikingSource VIKINGv20170715 discrete image classification flag in J_1 smallint 2   -9999 src.class
j_1Class vikingSource VIKINGv20181012 discrete image classification flag in J_1 smallint 2   -9999 src.class;em.IR.J
j_1ClassStat vikingSource VIKINGv20151230 N(0,1) stellarness-of-profile statistic in J_1 real 4   -0.9999995e9 stat
j_1ClassStat vikingSource VIKINGv20160406 N(0,1) stellarness-of-profile statistic in J_1 real 4   -0.9999995e9 stat
j_1ClassStat vikingSource VIKINGv20161202 N(0,1) stellarness-of-profile statistic in J_1 real 4   -0.9999995e9 stat
j_1ClassStat vikingSource VIKINGv20170715 N(0,1) stellarness-of-profile statistic in J_1 real 4   -0.9999995e9 stat
j_1ClassStat vikingSource VIKINGv20181012 N(0,1) stellarness-of-profile statistic in J_1 real 4   -0.9999995e9 stat;em.IR.J
j_1Ell vikingSource VIKINGv20151230 1-b/a, where a/b=semi-major/minor axes in J_1 real 4   -0.9999995e9 src.ellipticity
j_1Ell vikingSource VIKINGv20160406 1-b/a, where a/b=semi-major/minor axes in J_1 real 4   -0.9999995e9 src.ellipticity
j_1Ell vikingSource VIKINGv20161202 1-b/a, where a/b=semi-major/minor axes in J_1 real 4   -0.9999995e9 src.ellipticity
j_1Ell vikingSource VIKINGv20170715 1-b/a, where a/b=semi-major/minor axes in J_1 real 4   -0.9999995e9 src.ellipticity
j_1Ell vikingSource VIKINGv20181012 1-b/a, where a/b=semi-major/minor axes in J_1 real 4   -0.9999995e9 src.ellipticity;em.IR.J
j_1eNum vikingMergeLog VIKINGv20151230 the extension number of this J_1 frame tinyint 1     meta.number
j_1eNum vikingMergeLog VIKINGv20160406 the extension number of this J_1 frame tinyint 1     meta.number
j_1eNum vikingMergeLog VIKINGv20161202 the extension number of this J_1 frame tinyint 1     meta.number
j_1eNum vikingMergeLog VIKINGv20170715 the extension number of this J_1 frame tinyint 1     meta.number
j_1eNum vikingMergeLog VIKINGv20181012 the extension number of this J_1 frame tinyint 1     meta.number;em.IR.J
j_1eNum vvvPsfDophotZYJHKsMergeLog VVVDR4 the extension number of this 1st epoch J frame tinyint 1     meta.number;em.IR.J
j_1ErrBits vikingSource VIKINGv20151230 processing warning/error bitwise flags in J_1 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.
j_1ErrBits vikingSource VIKINGv20160406 processing warning/error bitwise flags in J_1 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.
j_1ErrBits vikingSource VIKINGv20161202 processing warning/error bitwise flags in J_1 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.
j_1ErrBits vikingSource VIKINGv20170715 processing warning/error bitwise flags in J_1 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.
j_1ErrBits vikingSource VIKINGv20181012 processing warning/error bitwise flags in J_1 int 4   -99999999 meta.code;em.IR.J
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
j_1Eta vikingSource VIKINGv20151230 Offset of J_1 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.
j_1Eta vikingSource VIKINGv20160406 Offset of J_1 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.
j_1Eta vikingSource VIKINGv20161202 Offset of J_1 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.
j_1Eta vikingSource VIKINGv20170715 Offset of J_1 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.
j_1Eta vikingSource VIKINGv20181012 Offset of J_1 detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.J
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.
j_1Gausig vikingSource VIKINGv20151230 RMS of axes of ellipse fit in J_1 real 4 pixels -0.9999995e9 src.morph.param
j_1Gausig vikingSource VIKINGv20160406 RMS of axes of ellipse fit in J_1 real 4 pixels -0.9999995e9 src.morph.param
j_1Gausig vikingSource VIKINGv20161202 RMS of axes of ellipse fit in J_1 real 4 pixels -0.9999995e9 src.morph.param
j_1Gausig vikingSource VIKINGv20170715 RMS of axes of ellipse fit in J_1 real 4 pixels -0.9999995e9 src.morph.param
j_1Gausig vikingSource VIKINGv20181012 RMS of axes of ellipse fit in J_1 real 4 pixels -0.9999995e9 src.morph.param;em.IR.J
j_1HlCorSMjRadAs vikingSource VIKINGv20151230 Seeing corrected half-light, semi-major axis in J_1 band real 4 arcsec -0.9999995e9 phys.angSize
j_1HlCorSMjRadAs vikingSource VIKINGv20160406 Seeing corrected half-light, semi-major axis in J_1 band real 4 arcsec -0.9999995e9 phys.angSize
j_1HlCorSMjRadAs vikingSource VIKINGv20161202 Seeing corrected half-light, semi-major axis in J_1 band real 4 arcsec -0.9999995e9 phys.angSize
j_1HlCorSMjRadAs vikingSource VIKINGv20170715 Seeing corrected half-light, semi-major axis in J_1 band real 4 arcsec -0.9999995e9 phys.angSize
j_1HlCorSMjRadAs vikingSource VIKINGv20181012 Seeing corrected half-light, semi-major axis in J_1 band real 4 arcsec -0.9999995e9 phys.angSize;em.IR.J
j_1mfID vikingMergeLog VIKINGv20151230 the UID of the relevant J_1 multiframe bigint 8     meta.id;obs.field
j_1mfID vikingMergeLog VIKINGv20160406 the UID of the relevant J_1 multiframe bigint 8     meta.id;obs.field
j_1mfID vikingMergeLog VIKINGv20161202 the UID of the relevant J_1 multiframe bigint 8     meta.id;obs.field
j_1mfID vikingMergeLog VIKINGv20170715 the UID of the relevant J_1 multiframe bigint 8     meta.id;obs.field
j_1mfID vikingMergeLog VIKINGv20181012 the UID of the relevant J_1 multiframe bigint 8     meta.id;obs.field;em.IR.J
j_1mfID vvvPsfDophotZYJHKsMergeLog VVVDR4 the UID of the relevant 1st epoch J tile multiframe bigint 8     meta.id;obs.field;em.IR.J
j_1mhExt vikingSource VIKINGv20151230 Extended source colour J_1-H (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color;em.IR.H
Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
j_1mhExt vikingSource VIKINGv20160406 Extended source colour J_1-H (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color;em.IR.H
Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
j_1mhExt vikingSource VIKINGv20161202 Extended source colour J_1-H (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color;em.IR.H
Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
j_1mhExt vikingSource VIKINGv20170715 Extended source colour J_1-H (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color;em.IR.H
Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
j_1mhExt vikingSource VIKINGv20181012 Extended source colour J_1-H (using aperMagNoAperCorr3) real 4 mag -0.9999995e9 phot.color;em.IR.J;em.IR.H
Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
j_1mhExtErr vikingSource VIKINGv20151230 Error on extended source colour J_1-H real 4 mag -0.9999995e9 stat.error;em.IR.H
Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
j_1mhExtErr vikingSource VIKINGv20160406 Error on extended source colour J_1-H real 4 mag -0.9999995e9 stat.error;em.IR.H
Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
j_1mhExtErr vikingSource VIKINGv20161202 Error on extended source colour J_1-H real 4 mag -0.9999995e9 stat.error;em.IR.H
Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
j_1mhExtErr vikingSource VIKINGv20170715 Error on extended source colour J_1-H real 4 mag -0.9999995e9 stat.error;em.IR.H
Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
j_1mhExtErr vikingSource VIKINGv20181012 Error on extended source colour J_1-H real 4 mag -0.9999995e9 stat.error;em.IR.J;em.IR.H
Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
j_1mhPnt vikingSource VIKINGv20151230 Point source colour J_1-H (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H
Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
j_1mhPnt vikingSource VIKINGv20160406 Point source colour J_1-H (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H
Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
j_1mhPnt vikingSource VIKINGv20161202 Point source colour J_1-H (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H
Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
j_1mhPnt vikingSource VIKINGv20170715 Point source colour J_1-H (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.H
Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
j_1mhPnt vikingSource VIKINGv20181012 Point source colour J_1-H (using aperMag3) real 4 mag -0.9999995e9 phot.color;em.IR.J;em.IR.H
Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
j_1mhPntErr vikingSource VIKINGv20151230 Error on point source colour J_1-H real 4 mag -0.9999995e9 stat.error;em.IR.H
Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
j_1mhPntErr vikingSource VIKINGv20160406 Error on point source colour J_1-H real 4 mag -0.9999995e9 stat.error;em.IR.H
Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
j_1mhPntErr vikingSource VIKINGv20161202 Error on point source colour J_1-H real 4 mag -0.9999995e9 stat.error;em.IR.H
Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
j_1mhPntErr vikingSource VIKINGv20170715 Error on point source colour J_1-H real 4 mag -0.9999995e9 stat.error;em.IR.H
Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
j_1mhPntErr vikingSource VIKINGv20181012 Error on point source colour J_1-H real 4 mag -0.9999995e9 stat.error;em.IR.J;em.IR.H
Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.
j_1Mjd vikingSource VIKINGv20151230 Modified Julian Day in J_1 band float 8 days -0.9999995e9 time.epoch
j_1Mjd vikingSource VIKINGv20160406 Modified Julian Day in J_1 band float 8 days -0.9999995e9 time.epoch
j_1Mjd vikingSource VIKINGv20161202 Modified Julian Day in J_1 band float 8 days -0.9999995e9 time.epoch
j_1Mjd vikingSource VIKINGv20170715 Modified Julian Day in J_1 band float 8 days -0.9999995e9 time.epoch
j_1Mjd vikingSource VIKINGv20181012 Modified Julian Day in J_1 band float 8 days -0.9999995e9 time.epoch;em.IR.J
j_1Mjd vvvPsfDophotZYJHKsMergeLog VVVDR4 the MJD of the 1st epoch J tile multiframe float 8     time;em.IR.J
j_1PA vikingSource VIKINGv20151230 ellipse fit celestial orientation in J_1 real 4 Degrees -0.9999995e9 pos.posAng
j_1PA vikingSource VIKINGv20160406 ellipse fit celestial orientation in J_1 real 4 Degrees -0.9999995e9 pos.posAng
j_1PA vikingSource VIKINGv20161202 ellipse fit celestial orientation in J_1 real 4 Degrees -0.9999995e9 pos.posAng
j_1PA vikingSource VIKINGv20170715 ellipse fit celestial orientation in J_1 real 4 Degrees -0.9999995e9 pos.posAng
j_1PA vikingSource VIKINGv20181012 ellipse fit celestial orientation in J_1 real 4 Degrees -0.9999995e9 pos.posAng;em.IR.J
j_1PetroMag vikingSource VIKINGv20151230 Extended source J_1 mag (Petrosian) real 4 mag -0.9999995e9 phot.mag
j_1PetroMag vikingSource VIKINGv20160406 Extended source J_1 mag (Petrosian) real 4 mag -0.9999995e9 phot.mag
j_1PetroMag vikingSource VIKINGv20161202 Extended source J_1 mag (Petrosian) real 4 mag -0.9999995e9 phot.mag
j_1PetroMag vikingSource VIKINGv20170715 Extended source J_1 mag (Petrosian) real 4 mag -0.9999995e9 phot.mag
j_1PetroMag vikingSource VIKINGv20181012 Extended source J_1 mag (Petrosian) real 4 mag -0.9999995e9 phot.mag;em.IR.J
j_1PetroMagErr vikingSource VIKINGv20151230 Error in extended source J_1 mag (Petrosian) real 4 mag -0.9999995e9 stat.error;phot.mag
j_1PetroMagErr vikingSource VIKINGv20160406 Error in extended source J_1 mag (Petrosian) real 4 mag -0.9999995e9 stat.error;phot.mag
j_1PetroMagErr vikingSource VIKINGv20161202 Error in extended source J_1 mag (Petrosian) real 4 mag -0.9999995e9 stat.error;phot.mag
j_1PetroMagErr vikingSource VIKINGv20170715 Error in extended source J_1 mag (Petrosian) real 4 mag -0.9999995e9 stat.error;phot.mag
j_1PetroMagErr vikingSource VIKINGv20181012 Error in extended source J_1 mag (Petrosian) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
j_1ppErrBits vikingSource VIKINGv20151230 additional WFAU post-processing error bits in J_1 int 4   0 meta.code
Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:
 Byte Bit Detection quality issue Threshold or bit mask Applies to Decimal Hexadecimal 0 4 Deblended 16 0x00000010 All VDFS catalogues 0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues 0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues 1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles 2 16 Close to saturated 65536 0x00010000 All VDFS catalogues 2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only 2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues 2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles 3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.
j_1ppErrBits vikingSource VIKINGv20160406 additional WFAU post-processing error bits in J_1 int 4   0 meta.code
Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:
 Byte Bit Detection quality issue Threshold or bit mask Applies to Decimal Hexadecimal 0 4 Deblended 16 0x00000010 All VDFS catalogues 0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues 0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues 1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles 2 16 Close to saturated 65536 0x00010000 All VDFS catalogues 2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only 2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues 2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles 3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.
j_1ppErrBits vikingSource VIKINGv20161202 additional WFAU post-processing error bits in J_1 int 4   0 meta.code
Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:
 Byte Bit Detection quality issue Threshold or bit mask Applies to Decimal Hexadecimal 0 4 Deblended 16 0x00000010 All VDFS catalogues 0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues 0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues 1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles 2 16 Close to saturated 65536 0x00010000 All VDFS catalogues 2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only 2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues 2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles 3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.
j_1ppErrBits vikingSource VIKINGv20170715 additional WFAU post-processing error bits in J_1 int 4   0 meta.code
Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:
 Byte Bit Detection quality issue Threshold or bit mask Applies to Decimal Hexadecimal 0 4 Deblended 16 0x00000010 All VDFS catalogues 0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues 0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues 1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles 2 16 Close to saturated 65536 0x00010000 All VDFS catalogues 2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only 2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues 2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles 3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.
j_1ppErrBits vikingSource VIKINGv20181012 additional WFAU post-processing error bits in J_1 int 4   0 meta.code;em.IR.J
Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:
 Byte Bit Detection quality issue Threshold or bit mask Applies to Decimal Hexadecimal 0 4 Deblended 16 0x00000010 All VDFS catalogues 0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues 0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues 1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles 2 16 Close to saturated 65536 0x00010000 All VDFS catalogues 2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only 2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues 2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles 3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.
j_1PsfMag vikingSource VIKINGv20151230 Point source profile-fitted J_1 mag real 4 mag -0.9999995e9 phot.mag
j_1PsfMag vikingSource VIKINGv20160406 Point source profile-fitted J_1 mag real 4 mag -0.9999995e9 phot.mag
j_1PsfMag vikingSource VIKINGv20161202 Point source profile-fitted J_1 mag real 4 mag -0.9999995e9 phot.mag
j_1PsfMag vikingSource VIKINGv20170715 Point source profile-fitted J_1 mag real 4 mag -0.9999995e9 phot.mag
j_1PsfMag vikingSource VIKINGv20181012 Point source profile-fitted J_1 mag real 4 mag -0.9999995e9 phot.mag;em.IR.J
j_1PsfMagErr vikingSource VIKINGv20151230 Error in point source profile-fitted J_1 mag real 4 mag -0.9999995e9 stat.error;phot.mag
j_1PsfMagErr vikingSource VIKINGv20160406 Error in point source profile-fitted J_1 mag real 4 mag -0.9999995e9 stat.error;phot.mag
j_1PsfMagErr vikingSource VIKINGv20161202 Error in point source profile-fitted J_1 mag real 4 mag -0.9999995e9 stat.error;phot.mag
j_1PsfMagErr vikingSource VIKINGv20170715 Error in point source profile-fitted J_1 mag real 4 mag -0.9999995e9 stat.error;phot.mag
j_1PsfMagErr vikingSource VIKINGv20181012 Error in point source profile-fitted J_1 mag real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
j_1SeqNum vikingSource VIKINGv20151230 the running number of the J_1 detection int 4   -99999999 meta.number
j_1SeqNum vikingSource VIKINGv20160406 the running number of the J_1 detection int 4   -99999999 meta.number
j_1SeqNum vikingSource VIKINGv20161202 the running number of the J_1 detection int 4   -99999999 meta.number
j_1SeqNum vikingSource VIKINGv20170715 the running number of the J_1 detection int 4   -99999999 meta.number
j_1SeqNum vikingSource VIKINGv20181012 the running number of the J_1 detection int 4   -99999999 meta.number;em.IR.J
j_1SerMag2D vikingSource VIKINGv20151230 Extended source J_1 mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag
j_1SerMag2D vikingSource VIKINGv20160406 Extended source J_1 mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag
j_1SerMag2D vikingSource VIKINGv20161202 Extended source J_1 mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag
j_1SerMag2D vikingSource VIKINGv20170715 Extended source J_1 mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag
j_1SerMag2D vikingSource VIKINGv20181012 Extended source J_1 mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag;em.IR.J
j_1SerMag2DErr vikingSource VIKINGv20151230 Error in extended source J_1 mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;phot.mag
j_1SerMag2DErr vikingSource VIKINGv20160406 Error in extended source J_1 mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;phot.mag
j_1SerMag2DErr vikingSource VIKINGv20161202 Error in extended source J_1 mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;phot.mag
j_1SerMag2DErr vikingSource VIKINGv20170715 Error in extended source J_1 mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;phot.mag
j_1SerMag2DErr vikingSource VIKINGv20181012 Error in extended source J_1 mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
j_1Xi vikingSource VIKINGv20151230 Offset of J_1 detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;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.
j_1Xi vikingSource VIKINGv20160406 Offset of J_1 detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;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.
j_1Xi vikingSource VIKINGv20161202 Offset of J_1 detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;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.
j_1Xi vikingSource VIKINGv20170715 Offset of J_1 detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;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.
j_1Xi vikingSource VIKINGv20181012 Offset of J_1 detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff;em.IR.J
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.
j_2AperMag3 vikingSource VIKINGv20151230 Default point source J_2 aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
j_2AperMag3 vikingSource VIKINGv20160406 Default point source J_2 aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
j_2AperMag3 vikingSource VIKINGv20161202 Default point source J_2 aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
j_2AperMag3 vikingSource VIKINGv20170715 Default point source J_2 aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
j_2AperMag3 vikingSource VIKINGv20181012 Default point source J_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.J
j_2AperMag3Err vikingSource VIKINGv20151230 Error in default point/extended source J_2 mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag
j_2AperMag3Err vikingSource VIKINGv20160406 Error in default point/extended source J_2 mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag
j_2AperMag3Err vikingSource VIKINGv20161202 Error in default point/extended source J_2 mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag
j_2AperMag3Err vikingSource VIKINGv20170715 Error in default point/extended source J_2 mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag
j_2AperMag3Err vikingSource VIKINGv20181012 Error in default point/extended source J_2 mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
j_2AperMag4 vikingSource VIKINGv20151230 Point source J_2 aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
j_2AperMag4 vikingSource VIKINGv20160406 Point source J_2 aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
j_2AperMag4 vikingSource VIKINGv20161202 Point source J_2 aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
j_2AperMag4 vikingSource VIKINGv20170715 Point source J_2 aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
j_2AperMag4 vikingSource VIKINGv20181012 Point source J_2 aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
j_2AperMag4Err vikingSource VIKINGv20151230 Error in point/extended source J_2 mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag
j_2AperMag4Err vikingSource VIKINGv20160406 Error in point/extended source J_2 mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag
j_2AperMag4Err vikingSource VIKINGv20161202 Error in point/extended source J_2 mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag
j_2AperMag4Err vikingSource VIKINGv20170715 Error in point/extended source J_2 mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag
j_2AperMag4Err vikingSource VIKINGv20181012 Error in point/extended source J_2 mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
j_2AperMag6 vikingSource VIKINGv20151230 Point source J_2 aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
j_2AperMag6 vikingSource VIKINGv20160406 Point source J_2 aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
j_2AperMag6 vikingSource VIKINGv20161202 Point source J_2 aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
j_2AperMag6 vikingSource VIKINGv20170715 Point source J_2 aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
j_2AperMag6 vikingSource VIKINGv20181012 Point source J_2 aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
j_2AperMag6Err vikingSource VIKINGv20151230 Error in point/extended source J_2 mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag
j_2AperMag6Err vikingSource VIKINGv20160406 Error in point/extended source J_2 mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag
j_2AperMag6Err vikingSource VIKINGv20161202 Error in point/extended source J_2 mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag
j_2AperMag6Err vikingSource VIKINGv20170715 Error in point/extended source J_2 mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag
j_2AperMag6Err vikingSource VIKINGv20181012 Error in point/extended source J_2 mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
j_2AperMagNoAperCorr3 vikingSource VIKINGv20151230 Default extended source J_2 aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
j_2AperMagNoAperCorr3 vikingSource VIKINGv20160406 Default extended source J_2 aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
j_2AperMagNoAperCorr3 vikingSource VIKINGv20161202 Default extended source J_2 aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
j_2AperMagNoAperCorr3 vikingSource VIKINGv20170715 Default extended source J_2 aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
j_2AperMagNoAperCorr3 vikingSource VIKINGv20181012 Default extended source J_2 aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
j_2AperMagNoAperCorr4 vikingSource VIKINGv20151230 Extended source J_2 aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
j_2AperMagNoAperCorr4 vikingSource VIKINGv20160406 Extended source J_2 aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
j_2AperMagNoAperCorr4 vikingSource VIKINGv20161202 Extended source J_2 aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
j_2AperMagNoAperCorr4 vikingSource VIKINGv20170715 Extended source J_2 aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
j_2AperMagNoAperCorr4 vikingSource VIKINGv20181012 Extended source J_2 aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
j_2AperMagNoAperCorr6 vikingSource VIKINGv20151230 Extended source J_2 aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
j_2AperMagNoAperCorr6 vikingSource VIKINGv20160406 Extended source J_2 aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
j_2AperMagNoAperCorr6 vikingSource VIKINGv20161202 Extended source J_2 aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
j_2AperMagNoAperCorr6 vikingSource VIKINGv20170715 Extended source J_2 aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
j_2AperMagNoAperCorr6 vikingSource VIKINGv20181012 Extended source J_2 aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
j_2AverageConf vikingSource VIKINGv20151230 average confidence in 2 arcsec diameter default aperture (aper3) J_2 real 4   -0.9999995e9 stat.likelihood
j_2AverageConf vikingSource VIKINGv20160406 average confidence in 2 arcsec diameter default aperture (aper3) J_2 real 4   -0.9999995e9 stat.likelihood
j_2AverageConf vikingSource VIKINGv20161202 average confidence in 2 arcsec diameter default aperture (aper3) J_2 real 4   -0.9999995e9 stat.likelihood
j_2AverageConf vikingSource VIKINGv20170715 average confidence in 2 arcsec diameter default aperture (aper3) J_2 real 4   -0.9999995e9 stat.likelihood
j_2AverageConf vikingSource VIKINGv20181012 average confidence in 2 arcsec diameter default aperture (aper3) J_2 real 4   -0.9999995e9 stat.likelihood;em.IR.J
j_2Class vikingSource VIKINGv20151230 discrete image classification flag in J_2 smallint 2   -9999 src.class
j_2Class vikingSource VIKINGv20160406 discrete image classification flag in J_2 smallint 2   -9999 src.class
j_2Class vikingSource VIKINGv20161202 discrete image classification flag in J_2 smallint 2   -9999 src.class
j_2Class vikingSource VIKINGv20170715 discrete image classification flag in J_2 smallint 2   -9999 src.class
j_2Class vikingSource VIKINGv20181012 discrete image classification flag in J_2 smallint 2   -9999 src.class;em.IR.J
j_2ClassStat vikingSource VIKINGv20151230 N(0,1) stellarness-of-profile statistic in J_2 real 4   -0.9999995e9 stat
j_2ClassStat vikingSource VIKINGv20160406 N(0,1) stellarness-of-profile statistic in J_2 real 4   -0.9999995e9 stat
j_2ClassStat vikingSource VIKINGv20161202 N(0,1) stellarness-of-profile statistic in J_2 real 4   -0.9999995e9 stat
j_2ClassStat vikingSource VIKINGv20170715 N(0,1) stellarness-of-profile statistic in J_2 real 4   -0.9999995e9 stat
j_2ClassStat vikingSource VIKINGv20181012 N(0,1) stellarness-of-profile statistic in J_2 real 4   -0.9999995e9 stat;em.IR.J
j_2Ell vikingSource VIKINGv20151230 1-b/a, where a/b=semi-major/minor axes in J_2 real 4   -0.9999995e9 src.ellipticity
j_2Ell vikingSource VIKINGv20160406 1-b/a, where a/b=semi-major/minor axes in J_2 real 4   -0.9999995e9 src.ellipticity
j_2Ell vikingSource VIKINGv20161202 1-b/a, where a/b=semi-major/minor axes in J_2 real 4   -0.9999995e9 src.ellipticity
j_2Ell vikingSource VIKINGv20170715 1-b/a, where a/b=semi-major/minor axes in J_2 real 4   -0.9999995e9 src.ellipticity
j_2Ell vikingSource VIKINGv20181012 1-b/a, where a/b=semi-major/minor axes in J_2 real 4   -0.9999995e9 src.ellipticity;em.IR.J
j_2eNum vikingMergeLog VIKINGv20151230 the extension number of this J_2 frame tinyint 1     meta.number
j_2eNum vikingMergeLog VIKINGv20160406 the extension number of this J_2 frame tinyint 1     meta.number
j_2eNum vikingMergeLog VIKINGv20161202 the extension number of this J_2 frame tinyint 1     meta.number
j_2eNum vikingMergeLog VIKINGv20170715 the extension number of this J_2 frame tinyint 1     meta.number
j_2eNum vikingMergeLog VIKINGv20181012 the extension number of this J_2 frame tinyint 1     meta.number;em.IR.J
j_2eNum vvvPsfDophotZYJHKsMergeLog VVVDR4 the extension number of this 2nd epoch J frame tinyint 1     meta.number;em.IR.J
j_2ErrBits vikingSource VIKINGv20151230 processing warning/error bitwise flags in J_2 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.
j_2ErrBits vikingSource VIKINGv20160406 processing warning/error bitwise flags in J_2 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.
j_2ErrBits vikingSource VIKINGv20161202 processing warning/error bitwise flags in J_2 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.
j_2ErrBits vikingSource VIKINGv20170715 processing warning/error bitwise flags in J_2 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.
j_2ErrBits vikingSource VIKINGv20181012 processing warning/error bitwise flags in J_2 int 4   -99999999 meta.code;em.IR.J
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
j_2Eta vikingSource VIKINGv20151230 Offset of J_2 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.
j_2Eta vikingSource VIKINGv20160406 Offset of J_2 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.
j_2Eta vikingSource VIKINGv20161202 Offset of J_2 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.
j_2Eta vikingSource VIKINGv20170715 Offset of J_2 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.
j_2Eta vikingSource VIKINGv20181012 Offset of J_2 detection from master position (+north/-south) real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff;em.IR.J
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.
j_2Gausig vikingSource VIKINGv20151230 RMS of axes of ellipse fit in J_2 real 4 pixels -0.9999995e9 src.morph.param
j_2Gausig vikingSource VIKINGv20160406 RMS of axes of ellipse fit in J_2 real 4 pixels -0.9999995e9 src.morph.param
j_2Gausig vikingSource VIKINGv20161202 RMS of axes of ellipse fit in J_2 real 4 pixels -0.9999995e9 src.morph.param
j_2Gausig vikingSource VIKINGv20170715 RMS of axes of ellipse fit in J_2 real 4 pixels -0.9999995e9 src.morph.param
j_2Gausig vikingSource VIKINGv20181012 RMS of axes of ellipse fit in J_2 real 4 pixels -0.9999995e9 src.morph.param;em.IR.J
j_2HlCorSMjRadAs vikingSource VIKINGv20151230 Seeing corrected half-light, semi-major axis in J_2 band real 4 arcsec -0.9999995e9 phys.angSize
j_2HlCorSMjRadAs vikingSource VIKINGv20160406 Seeing corrected half-light, semi-major axis in J_2 band real 4 arcsec -0.9999995e9 phys.angSize
j_2HlCorSMjRadAs vikingSource VIKINGv20161202 Seeing corrected half-light, semi-major axis in J_2 band real 4 arcsec -0.9999995e9 phys.angSize
j_2HlCorSMjRadAs vikingSource VIKINGv20170715 Seeing corrected half-light, semi-major axis in J_2 band real 4 arcsec -0.9999995e9 phys.angSize
j_2HlCorSMjRadAs vikingSource VIKINGv20181012 Seeing corrected half-light, semi-major axis in J_2 band real 4 arcsec -0.9999995e9 phys.angSize;em.IR.J
j_2mfID vikingMergeLog VIKINGv20151230 the UID of the relevant J_2 multiframe bigint 8     meta.id;obs.field
j_2mfID vikingMergeLog VIKINGv20160406 the UID of the relevant J_2 multiframe bigint 8     meta.id;obs.field
j_2mfID vikingMergeLog VIKINGv20161202 the UID of the relevant J_2 multiframe bigint 8     meta.id;obs.field
j_2mfID vikingMergeLog VIKINGv20170715 the UID of the relevant J_2 multiframe bigint 8     meta.id;obs.field
j_2mfID vikingMergeLog VIKINGv20181012 the UID of the relevant J_2 multiframe bigint 8     meta.id;obs.field;em.IR.J
j_2mfID vvvPsfDophotZYJHKsMergeLog VVVDR4 the UID of the relevant 2nd epoch J tile multiframe bigint 8     meta.id;obs.field;em.IR.J
j_2Mjd vikingSource VIKINGv20151230 Modified Julian Day in J_2 band float 8 days -0.9999995e9 time.epoch
j_2Mjd vikingSource VIKINGv20160406 Modified Julian Day in J_2 band float 8 days -0.9999995e9 time.epoch
j_2Mjd vikingSource VIKINGv20161202 Modified Julian Day in J_2 band float 8 days -0.9999995e9 time.epoch
j_2Mjd vikingSource VIKINGv20170715 Modified Julian Day in J_2 band float 8 days -0.9999995e9 time.epoch
j_2Mjd vikingSource VIKINGv20181012 Modified Julian Day in J_2 band float 8 days -0.9999995e9 time.epoch;em.IR.J
j_2Mjd vvvPsfDophotZYJHKsMergeLog VVVDR4 the MJD of the 2nd epoch J tile multiframe float 8     time;em.IR.J
j_2mrat twomass_scn TWOMASS J-band average 2nd image moment ratio. real 4     stat.fit.param
j_2mrat twomass_sixx2_scn TWOMASS J band average 2nd image moment ratio for scan real 4
j_2PA vikingSource VIKINGv20151230 ellipse fit celestial orientation in J_2 real 4 Degrees -0.9999995e9 pos.posAng
j_2PA vikingSource VIKINGv20160406 ellipse fit celestial orientation in J_2 real 4 Degrees -0.9999995e9 pos.posAng
j_2PA vikingSource VIKINGv20161202 ellipse fit celestial orientation in J_2 real 4 Degrees -0.9999995e9 pos.posAng
j_2PA vikingSource VIKINGv20170715 ellipse fit celestial orientation in J_2 real 4 Degrees -0.9999995e9 pos.posAng
j_2PA vikingSource VIKINGv20181012 ellipse fit celestial orientation in J_2 real 4 Degrees -0.9999995e9 pos.posAng;em.IR.J
j_2PetroMag vikingSource VIKINGv20151230 Extended source J_2 mag (Petrosian) real 4 mag -0.9999995e9 phot.mag
j_2PetroMag vikingSource VIKINGv20160406 Extended source J_2 mag (Petrosian) real 4 mag -0.9999995e9 phot.mag
j_2PetroMag vikingSource VIKINGv20161202 Extended source J_2 mag (Petrosian) real 4 mag -0.9999995e9 phot.mag
j_2PetroMag vikingSource VIKINGv20170715 Extended source J_2 mag (Petrosian) real 4 mag -0.9999995e9 phot.mag
j_2PetroMag vikingSource VIKINGv20181012 Extended source J_2 mag (Petrosian) real 4 mag -0.9999995e9 phot.mag;em.IR.J
j_2PetroMagErr vikingSource VIKINGv20151230 Error in extended source J_2 mag (Petrosian) real 4 mag -0.9999995e9 stat.error;phot.mag
j_2PetroMagErr vikingSource VIKINGv20160406 Error in extended source J_2 mag (Petrosian) real 4 mag -0.9999995e9 stat.error;phot.mag
j_2PetroMagErr vikingSource VIKINGv20161202 Error in extended source J_2 mag (Petrosian) real 4 mag -0.9999995e9 stat.error;phot.mag
j_2PetroMagErr vikingSource VIKINGv20170715 Error in extended source J_2 mag (Petrosian) real 4 mag -0.9999995e9 stat.error;phot.mag
j_2PetroMagErr vikingSource VIKINGv20181012 Error in extended source J_2 mag (Petrosian) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
j_2ppErrBits vikingSource VIKINGv20151230 additional WFAU post-processing error bits in J_2 int 4   0 meta.code
Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:
 Byte Bit Detection quality issue Threshold or bit mask Applies to Decimal Hexadecimal 0 4 Deblended 16 0x00000010 All VDFS catalogues 0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues 0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues 1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles 2 16 Close to saturated 65536 0x00010000 All VDFS catalogues 2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only 2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues 2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles 3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.
j_2ppErrBits vikingSource VIKINGv20160406 additional WFAU post-processing error bits in J_2 int 4   0 meta.code
Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:
 Byte Bit Detection quality issue Threshold or bit mask Applies to Decimal Hexadecimal 0 4 Deblended 16 0x00000010 All VDFS catalogues 0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues 0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues 1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles 2 16 Close to saturated 65536 0x00010000 All VDFS catalogues 2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only 2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues 2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles 3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.
j_2ppErrBits vikingSource VIKINGv20161202 additional WFAU post-processing error bits in J_2 int 4   0 meta.code
Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:
 Byte Bit Detection quality issue Threshold or bit mask Applies to Decimal Hexadecimal 0 4 Deblended 16 0x00000010 All VDFS catalogues 0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues 0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues 1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles 2 16 Close to saturated 65536 0x00010000 All VDFS catalogues 2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only 2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues 2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles 3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.
j_2ppErrBits vikingSource VIKINGv20170715 additional WFAU post-processing error bits in J_2 int 4   0 meta.code
Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:
 Byte Bit Detection quality issue Threshold or bit mask Applies to Decimal Hexadecimal 0 4 Deblended 16 0x00000010 All VDFS catalogues 0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues 0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues 1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles 2 16 Close to saturated 65536 0x00010000 All VDFS catalogues 2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only 2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues 2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles 3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.
j_2ppErrBits vikingSource VIKINGv20181012 additional WFAU post-processing error bits in J_2 int 4   0 meta.code;em.IR.J
Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:
 Byte Bit Detection quality issue Threshold or bit mask Applies to Decimal Hexadecimal 0 4 Deblended 16 0x00000010 All VDFS catalogues 0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues 0 7 Low confidence in default aperture 128 0x00000080 All VDFS catalogues 1 12 Lies within detector 16 region of a tile 4096 0x00001000 All catalogues from tiles 2 16 Close to saturated 65536 0x00010000 All VDFS catalogues 2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only 2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues 2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles 3 24 Lies within an underexposed region of a tile due to missing detector 16777216 0x01000000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.
j_2PsfMag vikingSource VIKINGv20151230 Point source profile-fitted J_2 mag real 4 mag -0.9999995e9 phot.mag
j_2PsfMag vikingSource VIKINGv20160406 Point source profile-fitted J_2 mag real 4 mag -0.9999995e9 phot.mag
j_2PsfMag vikingSource VIKINGv20161202 Point source profile-fitted J_2 mag real 4 mag -0.9999995e9 phot.mag
j_2PsfMag vikingSource VIKINGv20170715 Point source profile-fitted J_2 mag real 4 mag -0.9999995e9 phot.mag
j_2PsfMag vikingSource VIKINGv20181012 Point source profile-fitted J_2 mag real 4 mag -0.9999995e9 phot.mag;em.IR.J
j_2PsfMagErr vikingSource VIKINGv20151230 Error in point source profile-fitted J_2 mag real 4 mag -0.9999995e9 stat.error;phot.mag
j_2PsfMagErr vikingSource VIKINGv20160406 Error in point source profile-fitted J_2 mag real 4 mag -0.9999995e9 stat.error;phot.mag
j_2PsfMagErr vikingSource VIKINGv20161202 Error in point source profile-fitted J_2 mag real 4 mag -0.9999995e9 stat.error;phot.mag
j_2PsfMagErr vikingSource VIKINGv20170715 Error in point source profile-fitted J_2 mag real 4 mag -0.9999995e9 stat.error;phot.mag
j_2PsfMagErr vikingSource VIKINGv20181012 Error in point source profile-fitted J_2 mag real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
j_2SeqNum vikingSource VIKINGv20151230 the running number of the J_2 detection int 4   -99999999 meta.number
j_2SeqNum vikingSource VIKINGv20160406 the running number of the J_2 detection int 4   -99999999 meta.number
j_2SeqNum vikingSource VIKINGv20161202 the running number of the J_2 detection int 4   -99999999 meta.number
j_2SeqNum vikingSource VIKINGv20170715 the running number of the J_2 detection int 4   -99999999 meta.number
j_2SeqNum vikingSource VIKINGv20181012 the running number of the J_2 detection int 4   -99999999 meta.number;em.IR.J
j_2SerMag2D vikingSource VIKINGv20151230 Extended source J_2 mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag
j_2SerMag2D vikingSource VIKINGv20160406 Extended source J_2 mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag
j_2SerMag2D vikingSource VIKINGv20161202 Extended source J_2 mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag
j_2SerMag2D vikingSource VIKINGv20170715 Extended source J_2 mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag
j_2SerMag2D vikingSource VIKINGv20181012 Extended source J_2 mag (profile-fitted) real 4 mag -0.9999995e9 phot.mag;em.IR.J
j_2SerMag2DErr vikingSource VIKINGv20151230 Error in extended source J_2 mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;phot.mag
j_2SerMag2DErr vikingSource VIKINGv20160406 Error in extended source J_2 mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;phot.mag
j_2SerMag2DErr vikingSource VIKINGv20161202 Error in extended source J_2 mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;phot.mag
j_2SerMag2DErr vikingSource VIKINGv20170715 Error in extended source J_2 mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;phot.mag
j_2SerMag2DErr vikingSource VIKINGv20181012 Error in extended source J_2 mag (profile-fitted) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
j_2Xi vikingSource VIKINGv20151230 Offset of J_2 detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;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.
j_2Xi vikingSource VIKINGv20160406 Offset of J_2 detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;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.
j_2Xi vikingSource VIKINGv20161202 Offset of J_2 detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;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.
j_2Xi vikingSource VIKINGv20170715 Offset of J_2 detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;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.
j_2Xi vikingSource VIKINGv20181012 Offset of J_2 detection from master position (+east/-west) real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff;em.IR.J
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.
j_5sig_ba twomass_xsc TWOMASS J minor/major axis ratio fit to the 5-sigma isophote. real 4     phys.size.axisRatio
j_5sig_phi twomass_xsc TWOMASS J angle to 5-sigma major axis (E of N). smallint 2 degrees   stat.error
j_5surf twomass_xsc TWOMASS J central surface brightness (r<=5). real 4 mag   phot.mag.sb
j_ba twomass_xsc TWOMASS J minor/major axis ratio fit to the 3-sigma isophote. real 4     phys.size.axisRatio
j_back twomass_xsc TWOMASS J coadd median background. real 4     meta.code
j_bisym_chi twomass_xsc TWOMASS J bi-symmetric cross-correlation chi. real 4     stat.fit.param
j_bisym_rat twomass_xsc TWOMASS J bi-symmetric flux ratio. real 4     phot.flux;arith.ratio
j_bndg_amp twomass_xsc TWOMASS J banding maximum FT amplitude on this side of coadd. real 4 DN   stat.fit.param
j_bndg_per twomass_xsc TWOMASS J banding Fourier Transf. period on this side of coadd. int 4 arcsec   stat.fit.param
j_chif_ellf twomass_xsc TWOMASS J % chi-fraction for elliptical fit to 3-sig isophote. real 4     stat.fit.param
j_cmsig twomass_psc TWOMASS Corrected photometric uncertainty for the default J-band magnitude. real 4 mag J-band phot.flux
j_con_indx twomass_xsc TWOMASS J concentration index r_75%/r_25%. real 4     phys.size;arith.ratio
j_d_area twomass_xsc TWOMASS J 5-sigma to 3-sigma differential area. smallint 2     stat.fit.residual
j_flg_10 twomass_xsc TWOMASS J confusion flag for 10 arcsec circular ap. mag. smallint 2     meta.code
j_flg_15 twomass_xsc TWOMASS J confusion flag for 15 arcsec circular ap. mag. smallint 2     meta.code
j_flg_20 twomass_xsc TWOMASS J confusion flag for 20 arcsec circular ap. mag. smallint 2     meta.code
j_flg_25 twomass_xsc TWOMASS J confusion flag for 25 arcsec circular ap. mag. smallint 2     meta.code
j_flg_30 twomass_xsc TWOMASS J confusion flag for 30 arcsec circular ap. mag. smallint 2     meta.code
j_flg_40 twomass_xsc TWOMASS J confusion flag for 40 arcsec circular ap. mag. smallint 2     meta.code
j_flg_5 twomass_xsc TWOMASS J confusion flag for 5 arcsec circular ap. mag. smallint 2     meta.code
j_flg_50 twomass_xsc TWOMASS J confusion flag for 50 arcsec circular ap. mag. smallint 2     meta.code
j_flg_60 twomass_xsc TWOMASS J confusion flag for 60 arcsec circular ap. mag. smallint 2     meta.code
j_flg_7 twomass_sixx2_xsc TWOMASS J confusion flag for 7 arcsec circular ap. mag smallint 2
j_flg_7 twomass_xsc TWOMASS J confusion flag for 7 arcsec circular ap. mag. smallint 2     meta.code
j_flg_70 twomass_xsc TWOMASS J confusion flag for 70 arcsec circular ap. mag. smallint 2     meta.code
j_flg_c twomass_xsc TWOMASS J confusion flag for Kron circular mag. smallint 2     meta.code
j_flg_e twomass_xsc TWOMASS J confusion flag for Kron elliptical mag. smallint 2     meta.code
j_flg_fc twomass_xsc TWOMASS J confusion flag for fiducial Kron circ. mag. smallint 2     meta.code
j_flg_fe twomass_xsc TWOMASS J confusion flag for fiducial Kron ell. mag. smallint 2     meta.code
j_flg_i20c twomass_xsc TWOMASS J confusion flag for 20mag/sq." iso. circ. mag. smallint 2     meta.code
j_flg_i20e twomass_xsc TWOMASS J confusion flag for 20mag/sq." iso. ell. mag. smallint 2     meta.code
j_flg_i21c twomass_xsc TWOMASS J confusion flag for 21mag/sq." iso. circ. mag. smallint 2     meta.code
j_flg_i21e twomass_xsc TWOMASS J confusion flag for 21mag/sq." iso. ell. mag. smallint 2     meta.code
j_flg_j21fc twomass_xsc TWOMASS J confusion flag for 21mag/sq." iso. fid. circ. mag. smallint 2     meta.code
j_flg_j21fe twomass_xsc TWOMASS J confusion flag for 21mag/sq." iso. fid. ell. mag. smallint 2     meta.code
j_flg_k20fc twomass_xsc TWOMASS J confusion flag for 20mag/sq." iso. fid. circ. mag. smallint 2     meta.code
j_flg_k20fe twomass_sixx2_xsc TWOMASS J confusion flag for 20mag/sq.″ iso. fid. ell. mag smallint 2
j_flg_k20fe twomass_xsc TWOMASS J confusion flag for 20mag/sq." iso. fid. ell. mag. smallint 2     meta.code
j_h twomass_sixx2_psc TWOMASS The J-H color, computed from the J-band and H-band magnitudes (j_m and h_m, respectively) of the source. In cases where the first or second digit in rd_flg is equal to either "0", "4", "6", or "9", no color is computed because the photometry in one or both bands is of lower quality or the source is not detected. real 4
j_k twomass_sixx2_psc TWOMASS The J-Ks color, computed from the J-band and Ks-band magnitudes (j_m and k_m, respectively) of the source. In cases where the first or third digit in rd_flg is equal to either "0", "4", "6", or "9", no color is computed because the photometry in one or both bands is of lower quality or the source is not detected. real 4
j_m twomass_psc TWOMASS Default J-band magnitude real 4 mag   phot.flux
j_m twomass_sixx2_psc TWOMASS J selected "default" magnitude real 4 mag
j_m_10 twomass_xsc TWOMASS J 10 arcsec radius circular aperture magnitude. real 4 mag   phot.flux
j_m_15 twomass_xsc TWOMASS J 15 arcsec radius circular aperture magnitude. real 4 mag   phot.flux
j_m_20 twomass_xsc TWOMASS J 20 arcsec radius circular aperture magnitude. real 4 mag   phot.flux
j_m_25 twomass_xsc TWOMASS J 25 arcsec radius circular aperture magnitude. real 4 mag   phot.flux
j_m_2mass allwise_sc2 WISE 2MASS J-band 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 J-band magnitude entry is "null". float 8 mag
j_m_30 twomass_xsc TWOMASS J 30 arcsec radius circular aperture magnitude. real 4 mag   phot.flux
j_m_40 twomass_xsc TWOMASS J 40 arcsec radius circular aperture magnitude. real 4 mag   phot.flux
j_m_5 twomass_xsc TWOMASS J 5 arcsec radius circular aperture magnitude. real 4 mag   phot.flux
j_m_50 twomass_xsc TWOMASS J 50 arcsec radius circular aperture magnitude. real 4 mag   phot.flux
j_m_60 twomass_xsc TWOMASS J 60 arcsec radius circular aperture magnitude. real 4 mag   phot.flux
j_m_7 twomass_sixx2_xsc TWOMASS J 7 arcsec radius circular aperture magnitude real 4 mag
j_m_7 twomass_xsc TWOMASS J 7 arcsec radius circular aperture magnitude. real 4 mag   phot.flux
j_m_70 twomass_xsc TWOMASS J 70 arcsec radius circular aperture magnitude. real 4 mag   phot.flux
j_m_c twomass_xsc TWOMASS J Kron circular aperture magnitude. real 4 mag   phot.flux
j_m_e twomass_xsc TWOMASS J Kron elliptical aperture magnitude. real 4 mag   phot.flux
j_m_ext twomass_sixx2_xsc TWOMASS J mag from fit extrapolation real 4 mag
j_m_ext twomass_xsc TWOMASS J mag from fit extrapolation. real 4 mag   phot.flux
j_m_fc twomass_xsc TWOMASS J fiducial Kron circular magnitude. real 4 mag   phot.flux
j_m_fe twomass_xsc TWOMASS J fiducial Kron ell. mag aperture magnitude. real 4 mag   phot.flux
j_m_i20c twomass_xsc TWOMASS J 20mag/sq." isophotal circular ap. magnitude. real 4 mag   phot.flux
j_m_i20e twomass_xsc TWOMASS J 20mag/sq." isophotal elliptical ap. magnitude. real 4 mag   phot.flux
j_m_i21c twomass_xsc TWOMASS J 21mag/sq." isophotal circular ap. magnitude. real 4 mag   phot.flux
j_m_i21e twomass_xsc TWOMASS J 21mag/sq." isophotal elliptical ap. magnitude. real 4 mag   phot.flux
j_m_j21fc twomass_xsc TWOMASS J 21mag/sq." isophotal fiducial circ. ap. mag. real 4 mag   phot.flux
j_m_j21fe twomass_xsc TWOMASS J 21mag/sq." isophotal fiducial ell. ap. magnitude. real 4 mag   phot.flux
j_m_k20fc twomass_xsc TWOMASS J 20mag/sq." isophotal fiducial circ. ap. mag. real 4 mag   phot.flux
J_M_K20FE twomass SIXDF J 20mag/sq." isophotal fiducial ell. ap. magnitude real 4 mag
j_m_k20fe twomass_sixx2_xsc TWOMASS J 20mag/sq.″ isophotal fiducial ell. ap. magnitude real 4 mag
j_m_k20fe twomass_xsc TWOMASS J 20mag/sq." isophotal fiducial ell. ap. magnitude. real 4 mag   phot.flux
j_m_stdap twomass_psc TWOMASS J-band "standard" aperture magnitude. real 4 mag   phot.flux
j_m_sys twomass_xsc TWOMASS J system photometry magnitude. real 4 mag   phot.flux
j_mnsurfb_eff twomass_xsc TWOMASS J mean surface brightness at the half-light radius. real 4 mag   phot.mag.sb
j_msig twomass_sixx2_psc TWOMASS J "default" mag uncertainty real 4 mag
j_msig_10 twomass_xsc TWOMASS J 1-sigma uncertainty in 10 arcsec circular ap. mag. real 4 mag   stat.error
j_msig_15 twomass_xsc TWOMASS J 1-sigma uncertainty in 15 arcsec circular ap. mag. real 4 mag   stat.error
j_msig_20 twomass_xsc TWOMASS J 1-sigma uncertainty in 20 arcsec circular ap. mag. real 4 mag   stat.error
j_msig_25 twomass_xsc TWOMASS J 1-sigma uncertainty in 25 arcsec circular ap. mag. real 4 mag   stat.error
j_msig_2mass allwise_sc2 WISE 2MASS J-band corrected photometric uncertainty of the associated 2MASS PSC source. This column is "null" if there is no associated 2MASS PSC source or if the 2MASS PSC J-band uncertainty entry is "null". float 8 mag
j_msig_30 twomass_xsc TWOMASS J 1-sigma uncertainty in 30 arcsec circular ap. mag. real 4 mag   stat.error
j_msig_40 twomass_xsc TWOMASS J 1-sigma uncertainty in 40 arcsec circular ap. mag. real 4 mag   stat.error
j_msig_5 twomass_xsc TWOMASS J 1-sigma uncertainty in 5 arcsec circular ap. mag. real 4 mag   stat.error
j_msig_50 twomass_xsc TWOMASS J 1-sigma uncertainty in 50 arcsec circular ap. mag. real 4 mag   stat.error
j_msig_60 twomass_xsc TWOMASS J 1-sigma uncertainty in 60 arcsec circular ap. mag. real 4 mag   stat.error
j_msig_7 twomass_sixx2_xsc TWOMASS J 1-sigma uncertainty in 7 arcsec circular ap. mag real 4 mag
j_msig_7 twomass_xsc TWOMASS J 1-sigma uncertainty in 7 arcsec circular ap. mag. real 4 mag   stat.error
j_msig_70 twomass_xsc TWOMASS J 1-sigma uncertainty in 70 arcsec circular ap. mag. real 4 mag   stat.error
j_msig_c twomass_xsc TWOMASS J 1-sigma uncertainty in Kron circular mag. real 4 mag   stat.error
j_msig_e twomass_xsc TWOMASS J 1-sigma uncertainty in Kron elliptical mag. real 4 mag   stat.error
j_msig_ext twomass_sixx2_xsc TWOMASS J 1-sigma uncertainty in mag from fit extrapolation real 4 mag
j_msig_ext twomass_xsc TWOMASS J 1-sigma uncertainty in mag from fit extrapolation. real 4 mag   stat.error
j_msig_fc twomass_xsc TWOMASS J 1-sigma uncertainty in fiducial Kron circ. mag. real 4 mag   stat.error
j_msig_fe twomass_xsc TWOMASS J 1-sigma uncertainty in fiducial Kron ell. mag. real 4 mag   stat.error
j_msig_i20c twomass_xsc TWOMASS J 1-sigma uncertainty in 20mag/sq." iso. circ. mag. real 4 mag   stat.error
j_msig_i20e twomass_xsc TWOMASS J 1-sigma uncertainty in 20mag/sq." iso. ell. mag. real 4 mag   stat.error
j_msig_i21c twomass_xsc TWOMASS J 1-sigma uncertainty in 21mag/sq." iso. circ. mag. real 4 mag   stat.error
j_msig_i21e twomass_xsc TWOMASS J 1-sigma uncertainty in 21mag/sq." iso. ell. mag. real 4 mag   stat.error
j_msig_j21fc twomass_xsc TWOMASS J 1-sigma uncertainty in 21mag/sq." iso.fid.circ.mag. real 4 mag   stat.error
j_msig_j21fe twomass_xsc TWOMASS J 1-sigma uncertainty in 21mag/sq." iso.fid.ell.mag. real 4 mag   stat.error
j_msig_k20fc twomass_xsc TWOMASS J 1-sigma uncertainty in 20mag/sq." iso.fid.circ. mag. real 4 mag   stat.error
j_msig_k20fe twomass_xsc TWOMASS J 1-sigma uncertainty in 20mag/sq." iso.fid.ell.mag. real 4 mag   stat.error
j_msig_stdap twomass_psc TWOMASS Uncertainty in the J-band standard aperture magnitude. real 4 mag   phot.flux
j_msig_sys twomass_xsc TWOMASS J 1-sigma uncertainty in system photometry mag. real 4 mag   stat.error
j_msigcom twomass_psc TWOMASS Combined, or total photometric uncertainty for the default J-band magnitude. real 4 mag J-band phot.flux
j_msigcom twomass_sixx2_psc TWOMASS combined (total) J band photometric uncertainty real 4 mag
j_msnr10 twomass_scn TWOMASS The estimated J-band magnitude at which SNR=10 is achieved for this scan. real 4 mag   phot.flux
j_msnr10 twomass_sixx2_scn TWOMASS J mag at which SNR=10 is achieved, from j_psp and j_zp_ap real 4 mag
j_n_snr10 twomass_scn TWOMASS Number of point sources at J-band with SNR>10 (instrumental mag <=15.8) int 4     meta.number
j_n_snr10 twomass_sixx2_scn TWOMASS number of J point sources with SNR>10 (instrumental m<=15.8) int 4
j_pchi twomass_xsc TWOMASS J chi^2 of fit to rad. profile (LCSB: alpha scale len). real 4     stat.fit.param
j_peak twomass_xsc TWOMASS J peak pixel brightness. real 4 mag   phot.mag.sb
j_perc_darea twomass_xsc TWOMASS J 5-sigma to 3-sigma percent area change. smallint 2     FIT_PARAM
j_phi twomass_xsc TWOMASS J angle to 3-sigma major axis (E of N). smallint 2 degrees   pos.posAng
j_psfchi twomass_psc TWOMASS Reduced chi-squared goodness-of-fit value for the J-band profile-fit photometry made on the 1.3 s "Read_2" exposures. real 4     stat.fit.param
j_psp twomass_scn TWOMASS J-band photometric sensitivity paramater (PSP). real 4     instr.sensitivity
j_psp twomass_sixx2_scn TWOMASS J photometric sensitivity param: j_shape_avg*(j_fbg_avg^.29) real 4
j_pts_noise twomass_scn TWOMASS Base-10 logarithm of the mode of the noise distribution for all point source detections in the scan, where the noise is estimated from the measured J-band photometric errors and is expressed in units of mJy. real 4     instr.det.noise
j_pts_noise twomass_sixx2_scn TWOMASS log10 of J band modal point src noise estimate real 4 logmJy
j_r_c twomass_xsc TWOMASS J Kron circular aperture radius. real 4 arcsec   phys.angSize;src
j_r_e twomass_xsc TWOMASS J Kron elliptical aperture semi-major axis. real 4 arcsec   phys.angSize;src
j_r_eff twomass_xsc TWOMASS J half-light (integrated half-flux point) radius. real 4 arcsec   phys.angSize;src
j_r_i20c twomass_xsc TWOMASS J 20mag/sq." isophotal circular aperture radius. real 4 arcsec   phys.angSize;src
j_r_i20e twomass_xsc TWOMASS J 20mag/sq." isophotal elliptical ap. semi-major axis. real 4 arcsec   phys.angSize;src
j_r_i21c twomass_xsc TWOMASS J 21mag/sq." isophotal circular aperture radius. real 4 arcsec   phys.angSize;src
j_r_i21e twomass_xsc TWOMASS J 21mag/sq." isophotal elliptical ap. semi-major axis. real 4 arcsec   phys.angSize;src
j_resid_ann twomass_xsc TWOMASS J residual annulus background median. real 4 DN   meta.code
j_sc_1mm twomass_xsc TWOMASS J 1st moment (score) (LCSB: super blk 2,4,8 SNR). real 4     meta.code
j_sc_2mm twomass_xsc TWOMASS J 2nd moment (score) (LCSB: SNRMAX - super SNR max). real 4     meta.code
j_sc_msh twomass_xsc TWOMASS J median shape score. real 4     meta.code
j_sc_mxdn twomass_xsc TWOMASS J mxdn (score) (LCSB: BSNR - block/smoothed SNR). real 4     meta.code
j_sc_r1 twomass_xsc TWOMASS J r1 (score). real 4     meta.code
j_sc_r23 twomass_xsc TWOMASS J r23 (score) (LCSB: TSNR - integrated SNR for r=15). real 4     meta.code
j_sc_sh twomass_xsc TWOMASS J shape (score). real 4     meta.code
j_sc_vint twomass_xsc TWOMASS J vint (score). real 4     meta.code
j_sc_wsh twomass_xsc TWOMASS J wsh (score) (LCSB: PSNR - peak raw SNR). real 4     meta.code
j_seetrack twomass_xsc TWOMASS J band seetracking score. real 4     meta.code
j_sh0 twomass_xsc TWOMASS J ridge shape (LCSB: BSNR limit). real 4     FIT_PARAM
j_shape_avg twomass_scn TWOMASS J-band average seeing shape for scan. real 4     instr.obsty.seeing
j_shape_avg twomass_sixx2_scn TWOMASS J band average seeing shape for scan real 4
j_shape_rms twomass_scn TWOMASS RMS-error of J-band average seeing shape. real 4     instr.obsty.seeing
j_shape_rms twomass_sixx2_scn TWOMASS rms of J band avg seeing shape for scan real 4
j_sig_sh0 twomass_xsc TWOMASS J ridge shape sigma (LCSB: B2SNR limit). real 4     FIT_PARAM
j_snr twomass_psc TWOMASS J-band "scan" signal-to-noise ratio. real 4 mag   instr.det.noise
j_snr twomass_sixx2_psc TWOMASS J band "scan" signal-to-noise ratio real 4
j_subst2 twomass_xsc TWOMASS J residual background #2 (score). real 4     meta.code
j_zp_ap twomass_scn TWOMASS Photometric zero-point for J-band aperture photometry. real 4 mag   phot.mag;arith.zp
j_zp_ap twomass_sixx2_scn TWOMASS J band ap. calibration photometric zero-point for scan real 4 mag
jAmpl vmcCepheidVariables VMCDR4 Peak-to-Peak amplitude in J band {catalogue TType keyword: A(J)} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.J
jAmpl vmcCepheidVariables VMCv20160311 Peak-to-Peak amplitude in J band {catalogue TType keyword: A(J)} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.J
jAmpl vmcCepheidVariables VMCv20160822 Peak-to-Peak amplitude in J band {catalogue TType keyword: A(J)} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.J
jAmpl vmcCepheidVariables VMCv20170109 Peak-to-Peak amplitude in J band {catalogue TType keyword: A(J)} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.J
jAmpl vmcCepheidVariables VMCv20170411 Peak-to-Peak amplitude in J band {catalogue TType keyword: A(J)} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.J
jAmpl vmcCepheidVariables VMCv20171101 Peak-to-Peak amplitude in J band {catalogue TType keyword: A(J)} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.J
jAmpl vmcCepheidVariables VMCv20180702 Peak-to-Peak amplitude in J band {catalogue TType keyword: A(J)} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.J
jAmpl vmcCepheidVariables VMCv20181120 Peak-to-Peak amplitude in J band {catalogue TType keyword: A(J)} real 4 mag -0.9999995e9 src.var.amplitude;em.IR.J
jAmplErr vmcCepheidVariables VMCDR4 Error in Peak-to-Peak amplitude in J band {catalogue TType keyword: e_A(J)} real 4 mag -0.9999995e9 stat.error;src.var.amplitude;em.IR.J
jAmplErr vmcCepheidVariables VMCv20160311 Error in Peak-to-Peak amplitude in J band {catalogue TType keyword: e_A(J)} real 4 mag -0.9999995e9 stat.error;src.var.amplitude;em.IR.J
jAmplErr vmcCepheidVariables VMCv20160822 Error in Peak-to-Peak amplitude in J band {catalogue TType keyword: e_A(J)} real 4 mag -0.9999995e9 stat.error;src.var.amplitude;em.IR.J
jAmplErr vmcCepheidVariables VMCv20170109 Error in Peak-to-Peak amplitude in J band {catalogue TType keyword: e_A(J)} real 4 mag -0.9999995e9 stat.error;src.var.amplitude;em.IR.J
jAmplErr vmcCepheidVariables VMCv20170411 Error in Peak-to-Peak amplitude in J band {catalogue TType keyword: e_A(J)} real 4 mag -0.9999995e9 stat.error;src.var.amplitude;em.IR.J
jAmplErr vmcCepheidVariables VMCv20171101 Error in Peak-to-Peak amplitude in J band {catalogue TType keyword: e_A(J)} real 4 mag -0.9999995e9 stat.error;src.var.amplitude;em.IR.J
jAmplErr vmcCepheidVariables VMCv20180702 Error in Peak-to-Peak amplitude in J band {catalogue TType keyword: e_A(J)} real 4 mag -0.9999995e9 stat.error;src.var.amplitude;em.IR.J
jAmplErr vmcCepheidVariables VMCv20181120 Error in Peak-to-Peak amplitude in J band {catalogue TType keyword: e_A(J)} real 4 mag -0.9999995e9 stat.error;src.var.amplitude;em.IR.J
jAperJky3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Default point source J aperture corrected (2.0 arcsec aperture diameter) calibrated flux
If in doubt use this flux estimator
real 4 jansky -0.9999995e9 phot.flux
jAperJky3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Default point source J aperture corrected (2.0 arcsec aperture diameter) calibrated flux
If in doubt use this flux estimator
real 4 jansky -0.9999995e9 phot.flux
jAperJky3Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in default point/extended source J (2.0 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error
jAperJky3Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in default point/extended source J (2.0 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error
jAperJky4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Point source J aperture corrected (2.8 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 phot.flux
jAperJky4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Point source J aperture corrected (2.8 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 phot.flux
jAperJky4Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in point/extended source J (2.8 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error
jAperJky4Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in point/extended source J (2.8 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error
jAperJky6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Point source J aperture corrected (5.7 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 phot.flux
jAperJky6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Point source J aperture corrected (5.7 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 phot.flux
jAperJky6Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in point/extended source J (5.7 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error
jAperJky6Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in point/extended source J (5.7 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error
jAperJkyNoAperCorr3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Default extended source J (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
jAperJkyNoAperCorr3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Default extended source J (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
jAperJkyNoAperCorr4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Extended source J (2.8 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux real 4 jansky -0.9999995e9 phot.flux
jAperJkyNoAperCorr4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Extended source J (2.8 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux real 4 jansky -0.9999995e9 phot.flux
jAperJkyNoAperCorr6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Extended source J (5.7 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux real 4 jansky -0.9999995e9 phot.flux
jAperJkyNoAperCorr6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Extended source J (5.7 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux real 4 jansky -0.9999995e9 phot.flux
jAperLup3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Default point source J aperture corrected (2.0 arcsec aperture diameter) luptitude
If in doubt use this flux estimator
real 4 lup -0.9999995e9 phot.lup
jAperLup3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Default point source J aperture corrected (2.0 arcsec aperture diameter) luptitude
If in doubt use this flux estimator
real 4 lup -0.9999995e9 phot.lup
jAperLup3Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in default point/extended source J (2.0 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error
jAperLup3Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in default point/extended source J (2.0 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error
jAperLup4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Point source J aperture corrected (2.8 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 phot.lup
jAperLup4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Point source J aperture corrected (2.8 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 phot.lup
jAperLup4Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in point/extended source J (2.8 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error
jAperLup4Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in point/extended source J (2.8 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error
jAperLup6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Point source J aperture corrected (5.7 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 phot.lup
jAperLup6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Point source J aperture corrected (5.7 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 phot.lup
jAperLup6Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in point/extended source J (5.7 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error
jAperLup6Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in point/extended source J (5.7 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error
jAperLupNoAperCorr3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Default extended source J (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
jAperLupNoAperCorr3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Default extended source J (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
jAperLupNoAperCorr4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Extended source J (2.8 arcsec aperture diameter, but no aperture correction applied) aperture luptitude real 4 lup -0.9999995e9 phot.lup
jAperLupNoAperCorr4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Extended source J (2.8 arcsec aperture diameter, but no aperture correction applied) aperture luptitude real 4 lup -0.9999995e9 phot.lup
jAperLupNoAperCorr6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Extended source J (5.7 arcsec aperture diameter, but no aperture correction applied) aperture luptitude real 4 lup -0.9999995e9 phot.lup
jAperLupNoAperCorr6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Extended source J (5.7 arcsec aperture diameter, but no aperture correction applied) aperture luptitude real 4 lup -0.9999995e9 phot.lup
jAperMag1 vmcSynopticSource VMCDR1 Extended source J aperture corrected mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag1 vmcSynopticSource VMCDR2 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag1 vmcSynopticSource VMCDR3 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag1 vmcSynopticSource VMCDR4 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag1 vmcSynopticSource VMCv20110816 Extended source J aperture corrected mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag1 vmcSynopticSource VMCv20110909 Extended source J aperture corrected mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag1 vmcSynopticSource VMCv20120126 Extended source J aperture corrected mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag1 vmcSynopticSource VMCv20121128 Extended source J aperture corrected mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag1 vmcSynopticSource VMCv20130304 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag1 vmcSynopticSource VMCv20130805 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag1 vmcSynopticSource VMCv20140428 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag1 vmcSynopticSource VMCv20140903 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag1 vmcSynopticSource VMCv20150309 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag1 vmcSynopticSource VMCv20151218 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag1 vmcSynopticSource VMCv20160311 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag1 vmcSynopticSource VMCv20160822 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag1 vmcSynopticSource VMCv20170109 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag1 vmcSynopticSource VMCv20170411 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag1 vmcSynopticSource VMCv20171101 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag1 vmcSynopticSource VMCv20180702 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag1 vmcSynopticSource VMCv20181120 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag1 vvvSource VVVDR4 Point source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag1 vvvSynopticSource VVVDR4 Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag1Err vmcSynopticSource VMCDR1 Error in extended source J mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag1Err vmcSynopticSource VMCDR2 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag1Err vmcSynopticSource VMCDR3 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag1Err vmcSynopticSource VMCDR4 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag1Err vmcSynopticSource VMCv20110816 Error in extended source J mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag1Err vmcSynopticSource VMCv20110909 Error in extended source J mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag1Err vmcSynopticSource VMCv20120126 Error in extended source J mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag1Err vmcSynopticSource VMCv20121128 Error in extended source J mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag1Err vmcSynopticSource VMCv20130304 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag1Err vmcSynopticSource VMCv20130805 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag1Err vmcSynopticSource VMCv20140428 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J
jAperMag1Err vmcSynopticSource VMCv20140903 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag1Err vmcSynopticSource VMCv20150309 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag1Err vmcSynopticSource VMCv20151218 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag1Err vmcSynopticSource VMCv20160311 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag1Err vmcSynopticSource VMCv20160822 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag1Err vmcSynopticSource VMCv20170109 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag1Err vmcSynopticSource VMCv20170411 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag1Err vmcSynopticSource VMCv20171101 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag1Err vmcSynopticSource VMCv20180702 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag1Err vmcSynopticSource VMCv20181120 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag1Err vvvSource VVVDR4 Error in point source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag1Err vvvSynopticSource VVVDR4 Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag2 vmcSynopticSource VMCDR1 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag2 vmcSynopticSource VMCDR2 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag2 vmcSynopticSource VMCDR3 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag2 vmcSynopticSource VMCDR4 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag2 vmcSynopticSource VMCv20110816 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag2 vmcSynopticSource VMCv20110909 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag2 vmcSynopticSource VMCv20120126 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag2 vmcSynopticSource VMCv20121128 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag2 vmcSynopticSource VMCv20130304 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag2 vmcSynopticSource VMCv20130805 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag2 vmcSynopticSource VMCv20140428 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag2 vmcSynopticSource VMCv20140903 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag2 vmcSynopticSource VMCv20150309 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag2 vmcSynopticSource VMCv20151218 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag2 vmcSynopticSource VMCv20160311 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag2 vmcSynopticSource VMCv20160822 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag2 vmcSynopticSource VMCv20170109 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag2 vmcSynopticSource VMCv20170411 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag2 vmcSynopticSource VMCv20171101 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag2 vmcSynopticSource VMCv20180702 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag2 vmcSynopticSource VMCv20181120 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag2 vvvSynopticSource VVVDR4 Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag2Err vmcSynopticSource VMCDR1 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag2Err vmcSynopticSource VMCDR2 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag2Err vmcSynopticSource VMCDR3 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag2Err vmcSynopticSource VMCDR4 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag2Err vmcSynopticSource VMCv20110816 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag2Err vmcSynopticSource VMCv20110909 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag2Err vmcSynopticSource VMCv20120126 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag2Err vmcSynopticSource VMCv20121128 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag2Err vmcSynopticSource VMCv20130304 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag2Err vmcSynopticSource VMCv20130805 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag2Err vmcSynopticSource VMCv20140428 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J
jAperMag2Err vmcSynopticSource VMCv20140903 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag2Err vmcSynopticSource VMCv20150309 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag2Err vmcSynopticSource VMCv20151218 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag2Err vmcSynopticSource VMCv20160311 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag2Err vmcSynopticSource VMCv20160822 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag2Err vmcSynopticSource VMCv20170109 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag2Err vmcSynopticSource VMCv20170411 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag2Err vmcSynopticSource VMCv20171101 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag2Err vmcSynopticSource VMCv20180702 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag2Err vmcSynopticSource VMCv20181120 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag2Err vvvSynopticSource VVVDR4 Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag3 vhsSource VHSDR1 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMag3 vhsSource VHSDR2 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMag3 vhsSource VHSDR3 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vhsSource VHSDR4 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vhsSource VHSDR6 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vhsSource VHSv20120926 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMag3 vhsSource VHSv20130417 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMag3 vhsSource VHSv20140409 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vhsSource VHSv20150108 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vhsSource VHSv20160114 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vhsSource VHSv20160507 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vhsSource VHSv20170630 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vhsSource VHSv20180419 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 videoSource VIDEODR2 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMag3 videoSource VIDEODR3 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMag3 videoSource VIDEODR4 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 videoSource VIDEODR5 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 videoSource VIDEOv20100513 Default point/extended source J mag, no aperture correction applied
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMag3 videoSource VIDEOv20111208 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMag3 vikingSource VIKINGDR2 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMag3 vikingSource VIKINGDR3 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMag3 vikingSource VIKINGDR4 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vikingSource VIKINGv20110714 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMag3 vikingSource VIKINGv20111019 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMag3 vikingSource VIKINGv20130417 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMag3 vikingSource VIKINGv20140402 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vikingSource VIKINGv20150421 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vikingSource VIKINGv20151230 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vikingSource VIKINGv20160406 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vikingSource VIKINGv20161202 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vikingSource VIKINGv20170715 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vikingSource VIKINGv20181012 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Default point source J aperture corrected (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMag3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Default point source J aperture corrected (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMag3 vmcSource VMCDR1 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMag3 vmcSource VMCDR2 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vmcSource VMCDR3 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vmcSource VMCDR4 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vmcSource VMCv20110816 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMag3 vmcSource VMCv20110909 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMag3 vmcSource VMCv20120126 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMag3 vmcSource VMCv20121128 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMag3 vmcSource VMCv20130304 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMag3 vmcSource VMCv20130805 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vmcSource VMCv20140428 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vmcSource VMCv20140903 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vmcSource VMCv20150309 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vmcSource VMCv20151218 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vmcSource VMCv20160311 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vmcSource VMCv20160822 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vmcSource VMCv20170109 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vmcSource VMCv20170411 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vmcSource VMCv20171101 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vmcSource VMCv20180702 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vmcSource VMCv20181120 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vmcSynopticSource VMCDR1 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag3 vmcSynopticSource VMCDR2 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vmcSynopticSource VMCDR3 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vmcSynopticSource VMCDR4 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vmcSynopticSource VMCv20110816 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag3 vmcSynopticSource VMCv20110909 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag3 vmcSynopticSource VMCv20120126 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag3 vmcSynopticSource VMCv20121128 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag3 vmcSynopticSource VMCv20130304 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag3 vmcSynopticSource VMCv20130805 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vmcSynopticSource VMCv20140428 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vmcSynopticSource VMCv20140903 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vmcSynopticSource VMCv20150309 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vmcSynopticSource VMCv20151218 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vmcSynopticSource VMCv20160311 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vmcSynopticSource VMCv20160822 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vmcSynopticSource VMCv20170109 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vmcSynopticSource VMCv20170411 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vmcSynopticSource VMCv20171101 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vmcSynopticSource VMCv20180702 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vmcSynopticSource VMCv20181120 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vvvSource VVVDR4 Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3 vvvSynopticSource VVVDR4 Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag3Err vhsSource VHSDR1 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag3Err vhsSource VHSDR2 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag3Err vhsSource VHSDR3 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J
jAperMag3Err vhsSource VHSDR4 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag3Err vhsSource VHSDR6 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag3Err vhsSource VHSv20120926 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag3Err vhsSource VHSv20130417 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag3Err vhsSource VHSv20140409 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J
jAperMag3Err vhsSource VHSv20150108 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag3Err vhsSource VHSv20160114 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag3Err vhsSource VHSv20160507 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag3Err vhsSource VHSv20170630 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag3Err vhsSource VHSv20180419 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag3Err videoSource VIDEODR2 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag3Err videoSource VIDEODR3 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag3Err videoSource VIDEODR4 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag3Err videoSource VIDEODR5 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag3Err videoSource VIDEOv20100513 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag3Err videoSource VIDEOv20111208 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag3Err vikingSource VIKINGDR2 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag3Err vikingSource VIKINGDR3 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag3Err vikingSource VIKINGDR4 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J
jAperMag3Err vikingSource VIKINGv20110714 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag3Err vikingSource VIKINGv20111019 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag3Err vikingSource VIKINGv20130417 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag3Err vikingSource VIKINGv20140402 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag3Err vikingSource VIKINGv20150421 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag3Err vikingSource VIKINGv20151230 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag3Err vikingSource VIKINGv20160406 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag3Err vikingSource VIKINGv20161202 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag3Err vikingSource VIKINGv20170715 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag3Err vikingSource VIKINGv20181012 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag3Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in default point/extended source J (2.0 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error
jAperMag3Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in default point/extended source J (2.0 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error
jAperMag3Err vmcSource VMCDR2 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag3Err vmcSource VMCDR3 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag3Err vmcSource VMCDR4 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag3Err vmcSource VMCv20110816 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag3Err vmcSource VMCv20110909 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag3Err vmcSource VMCv20120126 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag3Err vmcSource VMCv20121128 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag3Err vmcSource VMCv20130304 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag3Err vmcSource VMCv20130805 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag3Err vmcSource VMCv20140428 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J
jAperMag3Err vmcSource VMCv20140903 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag3Err vmcSource VMCv20150309 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag3Err vmcSource VMCv20151218 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag3Err vmcSource VMCv20160311 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag3Err vmcSource VMCv20160822 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag3Err vmcSource VMCv20170109 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag3Err vmcSource VMCv20170411 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag3Err vmcSource VMCv20171101 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag3Err vmcSource VMCv20180702 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag3Err vmcSource VMCv20181120 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag3Err vmcSource, vmcSynopticSource VMCDR1 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag3Err vvvSource VVVDR4 Error in default point source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag3Err vvvSynopticSource VVVDR4 Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag4 vhsSource VHSDR1 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag4 vhsSource VHSDR2 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag4 vhsSource VHSDR3 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vhsSource VHSDR4 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vhsSource VHSDR6 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vhsSource VHSv20120926 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag4 vhsSource VHSv20130417 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag4 vhsSource VHSv20140409 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vhsSource VHSv20150108 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vhsSource VHSv20160114 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vhsSource VHSv20160507 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vhsSource VHSv20170630 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vhsSource VHSv20180419 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 videoSource VIDEODR2 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag4 videoSource VIDEODR3 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag4 videoSource VIDEODR4 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 videoSource VIDEODR5 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 videoSource VIDEOv20100513 Extended source J mag, no aperture correction applied real 4 mag -0.9999995e9 phot.mag
jAperMag4 videoSource VIDEOv20111208 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag4 vikingSource VIKINGDR2 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag4 vikingSource VIKINGDR3 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag4 vikingSource VIKINGDR4 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vikingSource VIKINGv20110714 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag4 vikingSource VIKINGv20111019 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag4 vikingSource VIKINGv20130417 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag4 vikingSource VIKINGv20140402 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vikingSource VIKINGv20150421 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vikingSource VIKINGv20151230 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vikingSource VIKINGv20160406 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vikingSource VIKINGv20161202 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vikingSource VIKINGv20170715 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vikingSource VIKINGv20181012 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Point source J aperture corrected (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Point source J aperture corrected (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag4 vmcSource VMCDR1 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag4 vmcSource VMCDR2 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vmcSource VMCDR3 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vmcSource VMCDR4 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vmcSource VMCv20110816 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag4 vmcSource VMCv20110909 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag4 vmcSource VMCv20120126 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag4 vmcSource VMCv20121128 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag4 vmcSource VMCv20130304 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag4 vmcSource VMCv20130805 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vmcSource VMCv20140428 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vmcSource VMCv20140903 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vmcSource VMCv20150309 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vmcSource VMCv20151218 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vmcSource VMCv20160311 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vmcSource VMCv20160822 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vmcSource VMCv20170109 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vmcSource VMCv20170411 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vmcSource VMCv20171101 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vmcSource VMCv20180702 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vmcSource VMCv20181120 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vmcSynopticSource VMCDR1 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag4 vmcSynopticSource VMCDR2 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vmcSynopticSource VMCDR3 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vmcSynopticSource VMCDR4 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vmcSynopticSource VMCv20110816 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag4 vmcSynopticSource VMCv20110909 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag4 vmcSynopticSource VMCv20120126 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag4 vmcSynopticSource VMCv20121128 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag4 vmcSynopticSource VMCv20130304 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag4 vmcSynopticSource VMCv20130805 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vmcSynopticSource VMCv20140428 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vmcSynopticSource VMCv20140903 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vmcSynopticSource VMCv20150309 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vmcSynopticSource VMCv20151218 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vmcSynopticSource VMCv20160311 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vmcSynopticSource VMCv20160822 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vmcSynopticSource VMCv20170109 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vmcSynopticSource VMCv20170411 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vmcSynopticSource VMCv20171101 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vmcSynopticSource VMCv20180702 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vmcSynopticSource VMCv20181120 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vvvSource VVVDR4 Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4 vvvSynopticSource VVVDR4 Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag4Err vhsSource VHSDR1 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag4Err vhsSource VHSDR2 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag4Err vhsSource VHSDR3 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J
jAperMag4Err vhsSource VHSDR4 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag4Err vhsSource VHSDR6 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag4Err vhsSource VHSv20120926 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag4Err vhsSource VHSv20130417 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag4Err vhsSource VHSv20140409 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J
jAperMag4Err vhsSource VHSv20150108 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag4Err vhsSource VHSv20160114 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag4Err vhsSource VHSv20160507 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag4Err vhsSource VHSv20170630 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag4Err vhsSource VHSv20180419 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag4Err videoSource VIDEODR2 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag4Err videoSource VIDEODR3 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag4Err videoSource VIDEODR4 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag4Err videoSource VIDEODR5 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag4Err videoSource VIDEOv20100513 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag4Err videoSource VIDEOv20111208 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag4Err vikingSource VIKINGDR2 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag4Err vikingSource VIKINGDR3 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag4Err vikingSource VIKINGDR4 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J
jAperMag4Err vikingSource VIKINGv20110714 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag4Err vikingSource VIKINGv20111019 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag4Err vikingSource VIKINGv20130417 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag4Err vikingSource VIKINGv20140402 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag4Err vikingSource VIKINGv20150421 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag4Err vikingSource VIKINGv20151230 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag4Err vikingSource VIKINGv20160406 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag4Err vikingSource VIKINGv20161202 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag4Err vikingSource VIKINGv20170715 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag4Err vikingSource VIKINGv20181012 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag4Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in point/extended source J (2.8 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error
jAperMag4Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in point/extended source J (2.8 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error
jAperMag4Err vmcSource VMCDR1 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag4Err vmcSource VMCDR2 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag4Err vmcSource VMCDR3 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag4Err vmcSource VMCDR4 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag4Err vmcSource VMCv20110816 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag4Err vmcSource VMCv20110909 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag4Err vmcSource VMCv20120126 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag4Err vmcSource VMCv20121128 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag4Err vmcSource VMCv20130304 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag4Err vmcSource VMCv20130805 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag4Err vmcSource VMCv20140428 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J
jAperMag4Err vmcSource VMCv20140903 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag4Err vmcSource VMCv20150309 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag4Err vmcSource VMCv20151218 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag4Err vmcSource VMCv20160311 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag4Err vmcSource VMCv20160822 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag4Err vmcSource VMCv20170109 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag4Err vmcSource VMCv20170411 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag4Err vmcSource VMCv20171101 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag4Err vmcSource VMCv20180702 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag4Err vmcSource VMCv20181120 Error in point/extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag4Err vmcSynopticSource VMCDR1 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag4Err vmcSynopticSource VMCDR2 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag4Err vmcSynopticSource VMCDR3 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag4Err vmcSynopticSource VMCDR4 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag4Err vmcSynopticSource VMCv20110816 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag4Err vmcSynopticSource VMCv20110909 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag4Err vmcSynopticSource VMCv20120126 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag4Err vmcSynopticSource VMCv20121128 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag4Err vmcSynopticSource VMCv20130304 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag4Err vmcSynopticSource VMCv20130805 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag4Err vmcSynopticSource VMCv20140428 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J
jAperMag4Err vmcSynopticSource VMCv20140903 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag4Err vmcSynopticSource VMCv20150309 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag4Err vmcSynopticSource VMCv20151218 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag4Err vmcSynopticSource VMCv20160311 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag4Err vmcSynopticSource VMCv20160822 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag4Err vmcSynopticSource VMCv20170109 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag4Err vmcSynopticSource VMCv20170411 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag4Err vmcSynopticSource VMCv20171101 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag4Err vmcSynopticSource VMCv20180702 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag4Err vmcSynopticSource VMCv20181120 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag4Err vvvSource VVVDR4 Error in point source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag4Err vvvSynopticSource VVVDR4 Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag5 vmcSynopticSource VMCDR1 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag5 vmcSynopticSource VMCDR2 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag5 vmcSynopticSource VMCDR3 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag5 vmcSynopticSource VMCDR4 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag5 vmcSynopticSource VMCv20110816 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag5 vmcSynopticSource VMCv20110909 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag5 vmcSynopticSource VMCv20120126 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag5 vmcSynopticSource VMCv20121128 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag5 vmcSynopticSource VMCv20130304 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag5 vmcSynopticSource VMCv20130805 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag5 vmcSynopticSource VMCv20140428 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag5 vmcSynopticSource VMCv20140903 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag5 vmcSynopticSource VMCv20150309 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag5 vmcSynopticSource VMCv20151218 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag5 vmcSynopticSource VMCv20160311 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag5 vmcSynopticSource VMCv20160822 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag5 vmcSynopticSource VMCv20170109 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag5 vmcSynopticSource VMCv20170411 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag5 vmcSynopticSource VMCv20171101 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag5 vmcSynopticSource VMCv20180702 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag5 vmcSynopticSource VMCv20181120 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag5 vvvSynopticSource VVVDR4 Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag5Err vmcSynopticSource VMCDR1 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag5Err vmcSynopticSource VMCDR2 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag5Err vmcSynopticSource VMCDR3 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag5Err vmcSynopticSource VMCDR4 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag5Err vmcSynopticSource VMCv20110816 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag5Err vmcSynopticSource VMCv20110909 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag5Err vmcSynopticSource VMCv20120126 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag5Err vmcSynopticSource VMCv20121128 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag5Err vmcSynopticSource VMCv20130304 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag5Err vmcSynopticSource VMCv20130805 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag5Err vmcSynopticSource VMCv20140428 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J
jAperMag5Err vmcSynopticSource VMCv20140903 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag5Err vmcSynopticSource VMCv20150309 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag5Err vmcSynopticSource VMCv20151218 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag5Err vmcSynopticSource VMCv20160311 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag5Err vmcSynopticSource VMCv20160822 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag5Err vmcSynopticSource VMCv20170109 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag5Err vmcSynopticSource VMCv20170411 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag5Err vmcSynopticSource VMCv20171101 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag5Err vmcSynopticSource VMCv20180702 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag5Err vmcSynopticSource VMCv20181120 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag5Err vvvSynopticSource VVVDR4 Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag6 vhsSource VHSDR1 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag6 vhsSource VHSDR2 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag6 vhsSource VHSDR3 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag6 vhsSource VHSDR4 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag6 vhsSource VHSDR6 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag6 vhsSource VHSv20120926 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag6 vhsSource VHSv20130417 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag6 vhsSource VHSv20140409 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag6 vhsSource VHSv20150108 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag6 vhsSource VHSv20160114 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag6 vhsSource VHSv20160507 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag6 vhsSource VHSv20170630 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag6 vhsSource VHSv20180419 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag6 videoSource VIDEODR2 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag6 videoSource VIDEODR3 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag6 videoSource VIDEODR4 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag6 videoSource VIDEODR5 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag6 videoSource VIDEOv20100513 Extended source J mag, no aperture correction applied real 4 mag -0.9999995e9 phot.mag
jAperMag6 videoSource VIDEOv20111208 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag6 vikingSource VIKINGDR2 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag6 vikingSource VIKINGDR3 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag6 vikingSource VIKINGDR4 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag6 vikingSource VIKINGv20110714 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag6 vikingSource VIKINGv20111019 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag6 vikingSource VIKINGv20130417 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag6 vikingSource VIKINGv20140402 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag6 vikingSource VIKINGv20150421 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag6 vikingSource VIKINGv20151230 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag6 vikingSource VIKINGv20160406 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag6 vikingSource VIKINGv20161202 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag6 vikingSource VIKINGv20170715 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag6 vikingSource VIKINGv20181012 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Point source J aperture corrected (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Point source J aperture corrected (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag6 vmcSource VMCDR1 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag6 vmcSource VMCDR2 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag6 vmcSource VMCDR3 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag6 vmcSource VMCDR4 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag6 vmcSource VMCv20110816 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag6 vmcSource VMCv20110909 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag6 vmcSource VMCv20120126 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag6 vmcSource VMCv20121128 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag6 vmcSource VMCv20130304 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMag6 vmcSource VMCv20130805 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag6 vmcSource VMCv20140428 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag6 vmcSource VMCv20140903 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag6 vmcSource VMCv20150309 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag6 vmcSource VMCv20151218 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag6 vmcSource VMCv20160311 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag6 vmcSource VMCv20160822 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag6 vmcSource VMCv20170109 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag6 vmcSource VMCv20170411 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag6 vmcSource VMCv20171101 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag6 vmcSource VMCv20180702 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag6 vmcSource VMCv20181120 Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMag6Err vhsSource VHSDR1 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag6Err vhsSource VHSDR2 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag6Err vhsSource VHSDR3 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J
jAperMag6Err vhsSource VHSDR4 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag6Err vhsSource VHSDR6 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag6Err vhsSource VHSv20120926 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag6Err vhsSource VHSv20130417 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag6Err vhsSource VHSv20140409 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J
jAperMag6Err vhsSource VHSv20150108 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag6Err vhsSource VHSv20160114 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag6Err vhsSource VHSv20160507 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag6Err vhsSource VHSv20170630 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag6Err vhsSource VHSv20180419 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag6Err videoSource VIDEODR2 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag6Err videoSource VIDEODR3 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag6Err videoSource VIDEODR4 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag6Err videoSource VIDEODR5 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag6Err videoSource VIDEOv20100513 Error in extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag6Err videoSource VIDEOv20111208 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag6Err vikingSource VIKINGDR2 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag6Err vikingSource VIKINGDR3 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag6Err vikingSource VIKINGDR4 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J
jAperMag6Err vikingSource VIKINGv20110714 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag6Err vikingSource VIKINGv20111019 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag6Err vikingSource VIKINGv20130417 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag6Err vikingSource VIKINGv20140402 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag6Err vikingSource VIKINGv20150421 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag6Err vikingSource VIKINGv20151230 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag6Err vikingSource VIKINGv20160406 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag6Err vikingSource VIKINGv20161202 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag6Err vikingSource VIKINGv20170715 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag6Err vikingSource VIKINGv20181012 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag6Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Error in point/extended source J (5.7 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error
jAperMag6Err vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Error in point/extended source J (5.7 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error
jAperMag6Err vmcSource VMCDR1 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag6Err vmcSource VMCDR2 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag6Err vmcSource VMCDR3 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag6Err vmcSource VMCDR4 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag6Err vmcSource VMCv20110816 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag6Err vmcSource VMCv20110909 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag6Err vmcSource VMCv20120126 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag6Err vmcSource VMCv20121128 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag6Err vmcSource VMCv20130304 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag6Err vmcSource VMCv20130805 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error
jAperMag6Err vmcSource VMCv20140428 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J
jAperMag6Err vmcSource VMCv20140903 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag6Err vmcSource VMCv20150309 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;em.IR.J;phot.mag
jAperMag6Err vmcSource VMCv20151218 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag6Err vmcSource VMCv20160311 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag6Err vmcSource VMCv20160822 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag6Err vmcSource VMCv20170109 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag6Err vmcSource VMCv20170411 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag6Err vmcSource VMCv20171101 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag6Err vmcSource VMCv20180702 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMag6Err vmcSource VMCv20181120 Error in point/extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 stat.error;phot.mag;em.IR.J
jAperMagNoAperCorr3 vhsSource VHSDR1 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr3 vhsSource VHSDR2 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr3 vhsSource VHSDR3 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr3 vhsSource VHSDR4 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr3 vhsSource VHSDR6 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr3 vhsSource VHSv20120926 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr3 vhsSource VHSv20130417 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr3 vhsSource VHSv20140409 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr3 vhsSource VHSv20150108 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr3 vhsSource VHSv20160114 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr3 vhsSource VHSv20160507 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr3 vhsSource VHSv20170630 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr3 vhsSource VHSv20180419 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr3 videoSource VIDEODR2 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr3 videoSource VIDEODR3 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr3 videoSource VIDEODR4 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr3 videoSource VIDEODR5 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr3 videoSource VIDEOv20111208 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr3 vikingSource VIKINGDR2 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr3 vikingSource VIKINGDR3 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr3 vikingSource VIKINGDR4 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr3 vikingSource VIKINGv20110714 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr3 vikingSource VIKINGv20111019 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr3 vikingSource VIKINGv20130417 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr3 vikingSource VIKINGv20140402 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr3 vikingSource VIKINGv20150421 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr3 vikingSource VIKINGv20151230 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr3 vikingSource VIKINGv20160406 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr3 vikingSource VIKINGv20161202 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr3 vikingSource VIKINGv20170715 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr3 vikingSource VIKINGv20181012 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Default extended source J (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
jAperMagNoAperCorr3 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Default extended source J (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
jAperMagNoAperCorr3 vmcSource VMCDR1 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr3 vmcSource VMCDR2 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr3 vmcSource VMCDR3 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr3 vmcSource VMCDR4 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr3 vmcSource VMCv20110816 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr3 vmcSource VMCv20110909 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr3 vmcSource VMCv20120126 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr3 vmcSource VMCv20121128 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr3 vmcSource VMCv20130304 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr3 vmcSource VMCv20130805 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr3 vmcSource VMCv20140428 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr3 vmcSource VMCv20140903 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr3 vmcSource VMCv20150309 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr3 vmcSource VMCv20151218 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr3 vmcSource VMCv20160311 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr3 vmcSource VMCv20160822 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr3 vmcSource VMCv20170109 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr3 vmcSource VMCv20170411 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr3 vmcSource VMCv20171101 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr3 vmcSource VMCv20180702 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr3 vmcSource VMCv20181120 Default extended source J aperture mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator
real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr4 vhsSource VHSDR1 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr4 vhsSource VHSDR2 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr4 vhsSource VHSDR3 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr4 vhsSource VHSDR4 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr4 vhsSource VHSDR6 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr4 vhsSource VHSv20120926 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr4 vhsSource VHSv20130417 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr4 vhsSource VHSv20140409 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr4 vhsSource VHSv20150108 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr4 vhsSource VHSv20160114 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr4 vhsSource VHSv20160507 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr4 vhsSource VHSv20170630 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr4 vhsSource VHSv20180419 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr4 videoSource VIDEODR2 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr4 videoSource VIDEODR3 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr4 videoSource VIDEODR4 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr4 videoSource VIDEODR5 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr4 videoSource VIDEOv20111208 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr4 vikingSource VIKINGDR2 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr4 vikingSource VIKINGDR3 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr4 vikingSource VIKINGDR4 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr4 vikingSource VIKINGv20110714 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr4 vikingSource VIKINGv20111019 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr4 vikingSource VIKINGv20130417 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr4 vikingSource VIKINGv20140402 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr4 vikingSource VIKINGv20150421 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr4 vikingSource VIKINGv20151230 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr4 vikingSource VIKINGv20160406 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr4 vikingSource VIKINGv20161202 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr4 vikingSource VIKINGv20170715 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr4 vikingSource VIKINGv20181012 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Extended source J (2.8 arcsec aperture diameter, but no aperture correction applied) aperture magnitude real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr4 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Extended source J (2.8 arcsec aperture diameter, but no aperture correction applied) aperture magnitude real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr4 vmcSource VMCDR1 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr4 vmcSource VMCDR2 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr4 vmcSource VMCDR3 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr4 vmcSource VMCDR4 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr4 vmcSource VMCv20110816 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr4 vmcSource VMCv20110909 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr4 vmcSource VMCv20120126 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr4 vmcSource VMCv20121128 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr4 vmcSource VMCv20130304 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr4 vmcSource VMCv20130805 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr4 vmcSource VMCv20140428 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr4 vmcSource VMCv20140903 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr4 vmcSource VMCv20150309 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr4 vmcSource VMCv20151218 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr4 vmcSource VMCv20160311 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr4 vmcSource VMCv20160822 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr4 vmcSource VMCv20170109 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr4 vmcSource VMCv20170411 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr4 vmcSource VMCv20171101 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr4 vmcSource VMCv20180702 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr4 vmcSource VMCv20181120 Extended source J aperture mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr6 vhsSource VHSDR1 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr6 vhsSource VHSDR2 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr6 vhsSource VHSDR3 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr6 vhsSource VHSDR4 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr6 vhsSource VHSDR6 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr6 vhsSource VHSv20120926 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr6 vhsSource VHSv20130417 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr6 vhsSource VHSv20140409 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr6 vhsSource VHSv20150108 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr6 vhsSource VHSv20160114 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr6 vhsSource VHSv20160507 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr6 vhsSource VHSv20170630 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr6 vhsSource VHSv20180419 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr6 videoSource VIDEODR2 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr6 videoSource VIDEODR3 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr6 videoSource VIDEODR4 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr6 videoSource VIDEODR5 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr6 videoSource VIDEOv20111208 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr6 vikingSource VIKINGDR2 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr6 vikingSource VIKINGDR3 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr6 vikingSource VIKINGDR4 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr6 vikingSource VIKINGv20110714 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr6 vikingSource VIKINGv20111019 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr6 vikingSource VIKINGv20130417 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr6 vikingSource VIKINGv20140402 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr6 vikingSource VIKINGv20150421 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr6 vikingSource VIKINGv20151230 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr6 vikingSource VIKINGv20160406 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr6 vikingSource VIKINGv20161202 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr6 vikingSource VIKINGv20170715 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr6 vikingSource VIKINGv20181012 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 Extended source J (5.7 arcsec aperture diameter, but no aperture correction applied) aperture magnitude real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr6 vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 Extended source J (5.7 arcsec aperture diameter, but no aperture correction applied) aperture magnitude real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr6 vmcSource VMCDR1 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr6 vmcSource VMCDR2 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr6 vmcSource VMCDR3 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr6 vmcSource VMCDR4 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr6 vmcSource VMCv20110816 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr6 vmcSource VMCv20110909 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr6 vmcSource VMCv20120126 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr6 vmcSource VMCv20121128 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr6 vmcSource VMCv20130304 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag
jAperMagNoAperCorr6 vmcSource VMCv20130805 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr6 vmcSource VMCv20140428 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr6 vmcSource VMCv20140903 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr6 vmcSource VMCv20150309 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr6 vmcSource VMCv20151218 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr6 vmcSource VMCv20160311 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr6 vmcSource VMCv20160822 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr6 vmcSource VMCv20170109 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr6 vmcSource VMCv20170411 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr6 vmcSource VMCv20171101 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr6 vmcSource VMCv20180702 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jAperMagNoAperCorr6 vmcSource VMCv20181120 Extended source J aperture mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag;em.IR.J
jaStratAst videoVarFrameSetInfo VIDEODR2 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst videoVarFrameSetInfo VIDEODR3 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst videoVarFrameSetInfo VIDEODR4 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst videoVarFrameSetInfo VIDEODR5 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst videoVarFrameSetInfo VIDEOv20100513 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst videoVarFrameSetInfo VIDEOv20111208 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst vikingVarFrameSetInfo VIKINGDR2 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst vikingVarFrameSetInfo VIKINGDR3 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst vikingVarFrameSetInfo VIKINGDR4 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst vikingVarFrameSetInfo VIKINGv20110714 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst vikingVarFrameSetInfo VIKINGv20111019 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst vikingVarFrameSetInfo VIKINGv20130417 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst vikingVarFrameSetInfo VIKINGv20140402 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst vikingVarFrameSetInfo VIKINGv20150421 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst vikingVarFrameSetInfo VIKINGv20151230 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst vikingVarFrameSetInfo VIKINGv20160406 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst vikingVarFrameSetInfo VIKINGv20161202 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst vikingVarFrameSetInfo VIKINGv20170715 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst vikingVarFrameSetInfo VIKINGv20181012 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst vmcVarFrameSetInfo VMCDR1 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst vmcVarFrameSetInfo VMCDR2 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst vmcVarFrameSetInfo VMCDR3 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst vmcVarFrameSetInfo VMCDR4 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst vmcVarFrameSetInfo VMCv20110816 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst vmcVarFrameSetInfo VMCv20110909 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst vmcVarFrameSetInfo VMCv20120126 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst vmcVarFrameSetInfo VMCv20121128 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst vmcVarFrameSetInfo VMCv20130304 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst vmcVarFrameSetInfo VMCv20130805 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst vmcVarFrameSetInfo VMCv20140428 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst vmcVarFrameSetInfo VMCv20140903 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst vmcVarFrameSetInfo VMCv20150309 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst vmcVarFrameSetInfo VMCv20151218 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst vmcVarFrameSetInfo VMCv20160311 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst vmcVarFrameSetInfo VMCv20160822 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst vmcVarFrameSetInfo VMCv20170109 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst vmcVarFrameSetInfo VMCv20170411 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst vmcVarFrameSetInfo VMCv20171101 Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst vmcVarFrameSetInfo VMCv20180702 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratAst vmcVarFrameSetInfo VMCv20181120 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jaStratPht videoVarFrameSetInfo VIDEODR2 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht videoVarFrameSetInfo VIDEODR3 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht videoVarFrameSetInfo VIDEODR4 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht videoVarFrameSetInfo VIDEODR5 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht videoVarFrameSetInfo VIDEOv20100513 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht videoVarFrameSetInfo VIDEOv20111208 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht vikingVarFrameSetInfo VIKINGDR2 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht vikingVarFrameSetInfo VIKINGDR3 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht vikingVarFrameSetInfo VIKINGDR4 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht vikingVarFrameSetInfo VIKINGv20110714 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht vikingVarFrameSetInfo VIKINGv20111019 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht vikingVarFrameSetInfo VIKINGv20130417 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht vikingVarFrameSetInfo VIKINGv20140402 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht vikingVarFrameSetInfo VIKINGv20150421 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht vikingVarFrameSetInfo VIKINGv20151230 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht vikingVarFrameSetInfo VIKINGv20160406 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht vikingVarFrameSetInfo VIKINGv20161202 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht vikingVarFrameSetInfo VIKINGv20170715 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht vikingVarFrameSetInfo VIKINGv20181012 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht vmcVarFrameSetInfo VMCDR1 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht vmcVarFrameSetInfo VMCDR2 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht vmcVarFrameSetInfo VMCDR3 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht vmcVarFrameSetInfo VMCDR4 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht vmcVarFrameSetInfo VMCv20110816 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht vmcVarFrameSetInfo VMCv20110909 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht vmcVarFrameSetInfo VMCv20120126 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht vmcVarFrameSetInfo VMCv20121128 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht vmcVarFrameSetInfo VMCv20130304 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht vmcVarFrameSetInfo VMCv20130805 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht vmcVarFrameSetInfo VMCv20140428 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht vmcVarFrameSetInfo VMCv20140903 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht vmcVarFrameSetInfo VMCv20150309 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht vmcVarFrameSetInfo VMCv20151218 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht vmcVarFrameSetInfo VMCv20160311 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht vmcVarFrameSetInfo VMCv20160822 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht vmcVarFrameSetInfo VMCv20170109 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht vmcVarFrameSetInfo VMCv20170411 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht vmcVarFrameSetInfo VMCv20171101 Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht vmcVarFrameSetInfo VMCv20180702 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jaStratPht vmcVarFrameSetInfo VMCv20181120 Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jAverageConf vhsSource VHSDR1 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -99999999 meta.code
jAverageConf vhsSource VHSDR2 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -99999999 meta.code
jAverageConf vhsSource VHSDR3 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.J
jAverageConf vhsSource VHSDR4 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.J
jAverageConf vhsSource VHSDR6 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.J
jAverageConf vhsSource VHSv20120926 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -99999999 stat.likelihood;em.IR.NIR
jAverageConf vhsSource VHSv20130417 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.NIR
jAverageConf vhsSource VHSv20140409 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.J
jAverageConf vhsSource VHSv20150108 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.J
jAverageConf vhsSource VHSv20160114 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.J
jAverageConf vhsSource VHSv20160507 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.J
jAverageConf vhsSource VHSv20170630 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.J
jAverageConf vhsSource VHSv20180419 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.J
jAverageConf vikingSource VIKINGDR2 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -99999999 meta.code
jAverageConf vikingSource VIKINGDR3 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -99999999 stat.likelihood;em.IR.NIR
jAverageConf vikingSource VIKINGDR4 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.J
jAverageConf vikingSource VIKINGv20110714 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -99999999 meta.code
jAverageConf vikingSource VIKINGv20111019 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -99999999 meta.code
jAverageConf vikingSource VIKINGv20130417 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.NIR
jAverageConf vikingSource VIKINGv20140402 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.NIR
jAverageConf vikingSource VIKINGv20150421 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.J
jAverageConf vikingSource VIKINGv20151230 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.J
jAverageConf vikingSource VIKINGv20160406 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.J
jAverageConf vikingSource VIKINGv20161202 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.J
jAverageConf vikingSource VIKINGv20170715 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.J
jAverageConf vikingSource VIKINGv20181012 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.J
jAverageConf vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.NIR
jAverageConf vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.NIR
jAverageConf vmcSource VMCDR2 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.NIR
jAverageConf vmcSource VMCDR3 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.J
jAverageConf vmcSource VMCDR4 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.J
jAverageConf vmcSource VMCv20110816 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -99999999 meta.code
jAverageConf vmcSource VMCv20110909 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -99999999 meta.code
jAverageConf vmcSource VMCv20120126 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -99999999 meta.code
jAverageConf vmcSource VMCv20121128 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -99999999 stat.likelihood;em.IR.NIR
jAverageConf vmcSource VMCv20130304 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.NIR
jAverageConf vmcSource VMCv20130805 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.NIR
jAverageConf vmcSource VMCv20140428 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.J
jAverageConf vmcSource VMCv20140903 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.J
jAverageConf vmcSource VMCv20150309 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.J
jAverageConf vmcSource VMCv20151218 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.J
jAverageConf vmcSource VMCv20160311 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.J
jAverageConf vmcSource VMCv20160822 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.J
jAverageConf vmcSource VMCv20170109 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.J
jAverageConf vmcSource VMCv20170411 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.J
jAverageConf vmcSource VMCv20171101 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.J
jAverageConf vmcSource VMCv20180702 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.J
jAverageConf vmcSource VMCv20181120 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.J
jAverageConf vmcSource, vmcSynopticSource VMCDR1 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -99999999 meta.code
jAverageConf vvvSource, vvvSynopticSource VVVDR4 average confidence in 2 arcsec diameter default aperture (aper3) J real 4   -0.9999995e9 stat.likelihood;em.IR.J
jbestAper videoVariability VIDEODR2 Best aperture (1-6) for photometric statistics in the J band int 4   -9999
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper videoVariability VIDEODR3 Best aperture (1-6) for photometric statistics in the J band int 4   -9999 meta.code.class;em.IR.NIR
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper videoVariability VIDEODR4 Best aperture (1-6) for photometric statistics in the J band int 4   -9999 meta.code.class;em.IR.J
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper videoVariability VIDEODR5 Best aperture (1-6) for photometric statistics in the J band int 4   -9999 meta.code.class;em.IR.J
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper videoVariability VIDEOv20100513 Best aperture (1-6) for photometric statistics in the J band int 4   -9999
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper videoVariability VIDEOv20111208 Best aperture (1-6) for photometric statistics in the J band int 4   -9999
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper vikingVariability VIKINGDR2 Best aperture (1-6) for photometric statistics in the J band int 4   -9999
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper vikingVariability VIKINGDR3 Best aperture (1-6) for photometric statistics in the J band int 4   -9999 meta.code.class;em.IR.NIR
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper vikingVariability VIKINGDR4 Best aperture (1-6) for photometric statistics in the J band int 4   -9999 meta.code.class;em.IR.J
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper vikingVariability VIKINGv20110714 Best aperture (1-6) for photometric statistics in the J band int 4   -9999
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper vikingVariability VIKINGv20111019 Best aperture (1-6) for photometric statistics in the J band int 4   -9999
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper vikingVariability VIKINGv20130417 Best aperture (1-6) for photometric statistics in the J band int 4   -9999 meta.code.class;em.IR.NIR
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper vikingVariability VIKINGv20140402 Best aperture (1-6) for photometric statistics in the J band int 4   -9999 meta.code.class;em.IR.NIR
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper vikingVariability VIKINGv20150421 Best aperture (1-6) for photometric statistics in the J band int 4   -9999 meta.code.class;em.IR.J
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper vikingVariability VIKINGv20151230 Best aperture (1-6) for photometric statistics in the J band int 4   -9999 meta.code.class;em.IR.J
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper vikingVariability VIKINGv20160406 Best aperture (1-6) for photometric statistics in the J band int 4   -9999 meta.code.class;em.IR.J
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper vikingVariability VIKINGv20161202 Best aperture (1-6) for photometric statistics in the J band int 4   -9999 meta.code.class;em.IR.J
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper vikingVariability VIKINGv20170715 Best aperture (1-6) for photometric statistics in the J band int 4   -9999 meta.code.class;em.IR.J
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper vikingVariability VIKINGv20181012 Best aperture (1-6) for photometric statistics in the J band int 4   -9999 meta.code.class;em.IR.J
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper vmcVariability VMCDR1 Best aperture (1-6) for photometric statistics in the J band int 4   -9999
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper vmcVariability VMCDR2 Best aperture (1-6) for photometric statistics in the J band int 4   -9999 meta.code.class;em.IR.NIR
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper vmcVariability VMCDR3 Best aperture (1-6) for photometric statistics in the J band int 4   -9999 meta.code.class;em.IR.J
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper vmcVariability VMCDR4 Best aperture (1-6) for photometric statistics in the J band int 4   -9999 meta.code.class;em.IR.J
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper vmcVariability VMCv20110816 Best aperture (1-6) for photometric statistics in the J band int 4   -9999
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper vmcVariability VMCv20110909 Best aperture (1-6) for photometric statistics in the J band int 4   -9999
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper vmcVariability VMCv20120126 Best aperture (1-6) for photometric statistics in the J band int 4   -9999
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper vmcVariability VMCv20121128 Best aperture (1-6) for photometric statistics in the J band int 4   -9999 meta.code.class;em.IR.NIR
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper vmcVariability VMCv20130304 Best aperture (1-6) for photometric statistics in the J band int 4   -9999 meta.code.class;em.IR.NIR
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper vmcVariability VMCv20130805 Best aperture (1-6) for photometric statistics in the J band int 4   -9999 meta.code.class;em.IR.NIR
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper vmcVariability VMCv20140428 Best aperture (1-6) for photometric statistics in the J band int 4   -9999 meta.code.class;em.IR.J
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper vmcVariability VMCv20140903 Best aperture (1-6) for photometric statistics in the J band int 4   -9999 meta.code.class;em.IR.J
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper vmcVariability VMCv20150309 Best aperture (1-6) for photometric statistics in the J band int 4   -9999 meta.code.class;em.IR.J
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper vmcVariability VMCv20151218 Best aperture (1-6) for photometric statistics in the J band int 4   -9999 meta.code.class;em.IR.J
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper vmcVariability VMCv20160311 Best aperture (1-6) for photometric statistics in the J band int 4   -9999 meta.code.class;em.IR.J
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper vmcVariability VMCv20160822 Best aperture (1-6) for photometric statistics in the J band int 4   -9999 meta.code.class;em.IR.J
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper vmcVariability VMCv20170109 Best aperture (1-6) for photometric statistics in the J band int 4   -9999 meta.code.class;em.IR.J
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper vmcVariability VMCv20170411 Best aperture (1-6) for photometric statistics in the J band int 4   -9999 meta.code.class;em.IR.J
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper vmcVariability VMCv20171101 Best aperture (1-6) for photometric statistics in the J band int 4   -9999 meta.code.class;em.IR.J
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper vmcVariability VMCv20180702 Best aperture (1-6) for photometric statistics in the J band int 4   -9999 meta.code.class;em.IR.J
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbestAper vmcVariability VMCv20181120 Best aperture (1-6) for photometric statistics in the J band int 4   -9999 meta.code.class;em.IR.J
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)
jbStratAst videoVarFrameSetInfo VIDEODR2 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst videoVarFrameSetInfo VIDEODR3 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst videoVarFrameSetInfo VIDEODR4 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst videoVarFrameSetInfo VIDEODR5 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst videoVarFrameSetInfo VIDEOv20100513 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst videoVarFrameSetInfo VIDEOv20111208 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst vikingVarFrameSetInfo VIKINGDR2 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst vikingVarFrameSetInfo VIKINGDR3 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst vikingVarFrameSetInfo VIKINGDR4 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst vikingVarFrameSetInfo VIKINGv20110714 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst vikingVarFrameSetInfo VIKINGv20111019 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst vikingVarFrameSetInfo VIKINGv20130417 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst vikingVarFrameSetInfo VIKINGv20140402 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst vikingVarFrameSetInfo VIKINGv20150421 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst vikingVarFrameSetInfo VIKINGv20151230 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst vikingVarFrameSetInfo VIKINGv20160406 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst vikingVarFrameSetInfo VIKINGv20161202 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst vikingVarFrameSetInfo VIKINGv20170715 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst vikingVarFrameSetInfo VIKINGv20181012 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst vmcVarFrameSetInfo VMCDR1 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst vmcVarFrameSetInfo VMCDR2 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst vmcVarFrameSetInfo VMCDR3 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst vmcVarFrameSetInfo VMCDR4 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst vmcVarFrameSetInfo VMCv20110816 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst vmcVarFrameSetInfo VMCv20110909 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst vmcVarFrameSetInfo VMCv20120126 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst vmcVarFrameSetInfo VMCv20121128 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst vmcVarFrameSetInfo VMCv20130304 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst vmcVarFrameSetInfo VMCv20130805 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst vmcVarFrameSetInfo VMCv20140428 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst vmcVarFrameSetInfo VMCv20140903 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst vmcVarFrameSetInfo VMCv20150309 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst vmcVarFrameSetInfo VMCv20151218 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst vmcVarFrameSetInfo VMCv20160311 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst vmcVarFrameSetInfo VMCv20160822 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst vmcVarFrameSetInfo VMCv20170109 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst vmcVarFrameSetInfo VMCv20170411 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst vmcVarFrameSetInfo VMCv20171101 Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst vmcVarFrameSetInfo VMCv20180702 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratAst vmcVarFrameSetInfo VMCv20181120 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jbStratPht videoVarFrameSetInfo VIDEODR2 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht videoVarFrameSetInfo VIDEODR3 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht videoVarFrameSetInfo VIDEODR4 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht videoVarFrameSetInfo VIDEODR5 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht videoVarFrameSetInfo VIDEOv20100513 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht videoVarFrameSetInfo VIDEOv20111208 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht vikingVarFrameSetInfo VIKINGDR2 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht vikingVarFrameSetInfo VIKINGDR3 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht vikingVarFrameSetInfo VIKINGDR4 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht vikingVarFrameSetInfo VIKINGv20110714 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht vikingVarFrameSetInfo VIKINGv20111019 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht vikingVarFrameSetInfo VIKINGv20130417 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht vikingVarFrameSetInfo VIKINGv20140402 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht vikingVarFrameSetInfo VIKINGv20150421 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht vikingVarFrameSetInfo VIKINGv20151230 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht vikingVarFrameSetInfo VIKINGv20160406 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht vikingVarFrameSetInfo VIKINGv20161202 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht vikingVarFrameSetInfo VIKINGv20170715 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht vikingVarFrameSetInfo VIKINGv20181012 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht vmcVarFrameSetInfo VMCDR1 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht vmcVarFrameSetInfo VMCDR2 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht vmcVarFrameSetInfo VMCDR3 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht vmcVarFrameSetInfo VMCDR4 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht vmcVarFrameSetInfo VMCv20110816 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht vmcVarFrameSetInfo VMCv20110909 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht vmcVarFrameSetInfo VMCv20120126 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht vmcVarFrameSetInfo VMCv20121128 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht vmcVarFrameSetInfo VMCv20130304 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht vmcVarFrameSetInfo VMCv20130805 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht vmcVarFrameSetInfo VMCv20140428 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht vmcVarFrameSetInfo VMCv20140903 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht vmcVarFrameSetInfo VMCv20150309 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht vmcVarFrameSetInfo VMCv20151218 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht vmcVarFrameSetInfo VMCv20160311 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht vmcVarFrameSetInfo VMCv20160822 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht vmcVarFrameSetInfo VMCv20170109 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht vmcVarFrameSetInfo VMCv20170411 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht vmcVarFrameSetInfo VMCv20171101 Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht vmcVarFrameSetInfo VMCv20180702 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jbStratPht vmcVarFrameSetInfo VMCv20181120 Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqAst videoVarFrameSetInfo VIDEODR2 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst videoVarFrameSetInfo VIDEODR3 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst videoVarFrameSetInfo VIDEODR4 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst videoVarFrameSetInfo VIDEODR5 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst videoVarFrameSetInfo VIDEOv20100513 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst videoVarFrameSetInfo VIDEOv20111208 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst vikingVarFrameSetInfo VIKINGDR2 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst vikingVarFrameSetInfo VIKINGDR3 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst vikingVarFrameSetInfo VIKINGDR4 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst vikingVarFrameSetInfo VIKINGv20110714 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst vikingVarFrameSetInfo VIKINGv20111019 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst vikingVarFrameSetInfo VIKINGv20130417 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst vikingVarFrameSetInfo VIKINGv20140402 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst vikingVarFrameSetInfo VIKINGv20150421 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst vikingVarFrameSetInfo VIKINGv20151230 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst vikingVarFrameSetInfo VIKINGv20160406 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst vikingVarFrameSetInfo VIKINGv20161202 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst vikingVarFrameSetInfo VIKINGv20170715 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst vikingVarFrameSetInfo VIKINGv20181012 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst vmcVarFrameSetInfo VMCDR1 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst vmcVarFrameSetInfo VMCDR2 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst vmcVarFrameSetInfo VMCDR3 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst vmcVarFrameSetInfo VMCDR4 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst vmcVarFrameSetInfo VMCv20110816 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst vmcVarFrameSetInfo VMCv20110909 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst vmcVarFrameSetInfo VMCv20120126 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst vmcVarFrameSetInfo VMCv20121128 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst vmcVarFrameSetInfo VMCv20130304 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst vmcVarFrameSetInfo VMCv20130805 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst vmcVarFrameSetInfo VMCv20140428 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst vmcVarFrameSetInfo VMCv20140903 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst vmcVarFrameSetInfo VMCv20150309 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst vmcVarFrameSetInfo VMCv20151218 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst vmcVarFrameSetInfo VMCv20160311 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst vmcVarFrameSetInfo VMCv20160822 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst vmcVarFrameSetInfo VMCv20170109 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst vmcVarFrameSetInfo VMCv20170411 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst vmcVarFrameSetInfo VMCv20171101 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst vmcVarFrameSetInfo VMCv20180702 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqAst vmcVarFrameSetInfo VMCv20181120 Goodness of fit of Strateva function to astrometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jchiSqpd videoVariability VIDEODR2 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd videoVariability VIDEODR3 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd videoVariability VIDEODR4 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.J
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd videoVariability VIDEODR5 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.J
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd videoVariability VIDEOv20100513 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd videoVariability VIDEOv20111208 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd vikingVariability VIKINGDR2 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd vikingVariability VIKINGDR3 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd vikingVariability VIKINGDR4 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.J
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd vikingVariability VIKINGv20110714 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd vikingVariability VIKINGv20111019 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd vikingVariability VIKINGv20130417 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd vikingVariability VIKINGv20140402 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd vikingVariability VIKINGv20150421 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.J
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd vikingVariability VIKINGv20151230 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.J
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd vikingVariability VIKINGv20160406 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.J
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd vikingVariability VIKINGv20161202 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.J
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd vikingVariability VIKINGv20170715 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.J
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd vikingVariability VIKINGv20181012 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.J
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd vmcVariability VMCDR1 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd vmcVariability VMCDR2 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd vmcVariability VMCDR3 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.J
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd vmcVariability VMCDR4 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.J
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd vmcVariability VMCv20110816 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd vmcVariability VMCv20110909 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd vmcVariability VMCv20120126 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd vmcVariability VMCv20121128 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd vmcVariability VMCv20130304 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd vmcVariability VMCv20130805 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd vmcVariability VMCv20140428 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.J
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd vmcVariability VMCv20140903 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.J
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd vmcVariability VMCv20150309 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.J
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd vmcVariability VMCv20151218 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.J
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd vmcVariability VMCv20160311 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.J
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd vmcVariability VMCv20160822 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.J
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd vmcVariability VMCv20170109 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.J
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd vmcVariability VMCv20170411 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.J
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd vmcVariability VMCv20171101 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.J
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd vmcVariability VMCv20180702 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.J
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqpd vmcVariability VMCv20181120 Chi square (per degree of freedom) fit to data (mean and expected rms) real 4   -0.9999995e9 stat.fit.chi2;em.IR.J
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.
jchiSqPht videoVarFrameSetInfo VIDEODR2 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht videoVarFrameSetInfo VIDEODR3 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht videoVarFrameSetInfo VIDEODR4 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht videoVarFrameSetInfo VIDEODR5 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht videoVarFrameSetInfo VIDEOv20100513 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht videoVarFrameSetInfo VIDEOv20111208 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht vikingVarFrameSetInfo VIKINGDR2 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht vikingVarFrameSetInfo VIKINGDR3 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht vikingVarFrameSetInfo VIKINGDR4 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht vikingVarFrameSetInfo VIKINGv20110714 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht vikingVarFrameSetInfo VIKINGv20111019 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht vikingVarFrameSetInfo VIKINGv20130417 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht vikingVarFrameSetInfo VIKINGv20140402 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht vikingVarFrameSetInfo VIKINGv20150421 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht vikingVarFrameSetInfo VIKINGv20151230 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht vikingVarFrameSetInfo VIKINGv20160406 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht vikingVarFrameSetInfo VIKINGv20161202 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht vikingVarFrameSetInfo VIKINGv20170715 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht vikingVarFrameSetInfo VIKINGv20181012 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht vmcVarFrameSetInfo VMCDR1 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht vmcVarFrameSetInfo VMCDR2 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht vmcVarFrameSetInfo VMCDR3 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht vmcVarFrameSetInfo VMCDR4 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht vmcVarFrameSetInfo VMCv20110816 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht vmcVarFrameSetInfo VMCv20110909 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht vmcVarFrameSetInfo VMCv20120126 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht vmcVarFrameSetInfo VMCv20121128 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht vmcVarFrameSetInfo VMCv20130304 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht vmcVarFrameSetInfo VMCv20130805 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht vmcVarFrameSetInfo VMCv20140428 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht vmcVarFrameSetInfo VMCv20140903 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht vmcVarFrameSetInfo VMCv20150309 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht vmcVarFrameSetInfo VMCv20151218 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht vmcVarFrameSetInfo VMCv20160311 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht vmcVarFrameSetInfo VMCv20160822 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht vmcVarFrameSetInfo VMCv20170109 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht vmcVarFrameSetInfo VMCv20170411 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht vmcVarFrameSetInfo VMCv20171101 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht vmcVarFrameSetInfo VMCv20180702 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jchiSqPht vmcVarFrameSetInfo VMCv20181120 Goodness of fit of Strateva function to photometric data in J band real 4   -0.9999995e9 stat.fit.goodness;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
Jclass vvvParallaxCatalogue, vvvProperMotionCatalogue VVVDR4 VVV DR4 J 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: Jclass} int 4   -99999999
jClass vhsSource VHSDR2 discrete image classification flag in J smallint 2   -9999 src.class
jClass vhsSource VHSDR3 discrete image classification flag in J smallint 2   -9999 src.class;em.IR.J
jClass vhsSource VHSDR4 discrete image classification flag in J smallint 2   -9999 src.class;em.IR.J
jClass vhsSource VHSDR6 discrete image classification flag in J smallint 2   -9999 src.class;em.IR.J
jClass vhsSource VHSv20120926 discrete image classification flag in J smallint 2   -9999 src.class
jClass vhsSource VHSv20130417 discrete image classification flag in J smallint 2   -9999 src.class
jClass vhsSource VHSv20140409 discrete image classification flag in J smallint 2   -9999 src.class;em.IR.J
jClass vhsSource VHSv20150108 discrete image classification flag in J smallint 2   -9999 src.class;em.IR.J
jClass vhsSource VHSv20160114 discrete image classification flag in J smallint 2   -9999 src.class;em.IR.J
jClass vhsSource VHSv20160507 discrete image classification flag in J smallint 2   -9999 src.class;em.IR.J
jClass vhsSource VHSv20170630 discrete image classification flag in J smallint 2   -9999 src.class;em.IR.J
jClass vhsSource VHSv20180419 discrete image classification flag in J smallint 2   -9999 src.class;em.IR.J
jClass vhsSource, vhsSourceRemeasurement VHSDR1 discrete image classification flag in J smallint 2   -9999 src.class
jClass videoSource VIDEODR2 discrete image classification flag in J smallint 2   -9999 src.class
jClass videoSource VIDEODR3 discrete image classification flag in J smallint 2   -9999 src.class
jClass videoSource VIDEODR4 discrete image classification flag in J smallint 2   -9999 src.class;em.IR.J
jClass videoSource VIDEODR5 discrete image classification flag in J smallint 2   -9999 src.class;em.IR.J
jClass videoSource VIDEOv20111208 discrete image classification flag in J smallint 2   -9999 src.class
jClass videoSource, videoSourceRemeasurement VIDEOv20100513 discrete image classification flag in J smallint 2   -9999 src.class
jClass vikingSource VIKINGDR2 discrete image classification flag in J smallint 2   -9999 src.class
jClass vikingSource VIKINGDR3 discrete image classification flag in J smallint 2   -9999 src.class
jClass vikingSource VIKINGDR4 discrete image classification flag in J smallint 2   -9999 src.class;em.IR.J
jClass vikingSource VIKINGv20111019 discrete image classification flag in J smallint 2   -9999 src.class
jClass vikingSource VIKINGv20130417 discrete image classification flag in J smallint 2   -9999 src.class
jClass vikingSource VIKINGv20140402 discrete image classification flag in J smallint 2   -9999 src.class
jClass vikingSource VIKINGv20150421 discrete image classification flag in J smallint 2   -9999 src.class;em.IR.J
jClass vikingSource VIKINGv20151230 discrete image classification flag in J smallint 2   -9999 src.class;em.IR.J
jClass vikingSource VIKINGv20160406 discrete image classification flag in J smallint 2   -9999 src.class;em.IR.J
jClass vikingSource VIKINGv20161202 discrete image classification flag in J smallint 2   -9999 src.class;em.IR.J
jClass vikingSource VIKINGv20170715 discrete image classification flag in J smallint 2   -9999 src.class;em.IR.J
jClass vikingSource VIKINGv20181012 discrete image classification flag in J smallint 2   -9999 src.class;em.IR.J
jClass vikingSource, vikingSourceRemeasurement VIKINGv20110714 discrete image classification flag in J smallint 2   -9999 src.class
jClass vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 discrete image classification flag in J smallint 2   -9999 src.class
jClass vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 discrete image classification flag in J smallint 2   -9999 src.class
jClass vmcSource VMCDR2 discrete image classification flag in J smallint 2   -9999 src.class
jClass vmcSource VMCDR3 discrete image classification flag in J smallint 2   -9999 src.class;em.IR.J
jClass vmcSource VMCDR4 discrete image classification flag in J smallint 2   -9999 src.class;em.IR.J
jClass vmcSource VMCv20110909 discrete image classification flag in J smallint 2   -9999 src.class
jClass vmcSource VMCv20120126 discrete image classification flag in J smallint 2   -9999 src.class
jClass vmcSource VMCv20121128 discrete image classification flag in J smallint 2   -9999 src.class
jClass vmcSource VMCv20130304 discrete image classification flag in J smallint 2   -9999 src.class
jClass vmcSource VMCv20130805 discrete image classification flag in J smallint 2   -9999 src.class
jClass vmcSource VMCv20140428 discrete image classification flag in J smallint 2   -9999 src.class;em.IR.J
jClass vmcSource VMCv20140903 discrete image classification flag in J smallint 2   -9999 src.class;em.IR.J
jClass vmcSource VMCv20150309 discrete image classification flag in J smallint 2   -9999 src.class;em.IR.J
jClass vmcSource VMCv20151218 discrete image classification flag in J smallint 2   -9999 src.class;em.IR.J
jClass vmcSource VMCv20160311 discrete image classification flag in J smallint 2   -9999 src.class;em.IR.J
jClass vmcSource VMCv20160822 discrete image classification flag in J smallint 2   -9999 src.class;em.IR.J
jClass vmcSource VMCv20170109 discrete image classification flag in J smallint 2   -9999 src.class;em.IR.J
jClass vmcSource VMCv20170411 discrete image classification flag in J smallint 2   -9999 src.class;em.IR.J
jClass vmcSource VMCv20171101 discrete image classification flag in J smallint 2   -9999 src.class;em.IR.J
jClass vmcSource VMCv20180702 discrete image classification flag in J smallint 2   -9999 src.class;em.IR.J
jClass vmcSource VMCv20181120 discrete image classification flag in J smallint 2   -9999 src.class;em.IR.J
jClass vmcSource, vmcSourceRemeasurement VMCv20110816 discrete image classification flag in J smallint 2   -9999 src.class
jClass vmcSource, vmcSynopticSource VMCDR1 discrete image classification flag in J smallint 2   -9999 src.class
jClass vvvSource, vvvSynopticSource VVVDR4 discrete image classification flag in J smallint 2   -9999 src.class;em.IR.J
jClassStat vhsSource VHSDR2 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat
jClassStat vhsSource VHSDR3 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat;em.IR.J
jClassStat vhsSource VHSDR4 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat;em.IR.J
jClassStat vhsSource VHSDR6 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat;em.IR.J
jClassStat vhsSource VHSv20120926 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat
jClassStat vhsSource VHSv20130417 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat
jClassStat vhsSource VHSv20140409 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat;em.IR.J
jClassStat vhsSource VHSv20150108 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat;em.IR.J
jClassStat vhsSource VHSv20160114 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat;em.IR.J
jClassStat vhsSource VHSv20160507 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat;em.IR.J
jClassStat vhsSource VHSv20170630 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat;em.IR.J
jClassStat vhsSource VHSv20180419 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat;em.IR.J
jClassStat vhsSource, vhsSourceRemeasurement VHSDR1 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat
jClassStat videoSource VIDEODR2 S-Extractor classification statistic in J real 4   -0.9999995e9 stat
jClassStat videoSource VIDEODR3 S-Extractor classification statistic in J real 4   -0.9999995e9 stat
jClassStat videoSource VIDEODR4 S-Extractor classification statistic in J real 4   -0.9999995e9 stat;em.IR.J
jClassStat videoSource VIDEODR5 S-Extractor classification statistic in J real 4   -0.9999995e9 stat;em.IR.J
jClassStat videoSource VIDEOv20100513 S-Extractor classification statistic in J real 4   -0.9999995e9 stat
jClassStat videoSource VIDEOv20111208 S-Extractor classification statistic in J real 4   -0.9999995e9 stat
jClassStat videoSourceRemeasurement VIDEOv20100513 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat
jClassStat vikingSource VIKINGDR2 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat
jClassStat vikingSource VIKINGDR3 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat
jClassStat vikingSource VIKINGDR4 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat;em.IR.J
jClassStat vikingSource VIKINGv20111019 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat
jClassStat vikingSource VIKINGv20130417 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat
jClassStat vikingSource VIKINGv20140402 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat
jClassStat vikingSource VIKINGv20150421 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat;em.IR.J
jClassStat vikingSource VIKINGv20151230 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat;em.IR.J
jClassStat vikingSource VIKINGv20160406 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat;em.IR.J
jClassStat vikingSource VIKINGv20161202 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat;em.IR.J
jClassStat vikingSource VIKINGv20170715 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat;em.IR.J
jClassStat vikingSource VIKINGv20181012 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat;em.IR.J
jClassStat vikingSource, vikingSourceRemeasurement VIKINGv20110714 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat
jClassStat vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat
jClassStat vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat
jClassStat vmcSource VMCDR2 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat
jClassStat vmcSource VMCDR3 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat;em.IR.J
jClassStat vmcSource VMCDR4 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat;em.IR.J
jClassStat vmcSource VMCv20110909 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat
jClassStat vmcSource VMCv20120126 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat
jClassStat vmcSource VMCv20121128 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat
jClassStat vmcSource VMCv20130304 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat
jClassStat vmcSource VMCv20130805 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat
jClassStat vmcSource VMCv20140428 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat;em.IR.J
jClassStat vmcSource VMCv20140903 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat;em.IR.J
jClassStat vmcSource VMCv20150309 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat;em.IR.J
jClassStat vmcSource VMCv20151218 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat;em.IR.J
jClassStat vmcSource VMCv20160311 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat;em.IR.J
jClassStat vmcSource VMCv20160822 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat;em.IR.J
jClassStat vmcSource VMCv20170109 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat;em.IR.J
jClassStat vmcSource VMCv20170411 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat;em.IR.J
jClassStat vmcSource VMCv20171101 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat;em.IR.J
jClassStat vmcSource VMCv20180702 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat;em.IR.J
jClassStat vmcSource VMCv20181120 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat;em.IR.J
jClassStat vmcSource, vmcSourceRemeasurement VMCv20110816 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat
jClassStat vmcSource, vmcSynopticSource VMCDR1 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat
jClassStat vvvSource VVVDR4 S-Extractor classification statistic in J real 4   -0.9999995e9 stat;em.IR.J
jClassStat vvvSynopticSource VVVDR4 N(0,1) stellarness-of-profile statistic in J real 4   -0.9999995e9 stat;em.IR.J
jCorr twompzPhotoz TWOMPZ J 20mag/sq." isophotal fiducial ell. ap. magnitude with Galactic dust correction {image primary HDU keyword: Jcorr} real 4 mag -0.9999995e9 phot.mag;em.IR.J
jCorrErr twompzPhotoz TWOMPZ J 1-sigma uncertainty in 20mag/sq." aperture {image primary HDU keyword: j_msig_k20fe} real 4 mag -0.9999995e9
jcStratAst videoVarFrameSetInfo VIDEODR2 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst videoVarFrameSetInfo VIDEODR3 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst videoVarFrameSetInfo VIDEODR4 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst videoVarFrameSetInfo VIDEODR5 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst videoVarFrameSetInfo VIDEOv20100513 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst videoVarFrameSetInfo VIDEOv20111208 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst vikingVarFrameSetInfo VIKINGDR2 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst vikingVarFrameSetInfo VIKINGDR3 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst vikingVarFrameSetInfo VIKINGDR4 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst vikingVarFrameSetInfo VIKINGv20110714 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst vikingVarFrameSetInfo VIKINGv20111019 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst vikingVarFrameSetInfo VIKINGv20130417 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst vikingVarFrameSetInfo VIKINGv20140402 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst vikingVarFrameSetInfo VIKINGv20150421 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst vikingVarFrameSetInfo VIKINGv20151230 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst vikingVarFrameSetInfo VIKINGv20160406 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst vikingVarFrameSetInfo VIKINGv20161202 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst vikingVarFrameSetInfo VIKINGv20170715 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst vikingVarFrameSetInfo VIKINGv20181012 Parameter, c2 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst vmcVarFrameSetInfo VMCDR1 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst vmcVarFrameSetInfo VMCDR2 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst vmcVarFrameSetInfo VMCDR3 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst vmcVarFrameSetInfo VMCDR4 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst vmcVarFrameSetInfo VMCv20110816 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst vmcVarFrameSetInfo VMCv20110909 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst vmcVarFrameSetInfo VMCv20120126 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst vmcVarFrameSetInfo VMCv20121128 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst vmcVarFrameSetInfo VMCv20130304 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst vmcVarFrameSetInfo VMCv20130805 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst vmcVarFrameSetInfo VMCv20140428 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst vmcVarFrameSetInfo VMCv20140903 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst vmcVarFrameSetInfo VMCv20150309 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst vmcVarFrameSetInfo VMCv20151218 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst vmcVarFrameSetInfo VMCv20160311 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst vmcVarFrameSetInfo VMCv20160822 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst vmcVarFrameSetInfo VMCv20170109 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst vmcVarFrameSetInfo VMCv20170411 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst vmcVarFrameSetInfo VMCv20171101 Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst vmcVarFrameSetInfo VMCv20180702 Parameter, c2 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratAst vmcVarFrameSetInfo VMCv20181120 Parameter, c2 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in J band. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.
jcStratPht videoVarFrameSetInfo VIDEODR2 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht videoVarFrameSetInfo VIDEODR3 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht videoVarFrameSetInfo VIDEODR4 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht videoVarFrameSetInfo VIDEODR5 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht videoVarFrameSetInfo VIDEOv20100513 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht videoVarFrameSetInfo VIDEOv20111208 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht vikingVarFrameSetInfo VIKINGDR2 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht vikingVarFrameSetInfo VIKINGDR3 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht vikingVarFrameSetInfo VIKINGDR4 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht vikingVarFrameSetInfo VIKINGv20110714 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht vikingVarFrameSetInfo VIKINGv20111019 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht vikingVarFrameSetInfo VIKINGv20130417 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht vikingVarFrameSetInfo VIKINGv20140402 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht vikingVarFrameSetInfo VIKINGv20150421 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht vikingVarFrameSetInfo VIKINGv20151230 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht vikingVarFrameSetInfo VIKINGv20160406 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht vikingVarFrameSetInfo VIKINGv20161202 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht vikingVarFrameSetInfo VIKINGv20170715 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht vikingVarFrameSetInfo VIKINGv20181012 Parameter, c2 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht vmcVarFrameSetInfo VMCDR1 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht vmcVarFrameSetInfo VMCDR2 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht vmcVarFrameSetInfo VMCDR3 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht vmcVarFrameSetInfo VMCDR4 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht vmcVarFrameSetInfo VMCv20110816 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht vmcVarFrameSetInfo VMCv20110909 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht vmcVarFrameSetInfo VMCv20120126 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht vmcVarFrameSetInfo VMCv20121128 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht vmcVarFrameSetInfo VMCv20130304 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht vmcVarFrameSetInfo VMCv20130805 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.NIR
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht vmcVarFrameSetInfo VMCv20140428 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht vmcVarFrameSetInfo VMCv20140903 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht vmcVarFrameSetInfo VMCv20150309 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht vmcVarFrameSetInfo VMCv20151218 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht vmcVarFrameSetInfo VMCv20160311 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht vmcVarFrameSetInfo VMCv20160822 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht vmcVarFrameSetInfo VMCv20170109 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht vmcVarFrameSetInfo VMCv20170411 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht vmcVarFrameSetInfo VMCv20171101 Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht vmcVarFrameSetInfo VMCv20180702 Parameter, c2 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jcStratPht vmcVarFrameSetInfo VMCv20181120 Parameter, c2 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in J band. real 4   -0.9999995e9 stat.fit.param;em.IR.J
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.
jdate twomass_psc TWOMASS The Julian Date of the source measurement accurate to +-30 seconds. float 8 Julian days   time.epoch
jdate twomass_scn TWOMASS Julian Date at beginning of scan. float 8 Julian days   time.epoch
jdate twomass_sixx2_psc TWOMASS julian date of source measurement to +/- 30 sec float 8 jdate
jdate twomass_sixx2_scn TWOMASS Julian date beginning UT of scan data float 8 jdate
jdate twomass_xsc TWOMASS Julian date of the source measurement accurate to +-3 minutes. float 8 Julian days   time.epoch
jDeblend vhsSourceRemeasurement VHSDR1 placeholder flag indicating parent/child relation in J int 4   -99999999 meta.code
jDeblend videoSource, videoSourceRemeasurement VIDEOv20100513 placeholder flag indicating parent/child relation in J int 4   -99999999 meta.code
jDeblend vikingSourceRemeasurement VIKINGv20110714 placeholder flag indicating parent/child relation in J int 4   -99999999 meta.code
jDeblend vikingSourceRemeasurement VIKINGv20111019 placeholder flag indicating parent/child relation in J int 4   -99999999 meta.code
jDeblend vmcSourceRemeasurement VMCv20110816 placeholder flag indicating parent/child relation in J int 4   -99999999 meta.code
jDeblend vmcSourceRemeasurement VMCv20110909 placeholder flag indicating parent/child relation in J int 4   -99999999 meta.code
Jell vvvParallaxCatalogue, vvvProperMotionCatalogue VVVDR4 Ellipticity of the DR4 J detection. {catalogue TType keyword: Jell} real 4   -999999500.0
jEll vhsSource VHSDR2 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity
jEll vhsSource VHSDR3 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity;em.IR.J
jEll vhsSource VHSDR4 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity;em.IR.J
jEll vhsSource VHSDR6 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity;em.IR.J
jEll vhsSource VHSv20120926 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity
jEll vhsSource VHSv20130417 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity
jEll vhsSource VHSv20140409 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity;em.IR.J
jEll vhsSource VHSv20150108 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity;em.IR.J
jEll vhsSource VHSv20160114 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity;em.IR.J
jEll vhsSource VHSv20160507 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity;em.IR.J
jEll vhsSource VHSv20170630 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity;em.IR.J
jEll vhsSource VHSv20180419 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity;em.IR.J
jEll vhsSource, vhsSourceRemeasurement VHSDR1 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity
jEll videoSource VIDEODR2 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity
jEll videoSource VIDEODR3 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity
jEll videoSource VIDEODR4 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity;em.IR.J
jEll videoSource VIDEODR5 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity;em.IR.J
jEll videoSource VIDEOv20111208 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity
jEll videoSource, videoSourceRemeasurement VIDEOv20100513 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity
jEll vikingSource VIKINGDR2 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity
jEll vikingSource VIKINGDR3 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity
jEll vikingSource VIKINGDR4 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity;em.IR.J
jEll vikingSource VIKINGv20111019 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity
jEll vikingSource VIKINGv20130417 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity
jEll vikingSource VIKINGv20140402 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity
jEll vikingSource VIKINGv20150421 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity;em.IR.J
jEll vikingSource VIKINGv20151230 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity;em.IR.J
jEll vikingSource VIKINGv20160406 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity;em.IR.J
jEll vikingSource VIKINGv20161202 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity;em.IR.J
jEll vikingSource VIKINGv20170715 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity;em.IR.J
jEll vikingSource VIKINGv20181012 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity;em.IR.J
jEll vikingSource, vikingSourceRemeasurement VIKINGv20110714 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity
jEll vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity
jEll vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity
jEll vmcSource VMCDR2 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity
jEll vmcSource VMCDR3 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity;em.IR.J
jEll vmcSource VMCDR4 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity;em.IR.J
jEll vmcSource VMCv20110909 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity
jEll vmcSource VMCv20120126 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity
jEll vmcSource VMCv20121128 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity
jEll vmcSource VMCv20130304 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity
jEll vmcSource VMCv20130805 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity
jEll vmcSource VMCv20140428 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity;em.IR.J
jEll vmcSource VMCv20140903 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity;em.IR.J
jEll vmcSource VMCv20150309 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity;em.IR.J
jEll vmcSource VMCv20151218 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity;em.IR.J
jEll vmcSource VMCv20160311 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity;em.IR.J
jEll vmcSource VMCv20160822 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity;em.IR.J
jEll vmcSource VMCv20170109 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity;em.IR.J
jEll vmcSource VMCv20170411 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity;em.IR.J
jEll vmcSource VMCv20171101 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity;em.IR.J
jEll vmcSource VMCv20180702 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity;em.IR.J
jEll vmcSource VMCv20181120 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity;em.IR.J
jEll vmcSource, vmcSourceRemeasurement VMCv20110816 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity
jEll vmcSource, vmcSynopticSource VMCDR1 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity
jEll vvvSource, vvvSynopticSource VVVDR4 1-b/a, where a/b=semi-major/minor axes in J real 4   -0.9999995e9 src.ellipticity;em.IR.J
jeNum vhsMergeLog VHSDR1 the extension number of this J frame tinyint 1     meta.number
jeNum vhsMergeLog VHSDR2 the extension number of this J frame tinyint 1     meta.number
jeNum vhsMergeLog VHSDR3 the extension number of this J frame tinyint 1     meta.number;em.IR.J
jeNum vhsMergeLog VHSDR4 the extension number of this J frame tinyint 1     meta.number;em.IR.J
jeNum vhsMergeLog VHSDR6 the extension number of this J frame tinyint 1     meta.number;em.IR.J
jeNum vhsMergeLog VHSv20120926 the extension number of this J frame tinyint 1     meta.number
jeNum vhsMergeLog VHSv20130417 the extension number of this J frame tinyint 1     meta.number
jeNum vhsMergeLog VHSv20140409 the extension number of this J frame tinyint 1     meta.number;em.IR.J
jeNum vhsMergeLog VHSv20150108 the extension number of this J frame tinyint 1     meta.number;em.IR.J
jeNum vhsMergeLog VHSv20160114 the extension number of this J frame tinyint 1     meta.number;em.IR.J
jeNum vhsMergeLog VHSv20160507 the extension number of this J frame tinyint 1     meta.number;em.IR.J
jeNum vhsMergeLog VHSv20170630 the extension number of this J frame tinyint 1     meta.number;em.IR.J
jeNum vhsMergeLog VHSv20180419 the extension number of this J frame tinyint 1     meta.number;em.IR.J
jeNum videoMergeLog VIDEODR2 the extension number of this J frame tinyint 1     meta.number
jeNum videoMergeLog VIDEODR3 the extension number of this J frame tinyint 1     meta.number
jeNum videoMergeLog VIDEODR4 the extension number of this J frame tinyint 1     meta.number;em.IR.J
jeNum videoMergeLog VIDEODR5 the extension number of this J frame tinyint 1     meta.number;em.IR.J
jeNum videoMergeLog VIDEOv20100513 the extension number of this J frame tinyint 1     meta.number
jeNum videoMergeLog VIDEOv20111208 the extension number of this J frame tinyint 1     meta.number
jeNum vikingMergeLog VIKINGDR2 the extension number of this J frame tinyint 1     meta.number
jeNum vikingMergeLog VIKINGDR3 the extension number of this J frame tinyint 1     meta.number
jeNum vikingMergeLog VIKINGDR4 the extension number of this J frame tinyint 1     meta.number;em.IR.J
jeNum vikingMergeLog VIKINGv20110714 the extension number of this J frame tinyint 1     meta.number
jeNum vikingMergeLog VIKINGv20111019 the extension number of this J frame tinyint 1     meta.number
jeNum vikingMergeLog VIKINGv20130417 the extension number of this J frame tinyint 1     meta.number
jeNum vikingMergeLog VIKINGv20140402 the extension number of this J frame tinyint 1     meta.number
jeNum vikingMergeLog VIKINGv20150421 the extension number of this J frame tinyint 1     meta.number;em.IR.J
jeNum vikingMergeLog VIKINGv20151230 the extension number of this J frame tinyint 1     meta.number;em.IR.J
jeNum vikingMergeLog VIKINGv20160406 the extension number of this J frame tinyint 1     meta.number;em.IR.J
jeNum vikingMergeLog VIKINGv20161202 the extension number of this J frame tinyint 1     meta.number;em.IR.J
jeNum vikingMergeLog VIKINGv20170715 the extension number of this J frame tinyint 1     meta.number;em.IR.J
jeNum vikingMergeLog VIKINGv20181012 the extension number of this J frame tinyint 1     meta.number;em.IR.J
jeNum vikingZY_selJ_RemeasMergeLog VIKINGZYSELJv20160909 the extension number of this J frame tinyint 1     meta.number
jeNum vikingZY_selJ_RemeasMergeLog VIKINGZYSELJv20170124 the extension number of this J frame tinyint 1     meta.number
jeNum vmcMergeLog VMCDR2 the extension number of this J frame tinyint 1     meta.number
jeNum vmcMergeLog VMCDR3 the extension number of this J frame tinyint 1     meta.number;em.IR.J
jeNum vmcMergeLog VMCDR4 the extension number of this J frame tinyint 1     meta.number;em.IR.J
jeNum vmcMergeLog VMCv20110816 the extension number of this J frame tinyint 1     meta.number
jeNum vmcMergeLog VMCv20110909 the extension number of this J frame tinyint 1     meta.number
jeNum vmcMergeLog VMCv20120126 the extension number of this J frame tinyint 1     meta.number
jeNum vmcMergeLog VMCv20121128 the extension number of this J frame tinyint 1     meta.number
jeNum vmcMergeLog VMCv20130304 the extension number of this J frame tinyint 1     meta.number
jeNum vmcMergeLog VMCv20130805 the extension number of this J frame tinyint 1     meta.number
jeNum vmcMergeLog VMCv20140428 the extension number of this J frame tinyint 1     meta.number;em.IR.J
jeNum vmcMergeLog VMCv20140903 the extension number of this J frame tinyint 1     meta.number;em.IR.J
jeNum vmcMergeLog VMCv20150309 the extension number of this J frame tinyint 1     meta.number;em.IR.J
jeNum vmcMergeLog VMCv20151218 the extension number of this J frame tinyint 1     meta.number;em.IR.J
jeNum vmcMergeLog VMCv20160311 the extension number of this J frame tinyint 1     meta.number;em.IR.J
jeNum vmcMergeLog VMCv20160822 the extension number of this J frame tinyint 1     meta.number;em.IR.J
jeNum vmcMergeLog VMCv20170109 the extension number of this J frame tinyint 1     meta.number;em.IR.J
jeNum vmcMergeLog VMCv20170411 the extension number of this J frame tinyint 1     meta.number;em.IR.J
jeNum vmcMergeLog VMCv20171101 the extension number of this J frame tinyint 1     meta.number;em.IR.J
jeNum vmcMergeLog VMCv20180702 the extension number of this J frame tinyint 1     meta.number;em.IR.J
jeNum vmcMergeLog VMCv20181120 the extension number of this J frame tinyint 1     meta.number;em.IR.J
jeNum vmcMergeLog, vmcSynopticMergeLog VMCDR1 the extension number of this J frame tinyint 1     meta.number
jeNum vvvMergeLog, vvvPsfDaophotJKsMergeLog, vvvSynopticMergeLog VVVDR4 the extension number of this J frame tinyint 1     meta.number;em.IR.J
jErrBits vhsSource VHSDR1 processing warning/error bitwise flags in J 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.
jErrBits vhsSource VHSDR2 processing warning/error bitwise flags in J 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.
jErrBits vhsSource VHSDR3 processing warning/error bitwise flags in J int 4   -99999999 meta.code;em.IR.J
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
jErrBits vhsSource VHSDR4 processing warning/error bitwise flags in J int 4   -99999999 meta.code;em.IR.J
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
jErrBits vhsSource VHSDR6 processing warning/error bitwise flags in J int 4   -99999999 meta.code;em.IR.J
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
jErrBits vhsSource VHSv20120926 processing warning/error bitwise flags in J 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.
jErrBits vhsSource VHSv20130417 processing warning/error bitwise flags in J 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.
jErrBits vhsSource VHSv20140409 processing warning/error bitwise flags in J int 4   -99999999 meta.code;em.IR.J
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
jErrBits vhsSource VHSv20150108 processing warning/error bitwise flags in J int 4   -99999999 meta.code;em.IR.J
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
jErrBits vhsSource VHSv20160114 processing warning/error bitwise flags in J int 4   -99999999 meta.code;em.IR.J
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
jErrBits vhsSource VHSv20160507 processing warning/error bitwise flags in J int 4   -99999999 meta.code;em.IR.J
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
jErrBits vhsSource VHSv20170630 processing warning/error bitwise flags in J int 4   -99999999 meta.code;em.IR.J
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
jErrBits vhsSource VHSv20180419 processing warning/error bitwise flags in J int 4   -99999999 meta.code;em.IR.J
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
jErrBits vhsSourceRemeasurement VHSDR1 processing warning/error bitwise flags in J int 4   -99999999 meta.code
jErrBits videoSource VIDEODR2 processing warning/error bitwise flags in J 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

jErrBits videoSource VIDEODR3 processing warning/error bitwise flags in J 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

jErrBits videoSource VIDEODR4 processing warning/error bitwise flags in J int 4   -99999999 meta.code;em.IR.J
This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows:
 Bit Flag Meaning 1 The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected). 2 The object was originally blended with another 4 At least one pixel is saturated (or very close to) 8 The object is truncated (too close to an image boundary) 16 Object's aperture data are incomplete or corrupted 32 Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters. 64 Memory overflow occurred during deblending 128 Memory overflow occurred during extraction

jErrBits videoSource VIDEODR5 processing warning/error bitwise flags in J int 4   -99999999 meta.code;em.IR.J
This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows:
 Bit Flag Meaning 1 The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected). 2 The object was originally blended with another 4 At least one pixel is saturated (or very close to) 8 The object is truncated (too close to an image boundary) 16 Object's aperture data are incomplete or corrupted 32 Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters. 64 Memory overflow occurred during deblending 128 Memory overflow occurred during extraction

jErrBits videoSource VIDEOv20100513 processing warning/error bitwise flags in J 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

jErrBits videoSource VIDEOv20111208 processing warning/error bitwise flags in J 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

jErrBits videoSourceRemeasurement VIDEOv20100513 processing warning/error bitwise flags in J int 4   -99999999 meta.code
jErrBits vikingSource VIKINGDR2 processing warning/error bitwise flags in J 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.
jErrBits vikingSource VIKINGDR3 processing warning/error bitwise flags in J 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.
jErrBits vikingSource VIKINGDR4 processing warning/error bitwise flags in J int 4   -99999999 meta.code;em.IR.J
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
jErrBits vikingSource VIKINGv20110714 processing warning/error bitwise flags in J 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.
jErrBits vikingSource VIKINGv20111019 processing warning/error bitwise flags in J 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.
jErrBits vikingSource VIKINGv20130417 processing warning/error bitwise flags in J 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.
jErrBits vikingSource VIKINGv20140402 processing warning/error bitwise flags in J 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.
jErrBits vikingSource VIKINGv20150421 processing warning/error bitwise flags in J int 4   -99999999 meta.code;em.IR.J
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
jErrBits vikingSource VIKINGv20151230 processing warning/error bitwise flags in J int 4   -99999999 meta.code;em.IR.J
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
jErrBits vikingSource VIKINGv20160406 processing warning/error bitwise flags in J int 4   -99999999 meta.code;em.IR.J
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
jErrBits vikingSource VIKINGv20161202 processing warning/error bitwise flags in J int 4   -99999999 meta.code;em.IR.J
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
jErrBits vikingSource VIKINGv20170715 processing warning/error bitwise flags in J int 4   -99999999 meta.code;em.IR.J
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
jErrBits vikingSource VIKINGv20181012 processing warning/error bitwise flags in J int 4   -99999999 meta.code;em.IR.J
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
jErrBits vikingSourceRemeasurement VIKINGv20110714 processing warning/error bitwise flags in J int 4   -99999999 meta.code
jErrBits vikingSourceRemeasurement VIKINGv20111019 processing warning/error bitwise flags in J int 4   -99999999 meta.code
jErrBits vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20160909 processing warning/error bitwise flags in J 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.
jErrBits vikingZY_selJ_SourceRemeasurement VIKINGZYSELJv20170124 processing warning/error bitwise flags in J 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.
jErrBits vmcSource VMCDR2 processing warning/error bitwise flags in J 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.
jErrBits vmcSource VMCDR3 processing warning/error bitwise flags in J int 4   -99999999 meta.code;em.IR.J
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
jErrBits vmcSource VMCDR4 processing warning/error bitwise flags in J int 4   -99999999 meta.code;em.IR.J
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.
jErrBits vmcSource VMCv20110816 processing warning/error bitwise flags in J 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.
jErrBits vmcSource VMCv20110909 processing warning/error bitwise flags in J 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.
jErrBits vmcSource VMCv20120126 processing warning/error bitwise flags in J 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.
jErrBits vmcSource VMCv20121128 processing warning/error bitwise flags in J int 4   -99999999 meta.code
Apparently not actuall