J 
Name  Schema Table  Database  Description  Type  Length  Unit  Default Value  Unified Content Descriptor 
j_1AperMag3 
lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource 
WSA 
Default point source J_1 aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
j_1AperMag3 
lasSource 
WSA 
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_1AperMag3Err 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
Error in default point source J_1 mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
j_1AperMag4 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
Point source J_1 aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
j_1AperMag4Err 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
Error in point source J_1 mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
j_1AperMag6 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
Point source J_1 aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
j_1AperMag6Err 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
Error in point source J_1 mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
j_1Class 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
discrete image classification flag in J_1 
smallint 
2 

9999 
CLASS_MISC 
j_1ClassStat 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
N(0,1) stellarnessofprofile statistic in J_1 
real 
4 

0.9999995e9 
STAT_PROP 
j_1Deblend 
lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource 
WSA 
placeholder flag indicating parent/child relation in J_1 
int 
4 

99999999 
CODE_MISC 
j_1Deblend 
lasSource 
WSA 
placeholder flag indicating parent/child relation in J_1 
int 
4 

99999999 
CODE_MISC 
This CASU pipeline processing source extraction flag is a placeholder only, and is always set to zero in all passbands in the merged source lists. If you need to know when a particular image detection is a component of a deblend or not, test bit 4 of attribute ppErrBits (see corresponding glossary entry) which is set by WFAU's postprocessing software based on testing the areal profiles aprof28 (these are set by CASU to 1 for deblended components, or positive values for nondeblended detections). We encode this in an information bit of ppErrBits for convenience when querying the merged source tables. 
j_1Ell 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
1b/a, where a/b=semimajor/minor axes in J_1 
real 
4 

0.9999995e9 
PHYS_ELLIPTICITY 
j_1eNum 
lasMergeLog, lasYJHKmergeLog 
WSA 
the extension number of this J_1 frame 
tinyint 
1 


NUMBER 
j_1ErrBits 
lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource 
WSA 
processing warning/error bitwise flags in J_1 
int 
4 

99999999 
CODE_MISC 
j_1ErrBits 
lasSource 
WSA 
processing warning/error bitwise flags in J_1 
int 
4 

99999999 
CODE_MISC 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
j_1Eta 
lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource 
WSA 
Offset of J_1 detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
POS_EQ_DEC_OFF 
j_1Eta 
lasSource 
WSA 
Offset of J_1 detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
POS_EQ_DEC_OFF 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 2.0 (UKIDSS LAS and GPS; UHS; also nonsurvey programmes) or 1.0 (UKIDSS GPS, DXS and UDS) arcseconds is used, the higher value enabling pairing of moving sources when epoch separations may be several years. 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 LAS, you might wish to insist that the offsets in the selected sample are all below 1 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 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
RMS of axes of ellipse fit in J_1 
real 
4 
pixels 
0.9999995e9 
MORPH_PARAM 
j_1HallMag 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
Total point source J_1 mag 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
j_1HallMagErr 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
Error in total point source J_1 mag 
real 
4 
mag 
0.9999995e9 
ERROR 
j_1mfID 
lasMergeLog, lasYJHKmergeLog 
WSA 
the UID of the relevant J_1 multiframe 
bigint 
8 


ID_FRAME 
j_1mhExt 
lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource 
WSA 
Extended source colour J_1H (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
j_1mhExt 
lasSource 
WSA 
Extended source colour J_1H (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
j_1mhExtErr 
lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource 
WSA 
Error on extended source colour J_1H 
real 
4 
mag 
0.9999995e9 
ERROR 
j_1mhExtErr 
lasSource 
WSA 
Error on extended source colour J_1H 
real 
4 
mag 
0.9999995e9 
ERROR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
j_1mhPnt 
lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource 
WSA 
Point source colour J_1H (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
j_1mhPnt 
lasSource 
WSA 
Point source colour J_1H (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
j_1mhPntErr 
lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource 
WSA 
Error on point source colour J_1H 
real 
4 
mag 
0.9999995e9 
ERROR 
j_1mhPntErr 
lasSource 
WSA 
Error on point source colour J_1H 
real 
4 
mag 
0.9999995e9 
ERROR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
j_1PA 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
ellipse fit celestial orientation in J_1 
real 
4 
Degrees 
0.9999995e9 
POS_POSANG 
j_1PetroMag 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
Extended source J_1 mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
j_1PetroMagErr 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
Error in extended source J_1 mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
ERROR 
j_1ppErrBits 
lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource 
WSA 
additional WFAU postprocessing error bits in J_1 
int 
4 

0 
CODE_MISC 
j_1ppErrBits 
lasSource 
WSA 
additional WFAU postprocessing error bits in J_1 
int 
4 

0 
CODE_MISC 
Postprocessing error quality bit flags assigned (NB: from UKIDSS DR2 release onwards) in the WSA curation procedure for survey data. From least to most significant byte in the 4byte 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  1  15  Source in poor flat field region  32768  0x00008000  All but mosaics  2  16  Close to saturated  65536  0x00010000  All VDFS catalogues (though deeps excluded prior to DR8)  2  17  Photometric calibration probably subject to systematic error  131072  0x00020000  GPS only  2  19  Possible crosstalk artefact/contamination  524288  0x00080000  All but GPS  2  22  Lies within a dither offset of the stacked frame boundary  4194304  0x00400000  All but mosaics  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 K band sources in the LAS 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 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
Point source profilefitted J_1 mag 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
j_1PsfMagErr 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
Error in point source profilefitted J_1 mag 
real 
4 
mag 
0.9999995e9 
ERROR 
j_1SeqNum 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
the running number of the J_1 detection 
int 
4 

99999999 
ID_NUMBER 
j_1SerMag2D 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
Extended source J_1 mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
j_1SerMag2DErr 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
Error in extended source J_1 mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
ERROR 
j_1Xi 
lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource 
WSA 
Offset of J_1 detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
POS_EQ_RA_OFF 
j_1Xi 
lasSource 
WSA 
Offset of J_1 detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
POS_EQ_RA_OFF 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 2.0 (UKIDSS LAS and GPS; UHS; also nonsurvey programmes) or 1.0 (UKIDSS GPS, DXS and UDS) arcseconds is used, the higher value enabling pairing of moving sources when epoch separations may be several years. 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 LAS, you might wish to insist that the offsets in the selected sample are all below 1 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 
lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource 
WSA 
Default point source J_2 aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
j_2AperMag3 
lasSource 
WSA 
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_2AperMag3Err 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
Error in default point source J_2 mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
j_2AperMag4 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
Point source J_2 aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
j_2AperMag4Err 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
Error in point source J_2 mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
j_2AperMag6 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
Point source J_2 aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
j_2AperMag6Err 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
Error in point source J_2 mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
j_2Class 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
discrete image classification flag in J_2 
smallint 
2 

9999 
CLASS_MISC 
j_2ClassStat 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
N(0,1) stellarnessofprofile statistic in J_2 
real 
4 

0.9999995e9 
STAT_PROP 
j_2Deblend 
lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource 
WSA 
placeholder flag indicating parent/child relation in J_2 
int 
4 

99999999 
CODE_MISC 
j_2Deblend 
lasSource 
WSA 
placeholder flag indicating parent/child relation in J_2 
int 
4 

99999999 
CODE_MISC 
This CASU pipeline processing source extraction flag is a placeholder only, and is always set to zero in all passbands in the merged source lists. If you need to know when a particular image detection is a component of a deblend or not, test bit 4 of attribute ppErrBits (see corresponding glossary entry) which is set by WFAU's postprocessing software based on testing the areal profiles aprof28 (these are set by CASU to 1 for deblended components, or positive values for nondeblended detections). We encode this in an information bit of ppErrBits for convenience when querying the merged source tables. 
j_2Ell 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
1b/a, where a/b=semimajor/minor axes in J_2 
real 
4 

0.9999995e9 
PHYS_ELLIPTICITY 
j_2eNum 
lasMergeLog, lasYJHKmergeLog 
WSA 
the extension number of this J_2 frame 
tinyint 
1 


NUMBER 
j_2ErrBits 
lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource 
WSA 
processing warning/error bitwise flags in J_2 
int 
4 

99999999 
CODE_MISC 
j_2ErrBits 
lasSource 
WSA 
processing warning/error bitwise flags in J_2 
int 
4 

99999999 
CODE_MISC 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
j_2Eta 
lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource 
WSA 
Offset of J_2 detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
POS_EQ_DEC_OFF 
j_2Eta 
lasSource 
WSA 
Offset of J_2 detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
POS_EQ_DEC_OFF 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 2.0 (UKIDSS LAS and GPS; UHS; also nonsurvey programmes) or 1.0 (UKIDSS GPS, DXS and UDS) arcseconds is used, the higher value enabling pairing of moving sources when epoch separations may be several years. 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 LAS, you might wish to insist that the offsets in the selected sample are all below 1 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 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
RMS of axes of ellipse fit in J_2 
real 
4 
pixels 
0.9999995e9 
MORPH_PARAM 
j_2HallMag 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
Total point source J_2 mag 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
j_2HallMagErr 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
Error in total point source J_2 mag 
real 
4 
mag 
0.9999995e9 
ERROR 
j_2mfID 
lasMergeLog, lasYJHKmergeLog 
WSA 
the UID of the relevant J_2 multiframe 
bigint 
8 


ID_FRAME 
j_2mhExt 
lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource 
WSA 
Extended source colour J_2H (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
j_2mhExt 
lasSource 
WSA 
Extended source colour J_2H (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
j_2mhExtErr 
lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource 
WSA 
Error on extended source colour J_2H 
real 
4 
mag 
0.9999995e9 
ERROR 
j_2mhExtErr 
lasSource 
WSA 
Error on extended source colour J_2H 
real 
4 
mag 
0.9999995e9 
ERROR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
j_2mhPnt 
lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource 
WSA 
Point source colour J_2H (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
j_2mhPnt 
lasSource 
WSA 
Point source colour J_2H (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
j_2mhPntErr 
lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource 
WSA 
Error on point source colour J_2H 
real 
4 
mag 
0.9999995e9 
ERROR 
j_2mhPntErr 
lasSource 
WSA 
Error on point source colour J_2H 
real 
4 
mag 
0.9999995e9 
ERROR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
j_2mrat 
twomass_scn 
2MASS 
Jband average 2nd image moment ratio. 
real 
4 


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



j_2PA 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
ellipse fit celestial orientation in J_2 
real 
4 
Degrees 
0.9999995e9 
POS_POSANG 
j_2PetroMag 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
Extended source J_2 mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
j_2PetroMagErr 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
Error in extended source J_2 mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
ERROR 
j_2ppErrBits 
lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource 
WSA 
additional WFAU postprocessing error bits in J_2 
int 
4 

0 
CODE_MISC 
j_2ppErrBits 
lasSource 
WSA 
additional WFAU postprocessing error bits in J_2 
int 
4 

0 
CODE_MISC 
Postprocessing error quality bit flags assigned (NB: from UKIDSS DR2 release onwards) in the WSA curation procedure for survey data. From least to most significant byte in the 4byte 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  1  15  Source in poor flat field region  32768  0x00008000  All but mosaics  2  16  Close to saturated  65536  0x00010000  All VDFS catalogues (though deeps excluded prior to DR8)  2  17  Photometric calibration probably subject to systematic error  131072  0x00020000  GPS only  2  19  Possible crosstalk artefact/contamination  524288  0x00080000  All but GPS  2  22  Lies within a dither offset of the stacked frame boundary  4194304  0x00400000  All but mosaics  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 K band sources in the LAS 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 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
Point source profilefitted J_2 mag 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
j_2PsfMagErr 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
Error in point source profilefitted J_2 mag 
real 
4 
mag 
0.9999995e9 
ERROR 
j_2SeqNum 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
the running number of the J_2 detection 
int 
4 

99999999 
ID_NUMBER 
j_2SerMag2D 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
Extended source J_2 mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
j_2SerMag2DErr 
lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource 
WSA 
Error in extended source J_2 mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
ERROR 
j_2Xi 
lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource 
WSA 
Offset of J_2 detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
POS_EQ_RA_OFF 
j_2Xi 
lasSource 
WSA 
Offset of J_2 detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
POS_EQ_RA_OFF 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 2.0 (UKIDSS LAS and GPS; UHS; also nonsurvey programmes) or 1.0 (UKIDSS GPS, DXS and UDS) arcseconds is used, the higher value enabling pairing of moving sources when epoch separations may be several years. 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 LAS, you might wish to insist that the offsets in the selected sample are all below 1 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 
2MASS 
J minor/major axis ratio fit to the 5sigma isophote. 
real 
4 


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

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

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


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


CODE_MISC 
j_bisym_chi 
twomass_xsc 
2MASS 
J bisymmetric crosscorrelation chi. 
real 
4 


FIT_PARAM_VALUE 
j_bisym_rat 
twomass_xsc 
2MASS 
J bisymmetric flux ratio. 
real 
4 


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

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

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


FIT_PARAM_VALUE 
j_cmsig 
twomass_psc 
2MASS 
Corrected photometric uncertainty for the default Jband magnitude. 
real 
4 
mag 

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


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


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


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


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


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


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


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


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


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


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


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



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


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


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


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


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


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


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


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


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


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


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


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


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


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



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


CODE_MISC 
j_h 
twomass_sixx2_psc 
2MASS 
The JH color, computed from the Jband and Hband magnitudes (j_m and h_m, respectively) of the source. In cases where the first or second digit in rd_flg is equal to either "0", "4", "6", or "9", no color is computed because the photometry in one or both bands is of lower quality or the source is not detected. 
real 
4 



j_k 
twomass_sixx2_psc 
2MASS 
The JKs color, computed from the Jband and Ksband magnitudes (j_m and k_m, respectively) of the source. In cases where the first or third digit in rd_flg is equal to either "0", "4", "6", or "9", no color is computed because the photometry in one or both bands is of lower quality or the source is not detected. 
real 
4 



j_m 
twomass_psc 
2MASS 
Default Jband magnitude 
real 
4 
mag 

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


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

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

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

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

SPECT_FLUX_VALUE 
j_m_2mass 
allwise_sc 
WISE 
2MASS Jband 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 Jband magnitude entry is "null". 
float 
8 
mag 


j_m_2mass 
wise_allskysc 
WISE 
2MASS Jband magnitude or magnitude upper limit of the associated 2MASS PSC source. This column is default if there is no associated 2MASS PSC source or if the 2MASS PSC Jband magnitude entry is default. 
real 
4 
mag 
0.9999995e9 

j_m_2mass 
wise_prelimsc 
WISE 
2MASS Jband magnitude or magnitude upper limit of the associated 2MASS PSC source This column is default if there is no associated 2MASS PSC source or if the 2MASS PSC Jband magnitude entry is default 
real 
4 
mag 
0.9999995e9 

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

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

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

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

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

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


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

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

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

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

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


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

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

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

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

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

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

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

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

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

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

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


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

SPECT_FLUX_VALUE 
j_m_stdap 
twomass_psc 
2MASS 
Jband "standard" aperture magnitude. 
real 
4 
mag 

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

SPECT_FLUX_VALUE 
j_mnsurfb_eff 
twomass_xsc 
2MASS 
J mean surface brightness at the halflight radius. 
real 
4 
mag 

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


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

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

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

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

ERROR 
j_msig_2mass 
allwise_sc 
WISE 
2MASS Jband 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 Jband uncertainty entry is "null". 
float 
8 
mag 


j_msig_2mass 
wise_allskysc 
WISE 
2MASS Jband corrected photometric uncertainty of the associated 2MASS PSC source. This column is default if there is no associated 2MASS PSC source or if the 2MASS PSC Jband uncertainty entry is default. 
real 
4 
mag 
0.9999995e9 

j_msig_2mass 
wise_prelimsc 
WISE 
2MASS Jband corrected photometric uncertainty of the associated 2MASS PSC source This column is default if there is no associated 2MASS PSC source or if the 2MASS PSC Jband uncertainty entry is default 
real 
4 
mag 
0.9999995e9 

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

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

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

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

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

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


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

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

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

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

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


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

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

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

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

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

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

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

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

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

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

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

ERROR 
j_msig_stdap 
twomass_psc 
2MASS 
Uncertainty in the Jband standard aperture magnitude. 
real 
4 
mag 

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

ERROR 
j_msigcom 
twomass_psc 
2MASS 
Combined, or total photometric uncertainty for the default Jband magnitude. 
real 
4 
mag 

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


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

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


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


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



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


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

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


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

POS_POSANG 
j_psfchi 
twomass_psc 
2MASS 
Reduced chisquared goodnessoffit value for the Jband profilefit photometry made on the 1.3 s "Read_2" exposures. 
real 
4 


FIT_PARAM_VALUE 
j_psp 
twomass_scn 
2MASS 
Jband photometric sensitivity paramater (PSP). 
real 
4 


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



j_pts_noise 
twomass_scn 
2MASS 
Base10 logarithm of the mode of the noise distribution for all point source detections in the scan, where the noise is estimated from the measured Jband photometric errors and is expressed in units of mJy. 
real 
4 


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


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

EXTENSION_RAD 
j_r_e 
twomass_xsc 
2MASS 
J Kron elliptical aperture semimajor axis. 
real 
4 
arcsec 

EXTENSION_RAD 
j_r_eff 
twomass_xsc 
2MASS 
J halflight (integrated halfflux point) radius. 
real 
4 
arcsec 

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

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

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

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

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

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


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


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


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


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


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


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


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


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


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


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


FIT_PARAM 
j_shape_avg 
twomass_scn 
2MASS 
Jband average seeing shape for scan. 
real 
4 


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



j_shape_rms 
twomass_scn 
2MASS 
RMSerror of Jband average seeing shape. 
real 
4 


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



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


FIT_PARAM 
j_snr 
twomass_psc 
2MASS 
Jband "scan" signaltonoise ratio. 
real 
4 
mag 

INST_NOISE 
j_snr 
twomass_sixx2_psc 
2MASS 
J band "scan" signaltonoise ratio 
real 
4 



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


CODE_MISC 
j_zp_ap 
twomass_scn 
2MASS 
Photometric zeropoint for Jband aperture photometry. 
real 
4 
mag 

PHOT_ZP 
j_zp_ap 
twomass_sixx2_scn 
2MASS 
J band ap. calibration photometric zeropoint for scan 
real 
4 
mag 


jAperJky3 
lasYselJSourceRemeasurement 
WSA 
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 
lasYselJSourceRemeasurement 
WSA 
Error in default point/extended source J (2.0 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
stat.error 
jAperJky4 
lasYselJSourceRemeasurement 
WSA 
Point source J aperture corrected (2.8 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
jAperJky4Err 
lasYselJSourceRemeasurement 
WSA 
Error in point/extended source J (2.8 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
stat.error 
jAperJky6 
lasYselJSourceRemeasurement 
WSA 
Point source J aperture corrected (5.7 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
jAperJky6Err 
lasYselJSourceRemeasurement 
WSA 
Error in point/extended source J (5.7 arcsec aperture diameter) calibrated flux 
real 
4 
jansky 
0.9999995e9 
stat.error 
jAperJkyNoAperCorr3 
lasYselJSourceRemeasurement 
WSA 
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 
lasYselJSourceRemeasurement 
WSA 
Extended source J (2.8 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
jAperJkyNoAperCorr6 
lasYselJSourceRemeasurement 
WSA 
Extended source J (5.7 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux 
real 
4 
jansky 
0.9999995e9 
phot.flux 
jAperLup3 
lasYselJSourceRemeasurement 
WSA 
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 
lasYselJSourceRemeasurement 
WSA 
Error in default point/extended source J (2.0 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
stat.error 
jAperLup4 
lasYselJSourceRemeasurement 
WSA 
Point source J aperture corrected (2.8 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
jAperLup4Err 
lasYselJSourceRemeasurement 
WSA 
Error in point/extended source J (2.8 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
stat.error 
jAperLup6 
lasYselJSourceRemeasurement 
WSA 
Point source J aperture corrected (5.7 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
jAperLup6Err 
lasYselJSourceRemeasurement 
WSA 
Error in point/extended source J (5.7 arcsec aperture diameter) luptitude 
real 
4 
lup 
0.9999995e9 
stat.error 
jAperLupNoAperCorr3 
lasYselJSourceRemeasurement 
WSA 
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 
lasYselJSourceRemeasurement 
WSA 
Extended source J (2.8 arcsec aperture diameter, but no aperture correction applied) aperture luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
jAperLupNoAperCorr6 
lasYselJSourceRemeasurement 
WSA 
Extended source J (5.7 arcsec aperture diameter, but no aperture correction applied) aperture luptitude 
real 
4 
lup 
0.9999995e9 
phot.lup 
jAperMag1 
calSynopticSource 
WSACalib 
Extended source J aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
jAperMag1 
gpsJHKsource, gpsPointSource, reliableGpsPointSource 
WSA 
Default point source J aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
jAperMag1 
gpsSource 
WSA 
Default point source J aperture corrected mag (1.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
jAperMag1Err 
calSynopticSource 
WSACalib 
Error in extended source J mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
jAperMag1Err 
gpsJHKsource, gpsPointSource, gpsSource, reliableGpsPointSource 
WSA 
Error in point source J mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
jAperMag2 
calSynopticSource 
WSACalib 
Extended source J aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
jAperMag2Err 
calSynopticSource 
WSACalib 
Error in extended source J mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
jAperMag3 
calSource 
WSACalib 
Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
jAperMag3 
calSynopticSource 
WSACalib 
Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
jAperMag3 
dxsJKsource, gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, lasExtendedSource, lasPointSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource 
WSA 
Default point source J aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
jAperMag3 
dxsSource, gcsSource, gpsSource, lasSource 
WSA 
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 
lasYselJSourceRemeasurement 
WSA 
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 
reliableUdsSource 
WSA 
Default point/extended source J mag, no aperture correction applied 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
jAperMag3 
udsSource 
WSA 
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 
uhsSource, uhsSourceAll 
WSAUHS 
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 
jAperMag3Err 
calSource, calSynopticSource 
WSACalib 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
jAperMag3Err 
dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource 
WSA 
Error in default point source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
jAperMag3Err 
lasYselJSourceRemeasurement 
WSA 
Error in default point/extended source J (2.0 arcsec aperture diameter) magnitude 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag3Err 
reliableUdsSource, udsSource 
WSA 
Error in default point/extended source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
jAperMag3Err 
uhsSource, uhsSourceAll 
WSAUHS 
Error in default point source J mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
jAperMag4 
calSource, calSynopticSource 
WSACalib 
Extended source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
jAperMag4 
dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource 
WSA 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
jAperMag4 
lasYselJSourceRemeasurement 
WSA 
Point source J aperture corrected (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag4 
reliableUdsSource, udsSource 
WSA 
Extended source J mag, no aperture correction applied 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
jAperMag4 
uhsSource, uhsSourceAll 
WSAUHS 
Point source J aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
jAperMag4Err 
calSource, calSynopticSource 
WSACalib 
Error in extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
jAperMag4Err 
dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource 
WSA 
Error in point source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
jAperMag4Err 
lasYselJSourceRemeasurement 
WSA 
Error in point/extended source J (2.8 arcsec aperture diameter) magnitude 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag4Err 
reliableUdsSource, udsSource 
WSA 
Error in extended source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
jAperMag4Err 
uhsSource, uhsSourceAll 
WSAUHS 
Error in point source J mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
jAperMag5 
calSynopticSource 
WSACalib 
Extended source J aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
jAperMag5Err 
calSynopticSource 
WSACalib 
Error in extended source J mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
jAperMag6 
calSource 
WSACalib 
Extended source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
jAperMag6 
dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableLasPointSource 
WSA 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
jAperMag6 
lasYselJSourceRemeasurement 
WSA 
Point source J aperture corrected (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMag6 
reliableUdsSource, udsSource 
WSA 
Extended source J mag, no aperture correction applied 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
jAperMag6 
uhsSource, uhsSourceAll 
WSAUHS 
Point source J aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
jAperMag6Err 
calSource 
WSACalib 
Error in extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
jAperMag6Err 
dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableLasPointSource 
WSA 
Error in point source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
jAperMag6Err 
lasYselJSourceRemeasurement 
WSA 
Error in point/extended source J (5.7 arcsec aperture diameter) magnitude 
real 
4 
mag 
0.9999995e9 
stat.error 
jAperMag6Err 
reliableUdsSource, udsSource 
WSA 
Error in extended source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
jAperMag6Err 
uhsSource, uhsSourceAll 
WSAUHS 
Error in point source J mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
jAperMagNoAperCorr3 
lasYselJSourceRemeasurement 
WSA 
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 
jAperMagNoAperCorr4 
lasYselJSourceRemeasurement 
WSA 
Extended source J (2.8 arcsec aperture diameter, but no aperture correction applied) aperture magnitude 
real 
4 
mag 
0.9999995e9 
phot.mag 
jAperMagNoAperCorr6 
lasYselJSourceRemeasurement 
WSA 
Extended source J (5.7 arcsec aperture diameter, but no aperture correction applied) aperture magnitude 
real 
4 
mag 
0.9999995e9 
phot.mag 
jaStratAst 
calVarFrameSetInfo 
WSACalib 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
jaStratAst 
dxsVarFrameSetInfo, lasVarFrameSetInfo, udsVarFrameSetInfo 
WSA 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
jaStratAst 
uhsVarFrameSetInfo 
WSAUHS 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
jaStratPht 
calVarFrameSetInfo 
WSACalib 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
jaStratPht 
dxsVarFrameSetInfo, lasVarFrameSetInfo, udsVarFrameSetInfo 
WSA 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
jaStratPht 
uhsVarFrameSetInfo 
WSAUHS 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
jAverageConf 
lasYselJSourceRemeasurement 
WSA 
average confidence in 2 arcsec diameter default aperture (aper3) J 
real 
4 

0.9999995e9 
stat.likelihood;em.IR.NIR 
jbestAper 
calVariability 
WSACalib 
Best aperture (16) for photometric statistics in the J band 
int 
4 

9999 

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

9999 

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

9999 

Aperture magnitude (16) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) 
jbStratAst 
calVarFrameSetInfo 
WSACalib 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
jbStratAst 
dxsVarFrameSetInfo, lasVarFrameSetInfo, udsVarFrameSetInfo 
WSA 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
jbStratAst 
uhsVarFrameSetInfo 
WSAUHS 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
jbStratPht 
calVarFrameSetInfo 
WSACalib 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
jbStratPht 
dxsVarFrameSetInfo, lasVarFrameSetInfo, udsVarFrameSetInfo 
WSA 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
jbStratPht 
uhsVarFrameSetInfo 
WSAUHS 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
jchiSqAst 
calVarFrameSetInfo 
WSACalib 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
jchiSqAst 
dxsVarFrameSetInfo, lasVarFrameSetInfo, udsVarFrameSetInfo 
WSA 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
jchiSqAst 
uhsVarFrameSetInfo 
WSAUHS 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
jchiSqpd 
calVariability 
WSACalib 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 

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

0.9999995e9 

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

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
jchiSqPht 
calVarFrameSetInfo 
WSACalib 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
jchiSqPht 
dxsVarFrameSetInfo, lasVarFrameSetInfo, udsVarFrameSetInfo 
WSA 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
jchiSqPht 
uhsVarFrameSetInfo 
WSAUHS 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
jClass 
calSource, calSynopticSource 
WSACalib 
discrete image classification flag in J 
smallint 
2 

9999 
CLASS_MISC 
jClass 
dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource, udsSource 
WSA 
discrete image classification flag in J 
smallint 
2 

9999 
CLASS_MISC 
jClass 
lasYselJSourceRemeasurement 
WSA 
discrete image classification flag in J 
smallint 
2 

9999 
src.class 
jClass 
uhsSource, uhsSourceAll 
WSAUHS 
discrete image classification flag in J 
smallint 
2 

9999 
CLASS_MISC 
jClassStat 
calSource, calSynopticSource 
WSACalib 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
STAT_PROP 
jClassStat 
dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource 
WSA 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
STAT_PROP 
jClassStat 
lasYselJSourceRemeasurement 
WSA 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
stat 
jClassStat 
reliableUdsSource, udsSource 
WSA 
SExtractor classification statistic in J 
real 
4 

0.9999995e9 
STAT_PROP 
jClassStat 
uhsSource, uhsSourceAll 
WSAUHS 
N(0,1) stellarnessofprofile statistic in J 
real 
4 

0.9999995e9 
STAT_PROP 
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 1sigma uncertainty in 20mag/sq." aperture {image primary HDU keyword: j_msig_k20fe} 
real 
4 
mag 
0.9999995e9 

jcStratAst 
calVarFrameSetInfo 
WSACalib 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
jcStratAst 
dxsVarFrameSetInfo, lasVarFrameSetInfo, udsVarFrameSetInfo 
WSA 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
jcStratAst 
uhsVarFrameSetInfo 
WSAUHS 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
jcStratPht 
calVarFrameSetInfo 
WSACalib 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
jcStratPht 
dxsVarFrameSetInfo, lasVarFrameSetInfo, udsVarFrameSetInfo 
WSA 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
jcStratPht 
uhsVarFrameSetInfo 
WSAUHS 
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 medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
jdate 
twomass_psc 
2MASS 
The Julian Date of the source measurement accurate to +30 seconds. 
float 
8 
Julian days 

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

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


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


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

TIME_DATE 
jDeblend 
calSource 
WSACalib 
placeholder flag indicating parent/child relation in J 
int 
4 

99999999 
CODE_MISC 
This CASU pipeline processing source extraction flag is a placeholder only, and is always set to zero in all passbands in the merged source lists. If you need to know when a particular image detection is a component of a deblend or not, test bit 4 of attribute ppErrBits (see corresponding glossary entry) which is set by WFAU's postprocessing software based on testing the areal profiles aprof28 (these are set by CASU to 1 for deblended components, or positive values for nondeblended detections). We encode this in an information bit of ppErrBits for convenience when querying the merged source tables. 
jDeblend 
calSynopticSource 
WSACalib 
placeholder flag indicating parent/child relation in J 
int 
4 

99999999 
CODE_MISC 
jDeblend 
dxsJKsource, gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, lasExtendedSource, lasPointSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource, udsSource 
WSA 
placeholder flag indicating parent/child relation in J 
int 
4 

99999999 
CODE_MISC 
jDeblend 
dxsSource, gcsSource, gpsSource, lasSource 
WSA 
placeholder flag indicating parent/child relation in J 
int 
4 

99999999 
CODE_MISC 
This CASU pipeline processing source extraction flag is a placeholder only, and is always set to zero in all passbands in the merged source lists. If you need to know when a particular image detection is a component of a deblend or not, test bit 4 of attribute ppErrBits (see corresponding glossary entry) which is set by WFAU's postprocessing software based on testing the areal profiles aprof28 (these are set by CASU to 1 for deblended components, or positive values for nondeblended detections). We encode this in an information bit of ppErrBits for convenience when querying the merged source tables. 
jDeblend 
uhsSource, uhsSourceAll 
WSAUHS 
placeholder flag indicating parent/child relation in J 
int 
4 

99999999 
CODE_MISC 
This CASU pipeline processing source extraction flag is a placeholder only, and is always set to zero in all passbands in the merged source lists. If you need to know when a particular image detection is a component of a deblend or not, test bit 4 of attribute ppErrBits (see corresponding glossary entry) which is set by WFAU's postprocessing software based on testing the areal profiles aprof28 (these are set by CASU to 1 for deblended components, or positive values for nondeblended detections). We encode this in an information bit of ppErrBits for convenience when querying the merged source tables. 
jEll 
calSource, calSynopticSource 
WSACalib 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
PHYS_ELLIPTICITY 
jEll 
dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource, udsSource 
WSA 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
PHYS_ELLIPTICITY 
jEll 
lasYselJSourceRemeasurement 
WSA 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
src.ellipticty 
jEll 
uhsSource, uhsSourceAll 
WSAUHS 
1b/a, where a/b=semimajor/minor axes in J 
real 
4 

0.9999995e9 
PHYS_ELLIPTICITY 
jeNum 
calMergeLog, calSynopticMergeLog 
WSACalib 
the extension number of this J frame 
tinyint 
1 


NUMBER 
jeNum 
dxsJKmergeLog, gpsJHKmergeLog 
WSA 
the extension number of this frame 
tinyint 
1 


NUMBER 
jeNum 
dxsMergeLog, gcsMergeLog, gcsZYJHKmergeLog, gpsMergeLog, lasMergeLog, lasYJHKmergeLog, udsMergeLog 
WSA 
the extension number of this J frame 
tinyint 
1 


NUMBER 
jeNum 
lasYselJRemeasMergeLog 
WSA 
the extension number of this J frame 
tinyint 
1 


meta.number;em.IR.J 
jeNum 
uhsMergeLog 
WSAUHS 
the extension number of this J frame 
tinyint 
1 


NUMBER 
jErrBits 
calSource, calSynopticSource 
WSACalib 
processing warning/error bitwise flags in J 
int 
4 

99999999 
CODE_MISC 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
jErrBits 
dxsJKsource, gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, lasExtendedSource, lasPointSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource 
WSA 
processing warning/error bitwise flags in J 
int 
4 

99999999 
CODE_MISC 
jErrBits 
dxsSource, gcsSource, gpsSource, lasSource 
WSA 
processing warning/error bitwise flags in J 
int 
4 

99999999 
CODE_MISC 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
jErrBits 
lasYselJSourceRemeasurement 
WSA 
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 
udsSource 
WSA 
processing warning/error bitwise flags in J 
int 
4 

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

jErrBits 
uhsSource, uhsSourceAll 
WSAUHS 
processing warning/error bitwise flags in J 
int 
4 

99999999 
CODE_MISC 
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. 
jEta 
calSource, calSynopticSource 
WSACalib 
Offset of J detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
POS_EQ_DEC_OFF 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 2.0 (UKIDSS LAS and GPS; UHS; also nonsurvey programmes) or 1.0 (UKIDSS GPS, DXS and UDS) arcseconds is used, the higher value enabling pairing of moving sources when epoch separations may be several years. 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 LAS, you might wish to insist that the offsets in the selected sample are all below 1 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. 
jEta 
dxsJKsource, gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, lasExtendedSource, lasPointSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource 
WSA 
Offset of J detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
POS_EQ_DEC_OFF 
jEta 
dxsSource, gcsSource, gpsSource, lasSource, udsSource 
WSA 
Offset of J detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
POS_EQ_DEC_OFF 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 2.0 (UKIDSS LAS and GPS; UHS; also nonsurvey programmes) or 1.0 (UKIDSS GPS, DXS and UDS) arcseconds is used, the higher value enabling pairing of moving sources when epoch separations may be several years. 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 LAS, you might wish to insist that the offsets in the selected sample are all below 1 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. 
jEta 
uhsSource, uhsSourceAll 
WSAUHS 
Offset of J detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
POS_EQ_DEC_OFF 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 2.0 (UKIDSS LAS and GPS; UHS; also nonsurvey programmes) or 1.0 (UKIDSS GPS, DXS and UDS) arcseconds is used, the higher value enabling pairing of moving sources when epoch separations may be several years. 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 LAS, you might wish to insist that the offsets in the selected sample are all below 1 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. 
jexpML 
calVarFrameSetInfo 
WSACalib 
Expected magnitude limit of frameSet in this in J band. 
real 
4 

0.9999995e9 

The expected magnitude limit of an intermediate stack, based on the total exposure time. expML=Filter.oneSecML+1.25*log10(totalExpTime). Since different intermediate stacks can have different exposure times, the totalExpTime is the minimum, as long as the number of stacks with this minimum make up 10% of the total. This is a more conservative treatment than just taking the mean or median total exposure time. 
jexpML 
dxsVarFrameSetInfo, lasVarFrameSetInfo, udsVarFrameSetInfo 
WSA 
Expected magnitude limit of frameSet in this in J band. 
real 
4 

0.9999995e9 

The expected magnitude limit of an intermediate stack, based on the total exposure time. expML=Filter.oneSecML+1.25*log10(totalExpTime). Since different intermediate stacks can have different exposure times, the totalExpTime is the minimum, as long as the number of stacks with this minimum make up 10% of the total. This is a more conservative treatment than just taking the mean or median total exposure time. 
jexpML 
uhsVarFrameSetInfo 
WSAUHS 
Expected magnitude limit of frameSet in this in J band. 
real 
4 

0.9999995e9 

The expected magnitude limit of an intermediate stack, based on the total exposure time. expML=Filter.oneSecML+1.25*log10(totalExpTime). Since different intermediate stacks can have different exposure times, the totalExpTime is the minimum, as long as the number of stacks with this minimum make up 10% of the total. This is a more conservative treatment than just taking the mean or median total exposure time. 
jExpRms 
calVariability 
WSACalib 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in J band 
real 
4 
mag 
0.9999995e9 

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

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

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
jGausig 
calSource, calSynopticSource 
WSACalib 
RMS of axes of ellipse fit in J 
real 
4 
pixels 
0.9999995e9 
MORPH_PARAM 
jGausig 
dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource, udsSource 
WSA 
RMS of axes of ellipse fit in J 
real 
4 
pixels 
0.9999995e9 
MORPH_PARAM 
jGausig 
lasYselJSourceRemeasurement 
WSA 
RMS of axes of ellipse fit in J 
real 
4 
pixels 
0.9999995e9 
src.morph.param 
jGausig 
uhsSource, uhsSourceAll 
WSAUHS 
RMS of axes of ellipse fit in J 
real 
4 
pixels 
0.9999995e9 
MORPH_PARAM 
jHallMag 
calSource 
WSACalib 
Total point source J mag 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
jHallMag 
dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource 
WSA 
Total point source J mag 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
jHallMag 
reliableUdsSource, udsSource 
WSA 
Not available in SE output 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
jHallMag 
uhsSource, uhsSourceAll 
WSAUHS 
Total point source J mag 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
jHallMagErr 
calSource 
WSACalib 
Error in total point source J mag 
real 
4 
mag 
0.9999995e9 
ERROR 
jHallMagErr 
dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource 
WSA 
Error in total point source J mag 
real 
4 
mag 
0.9999995e9 
ERROR 
jHallMagErr 
reliableUdsSource, udsSource 
WSA 
Not available in SE output 
real 
4 
mag 
0.9999995e9 
ERROR 
jHallMagErr 
uhsSource, uhsSourceAll 
WSAUHS 
Error in total point source J mag 
real 
4 
mag 
0.9999995e9 
ERROR 
jhiWS 
calVariability 
WSACalib 
WelchStetson statistic between J and H. This assumes colour does not vary much and helps remove variation due to a few poor detections 
real 
4 

0.9999995e9 

The WelchStetson statistic is a measure of the correlation of the variability between two bands. We use the calculation in Welch D.L. and Stetson P.B. 1993, AJ, 105, 5, which is also used in Sesar et al. 2007, AJ, 134, 2236. We use the aperMag3 magnitude when comparing between bands. 
jIntRms 
calVariability 
WSACalib 
Intrinsic rms in Jband 
real 
4 
mag 
0.9999995e9 

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

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

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

0 

jisDefAst 
dxsVarFrameSetInfo, lasVarFrameSetInfo, udsVarFrameSetInfo 
WSA 
Use a default model for the astrometric noise in J band. 
tinyint 
1 

0 

jisDefAst 
uhsVarFrameSetInfo 
WSAUHS 
Use a default model for the astrometric noise in J band. 
tinyint 
1 

0 

jisDefPht 
calVarFrameSetInfo 
WSACalib 
Use a default model for the photometric noise in J band. 
tinyint 
1 

0 

jisDefPht 
dxsVarFrameSetInfo, lasVarFrameSetInfo, udsVarFrameSetInfo 
WSA 
Use a default model for the photometric noise in J band. 
tinyint 
1 

0 

jisDefPht 
uhsVarFrameSetInfo 
WSAUHS 
Use a default model for the photometric noise in J band. 
tinyint 
1 

0 

jIsMeas 
lasYselJSourceRemeasurement 
WSA 
Is pass band J measured? 0 no, 1 yes 
tinyint 
1 

0 
meta.code 
jitterID 
Multiframe 
WSA 
Serial number in this telescope jitter pattern {image primary HDU keyword: JITTER_I} 
smallint 
2 

9999 
meta.id 
jitterID 
Multiframe 
WSACalib 
Serial number in this telescope jitter pattern {image primary HDU keyword: JITTER_I} 
smallint 
2 

9999 
meta.id 
jitterID 
Multiframe 
WSATransit 
Serial number in this telescope jitter pattern {image primary HDU keyword: JITTER_I} 
smallint 
2 

9999 
meta.id 
jitterID 
Multiframe 
WSAUHS 
Serial number in this telescope jitter pattern {image primary HDU keyword: JITTER_I} 
smallint 
2 

9999 
meta.id 
jitterX 
Multiframe 
WSA 
X (RA) offset in tel jitter pattern {image primary HDU keyword: JITTER_X} 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff 
jitterX 
Multiframe 
WSACalib 
X (RA) offset in tel jitter pattern {image primary HDU keyword: JITTER_X} 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff 
jitterX 
Multiframe 
WSATransit 
X (RA) offset in tel jitter pattern {image primary HDU keyword: JITTER_X} 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff 
jitterX 
Multiframe 
WSAUHS 
X (RA) offset in tel jitter pattern {image primary HDU keyword: JITTER_X} 
real 
4 
arcsec 
0.9999995e9 
pos.eq.ra;arith.diff 
jitterY 
Multiframe 
WSA 
Y (Dec) offset in tel jitter pattern {image primary HDU keyword: JITTER_Y} 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
jitterY 
Multiframe 
WSACalib 
Y (Dec) offset in tel jitter pattern {image primary HDU keyword: JITTER_Y} 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
jitterY 
Multiframe 
WSATransit 
Y (Dec) offset in tel jitter pattern {image primary HDU keyword: JITTER_Y} 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
jitterY 
Multiframe 
WSAUHS 
Y (Dec) offset in tel jitter pattern {image primary HDU keyword: JITTER_Y} 
real 
4 
arcsec 
0.9999995e9 
pos.eq.dec;arith.diff 
jMag 
ukirtFSstars 
WSA 
J band total magnitude on the MKO(UFTI) system 
real 
4 
mag 

phot.mag 
jMag 
ukirtFSstars 
WSACalib 
J band total magnitude on the MKO(UFTI) system 
real 
4 
mag 

phot.mag 
jMag 
ukirtFSstars 
WSAUHS 
J band total magnitude on the MKO(UFTI) system 
real 
4 
mag 

phot.mag 
jMagErr 
ukirtFSstars 
WSA 
J band magnitude error 
real 
4 
mag 

stat.error 
jMagErr 
ukirtFSstars 
WSACalib 
J band magnitude error 
real 
4 
mag 

stat.error 
jMagErr 
ukirtFSstars 
WSAUHS 
J band magnitude error 
real 
4 
mag 

stat.error 
jMagMAD 
calVariability 
WSACalib 
Median Absolute Deviation of J magnitude 
real 
4 
mag 
0.9999995e9 

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

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

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

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

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

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

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
jmaxCadence 
dxsVariability, lasVariability, udsVariability 
WSA 
maximum gap between observations 
real 
4 
days 
0.9999995e9 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
jmaxCadence 
uhsVariability 
WSAUHS 
maximum gap between observations 
real 
4 
days 
0.9999995e9 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
jMaxMag 
calVariability 
WSACalib 
Maximum magnitude in J band, of good detections 
real 
4 

0.9999995e9 

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

0.9999995e9 

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

0.9999995e9 

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

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

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

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

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
jmedCadence 
dxsVariability, lasVariability, udsVariability 
WSA 
median gap between observations 
real 
4 
days 
0.9999995e9 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
jmedCadence 
uhsVariability 
WSAUHS 
median gap between observations 
real 
4 
days 
0.9999995e9 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
jmedianMag 
calVariability 
WSACalib 
Median J magnitude 
real 
4 
mag 
0.9999995e9 

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

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

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
jmfID 
calMergeLog, calSynopticMergeLog 
WSACalib 
the UID of the relevant J multiframe 
bigint 
8 


ID_FRAME 
jmfID 
dxsJKmergeLog, gpsJHKmergeLog 
WSA 
the UID of the relevant multiframe 
bigint 
8 


ID_FRAME 
jmfID 
dxsMergeLog, gcsMergeLog, gcsZYJHKmergeLog, gpsMergeLog, lasMergeLog, lasYJHKmergeLog, udsMergeLog 
WSA 
the UID of the relevant J multiframe 
bigint 
8 


ID_FRAME 
jmfID 
lasYselJRemeasMergeLog 
WSA 
the UID of the relevant J multiframe 
bigint 
8 


meta.id;obs.field;em.IR.J 
jmfID 
uhsMergeLog 
WSAUHS 
the UID of the relevant J multiframe 
bigint 
8 


ID_FRAME 
jmhExt 
calSource 
WSACalib 
Extended source colour JH (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
jmhExt 
dxsJKsource, gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, lasExtendedSource, lasPointSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource 
WSA 
Extended source colour JH (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
jmhExt 
dxsSource, gcsSource, gpsSource, lasSource, udsSource 
WSA 
Extended source colour JH (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
jmhExt 
lasYselJSourceRemeasurement 
WSA 
Extended source colour JH (using aperMagNoAperCorr3) 
real 
4 
mag 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
jmhExtErr 
calSource 
WSACalib 
Error on extended source colour JH 
real 
4 
mag 
0.9999995e9 
ERROR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
jmhExtErr 
dxsJKsource, gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, lasExtendedSource, lasPointSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource 
WSA 
Error on extended source colour JH 
real 
4 
mag 
0.9999995e9 
ERROR 
jmhExtErr 
dxsSource, gcsSource, gpsSource, lasSource, udsSource 
WSA 
Error on extended source colour JH 
real 
4 
mag 
0.9999995e9 
ERROR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
jmhExtErr 
lasYselJSourceRemeasurement 
WSA 
Error on extended source colour JH 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
jmhExtJky 
lasYselJSourceRemeasurement 
WSA 
Extended source colour calibrated flux H/J (using aperJkyNoAperCorr3) 
real 
4 
jansky 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
jmhExtJkyErr 
lasYselJSourceRemeasurement 
WSA 
Error on extended source colour calibrated flux H/J 
real 
4 
jansky 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
jmhExtLup 
lasYselJSourceRemeasurement 
WSA 
Extended source colour luptitudeJH (using aperLupNoAperCorr3) 
real 
4 
lup 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
jmhExtLupErr 
lasYselJSourceRemeasurement 
WSA 
Error on extended source colour luptitude JH 
real 
4 
lup 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
jmhPnt 
calSource, calSynopticSource 
WSACalib 
Point source colour JH (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
jmhPnt 
dxsJKsource, gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, lasExtendedSource, lasPointSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource 
WSA 
Point source colour JH (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
jmhPnt 
dxsSource, gcsSource, gpsSource, lasSource, udsSource 
WSA 
Point source colour JH (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
jmhPnt 
lasYselJSourceRemeasurement 
WSA 
Point source colour JH (using aperMag3) 
real 
4 
mag 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
jmhPntErr 
calSource, calSynopticSource 
WSACalib 
Error on point source colour JH 
real 
4 
mag 
0.9999995e9 
ERROR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
jmhPntErr 
dxsJKsource, gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, lasExtendedSource, lasPointSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource 
WSA 
Error on point source colour JH 
real 
4 
mag 
0.9999995e9 
ERROR 
jmhPntErr 
dxsSource, gcsSource, gpsSource, lasSource, udsSource 
WSA 
Error on point source colour JH 
real 
4 
mag 
0.9999995e9 
ERROR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
jmhPntErr 
lasYselJSourceRemeasurement 
WSA 
Error on point source colour JH 
real 
4 
mag 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
jmhPntJky 
lasYselJSourceRemeasurement 
WSA 
Point source colour calibrated flux H/J (using aperJky3) 
real 
4 
jansky 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
jmhPntJkyErr 
lasYselJSourceRemeasurement 
WSA 
Error on point source colour calibrated flux H/J 
real 
4 
jansky 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
jmhPntLup 
lasYselJSourceRemeasurement 
WSA 
Point source colour luptitude JH (using aperLup3) 
real 
4 
lup 
0.9999995e9 
phot.color 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
jmhPntLupErr 
lasYselJSourceRemeasurement 
WSA 
Error on point source colour luptitude JH 
real 
4 
lup 
0.9999995e9 
stat.error 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
jminCadence 
calVariability 
WSACalib 
minimum gap between observations 
real 
4 
days 
0.9999995e9 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
jminCadence 
dxsVariability, lasVariability, udsVariability 
WSA 
minimum gap between observations 
real 
4 
days 
0.9999995e9 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
jminCadence 
uhsVariability 
WSAUHS 
minimum gap between observations 
real 
4 
days 
0.9999995e9 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
jMinMag 
calVariability 
WSACalib 
Minimum magnitude in J band, of good detections 
real 
4 

0.9999995e9 

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

0.9999995e9 

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

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
jmkExt 
dxsJKsource, reliableDxsSource 
WSA 
Extended source colour JK (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
jmkExt 
dxsSource 
WSA 
Extended source colour JK (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
jmkExt 
uhsSource 
WSAUHS 
Extended source colour JK (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
jmkExtErr 
dxsJKsource, reliableDxsSource 
WSA 
Error on extended source colour JK 
real 
4 
mag 
0.9999995e9 
ERROR 
jmkExtErr 
dxsSource 
WSA 
Error on extended source colour JK 
real 
4 
mag 
0.9999995e9 
ERROR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
jmkExtErr 
uhsSource 
WSAUHS 
Error on extended source colour JK 
real 
4 
mag 
0.9999995e9 
ERROR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
jmkPnt 
dxsJKsource, reliableDxsSource 
WSA 
Point source colour JK (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
jmkPnt 
dxsSource 
WSA 
Point source colour JK (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
jmkPnt 
uhsSource 
WSAUHS 
Point source colour JK (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
jmkPntErr 
dxsJKsource, reliableDxsSource 
WSA 
Error on point source colour JK 
real 
4 
mag 
0.9999995e9 
ERROR 
jmkPntErr 
dxsSource 
WSA 
Error on point source colour JK 
real 
4 
mag 
0.9999995e9 
ERROR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
jmkPntErr 
uhsSource 
WSAUHS 
Error on point source colour JK 
real 
4 
mag 
0.9999995e9 
ERROR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
jndof 
calVariability 
WSACalib 
Number of degrees of freedom for chisquare 
smallint 
2 

9999 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
jndof 
dxsVariability, lasVariability, udsVariability 
WSA 
Number of degrees of freedom for chisquare 
smallint 
2 

9999 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
jndof 
uhsVariability 
WSAUHS 
Number of degrees of freedom for chisquare 
smallint 
2 

9999 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
jnDofAst 
calVarFrameSetInfo 
WSACalib 
Number of degrees of freedom of astrometric fit in J band. 
smallint 
2 

9999 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
jnDofAst 
dxsVarFrameSetInfo, lasVarFrameSetInfo, udsVarFrameSetInfo 
WSA 
Number of degrees of freedom of astrometric fit in J band. 
smallint 
2 

9999 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
jnDofAst 
uhsVarFrameSetInfo 
WSAUHS 
Number of degrees of freedom of astrometric fit in J band. 
smallint 
2 

9999 

The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
jnDofPht 
calVarFrameSetInfo 
WSACalib 
Number of degrees of freedom of photometric fit in J band. 
smallint 
2 

9999 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
jnDofPht 
dxsVarFrameSetInfo, lasVarFrameSetInfo, udsVarFrameSetInfo 
WSA 
Number of degrees of freedom of photometric fit in J band. 
smallint 
2 

9999 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
jnDofPht 
uhsVarFrameSetInfo 
WSAUHS 
Number of degrees of freedom of photometric fit in J band. 
smallint 
2 

9999 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
jnFlaggedObs 
calVariability 
WSACalib 
Number of detections in J band flagged as potentially spurious by calDetection.ppErrBits 
int 
4 

0 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
jnFlaggedObs 
dxsVariability 
WSA 
Number of detections in J band flagged as potentially spurious by dxsDetection.ppErrBits 
int 
4 

0 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
jnFlaggedObs 
lasVariability 
WSA 
Number of detections in J band flagged as potentially spurious by lasDetection.ppErrBits 
int 
4 

0 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
jnFlaggedObs 
udsVariability 
WSA 
Number of detections in J band flagged as potentially spurious by udsDetection.ppErrBits 
int 
4 

0 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
jnFlaggedObs 
uhsVariability 
WSAUHS 
Number of detections in J band flagged as potentially spurious by uhsDetection.ppErrBits 
int 
4 

0 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
jnGoodObs 
calVariability 
WSACalib 
Number of good detections in J band 
int 
4 

0 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
jnGoodObs 
dxsVariability, lasVariability, udsVariability 
WSA 
Number of good detections in J band 
int 
4 

0 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
jnGoodObs 
uhsVariability 
WSAUHS 
Number of good detections in J band 
int 
4 

0 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
jNgt3sig 
calVariability 
WSACalib 
Number of good detections in Jband that are more than 3 sigma deviations 
smallint 
2 

9999 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
jNgt3sig 
dxsVariability, lasVariability, udsVariability 
WSA 
Number of good detections in Jband that are more than 3 sigma deviations (jAperMagN < (jMeanMag3*jMagRms) 
smallint 
2 

9999 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
jNgt3sig 
uhsVariability 
WSAUHS 
Number of good detections in Jband that are more than 3 sigma deviations (jAperMagN < (jMeanMag3*jMagRms) 
smallint 
2 

9999 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
jnMissingObs 
calVariability 
WSACalib 
Number of J band frames that this object should have been detected on and was not 
int 
4 

0 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
jnMissingObs 
dxsVariability, lasVariability, udsVariability 
WSA 
Number of J band frames that this object should have been detected on and was not 
int 
4 

0 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
jnMissingObs 
uhsVariability 
WSAUHS 
Number of J band frames that this object should have been detected on and was not 
int 
4 

0 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
joinCriterion 
RequiredNeighbours 
WSA 
the join criterion (search radius for matches) 
real 
4 
degrees 

?? 
joinCriterion 
RequiredNeighbours 
WSACalib 
the join criterion (search radius for matches) 
real 
4 
degrees 

?? 
joinCriterion 
RequiredNeighbours 
WSATransit 
the join criterion (search radius for matches) 
real 
4 
degrees 

?? 
joinCriterion 
RequiredNeighbours 
WSAUHS 
the join criterion (search radius for matches) 
real 
4 
degrees 

?? 
jPA 
calSource, calSynopticSource 
WSACalib 
ellipse fit celestial orientation in J 
real 
4 
Degrees 
0.9999995e9 
POS_POSANG 
jPA 
dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource, udsSource 
WSA 
ellipse fit celestial orientation in J 
real 
4 
Degrees 
0.9999995e9 
POS_POSANG 
jPA 
lasYselJSourceRemeasurement 
WSA 
ellipse fit celestial orientation in J 
real 
4 
Degrees 
0.9999995e9 
pos.posAng 
jPA 
uhsSource, uhsSourceAll 
WSAUHS 
ellipse fit celestial orientation in J 
real 
4 
Degrees 
0.9999995e9 
POS_POSANG 
jPetroMag 
calSource 
WSACalib 
Extended source J mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
jPetroMag 
dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource, udsSource 
WSA 
Extended source J mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
jPetroMag 
uhsSource, uhsSourceAll 
WSAUHS 
Extended source J mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
jPetroMagErr 
calSource 
WSACalib 
Error in extended source J mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
ERROR 
jPetroMagErr 
dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource, udsSource 
WSA 
Error in extended source J mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
ERROR 
jPetroMagErr 
uhsSource, uhsSourceAll 
WSAUHS 
Error in extended source J mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
ERROR 
jppErrBits 
calSource, calSynopticSource 
WSACalib 
additional WFAU postprocessing error bits in J 
int 
4 

0 
CODE_MISC 
Postprocessing error quality bit flags assigned (NB: from UKIDSS DR2 release onwards) in the WSA curation procedure for survey data. From least to most significant byte in the 4byte 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  1  15  Source in poor flat field region  32768  0x00008000  All but mosaics  2  16  Close to saturated  65536  0x00010000  All VDFS catalogues (though deeps excluded prior to DR8)  2  17  Photometric calibration probably subject to systematic error  131072  0x00020000  GPS only  2  19  Possible crosstalk artefact/contamination  524288  0x00080000  All but GPS  2  22  Lies within a dither offset of the stacked frame boundary  4194304  0x00400000  All but mosaics  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 K band sources in the LAS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information. 
jppErrBits 
dxsJKsource, gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, lasExtendedSource, lasPointSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource, udsSource 
WSA 
additional WFAU postprocessing error bits in J 
int 
4 

0 
CODE_MISC 
jppErrBits 
dxsSource, gcsSource, gpsSource, lasSource 
WSA 
additional WFAU postprocessing error bits in J 
int 
4 

0 
CODE_MISC 
Postprocessing error quality bit flags assigned (NB: from UKIDSS DR2 release onwards) in the WSA curation procedure for survey data. From least to most significant byte in the 4byte 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  1  15  Source in poor flat field region  32768  0x00008000  All but mosaics  2  16  Close to saturated  65536  0x00010000  All VDFS catalogues (though deeps excluded prior to DR8)  2  17  Photometric calibration probably subject to systematic error  131072  0x00020000  GPS only  2  19  Possible crosstalk artefact/contamination  524288  0x00080000  All but GPS  2  22  Lies within a dither offset of the stacked frame boundary  4194304  0x00400000  All but mosaics  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 K band sources in the LAS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information. 
jppErrBits 
lasYselJSourceRemeasurement 
WSA 
additional WFAU postprocessing error bits in J 
int 
4 

0 
meta.code 
Postprocessing error quality bit flags assigned (NB: from UKIDSS DR2 release onwards) in the WSA curation procedure for survey data. From least to most significant byte in the 4byte 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  1  15  Source in poor flat field region  32768  0x00008000  All but mosaics  2  16  Close to saturated  65536  0x00010000  All VDFS catalogues (though deeps excluded prior to DR8)  2  17  Photometric calibration probably subject to systematic error  131072  0x00020000  GPS only  2  19  Possible crosstalk artefact/contamination  524288  0x00080000  All but GPS  2  22  Lies within a dither offset of the stacked frame boundary  4194304  0x00400000  All but mosaics  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 K band sources in the LAS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information. 
jppErrBits 
uhsSource, uhsSourceAll 
WSAUHS 
additional WFAU postprocessing error bits in J 
int 
4 

0 
CODE_MISC 
Postprocessing error quality bit flags assigned (NB: from UKIDSS DR2 release onwards) in the WSA curation procedure for survey data. From least to most significant byte in the 4byte 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  1  15  Source in poor flat field region  32768  0x00008000  All but mosaics  2  16  Close to saturated  65536  0x00010000  All VDFS catalogues (though deeps excluded prior to DR8)  2  17  Photometric calibration probably subject to systematic error  131072  0x00020000  GPS only  2  19  Possible crosstalk artefact/contamination  524288  0x00080000  All but GPS  2  22  Lies within a dither offset of the stacked frame boundary  4194304  0x00400000  All but mosaics  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 K band sources in the LAS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information. 
jprobVar 
calVariability 
WSACalib 
Probability of variable from chisquare (and other data) 
real 
4 

0.9999995e9 

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

0.9999995e9 

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

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
jPsfMag 
calSource 
WSACalib 
Point source profilefitted J mag 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
jPsfMag 
dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource 
WSA 
Point source profilefitted J mag 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
jPsfMag 
reliableUdsSource, udsSource 
WSA 
Not available in SE output 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
jPsfMag 
uhsSource, uhsSourceAll 
WSAUHS 
Point source profilefitted J mag 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
jPsfMagErr 
calSource 
WSACalib 
Error in point source profilefitted J mag 
real 
4 
mag 
0.9999995e9 
ERROR 
jPsfMagErr 
dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource 
WSA 
Error in point source profilefitted J mag 
real 
4 
mag 
0.9999995e9 
ERROR 
jPsfMagErr 
reliableUdsSource, udsSource 
WSA 
Not available in SE output 
real 
4 
mag 
0.9999995e9 
ERROR 
jPsfMagErr 
uhsSource, uhsSourceAll 
WSAUHS 
Error in point source profilefitted J mag 
real 
4 
mag 
0.9999995e9 
ERROR 
jSeqNum 
calSource, calSynopticSource 
WSACalib 
the running number of the J detection 
int 
4 

99999999 
ID_NUMBER 
jSeqNum 
dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource, udsSource 
WSA 
the running number of the J detection 
int 
4 

99999999 
ID_NUMBER 
jSeqNum 
uhsSource, uhsSourceAll 
WSAUHS 
the running number of the J detection 
int 
4 

99999999 
ID_NUMBER 
jSerMag2D 
calSource 
WSACalib 
Extended source J mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
jSerMag2D 
dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource 
WSA 
Extended source J mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
jSerMag2D 
reliableUdsSource, udsSource 
WSA 
Not available in SE output 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
jSerMag2D 
uhsSource, uhsSourceAll 
WSAUHS 
Extended source J mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
jSerMag2DErr 
calSource 
WSACalib 
Error in extended source J mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
ERROR 
jSerMag2DErr 
dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource 
WSA 
Error in extended source J mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
ERROR 
jSerMag2DErr 
reliableUdsSource, udsSource 
WSA 
Not available in SE output 
real 
4 
mag 
0.9999995e9 
ERROR 
jSerMag2DErr 
uhsSource, uhsSourceAll 
WSAUHS 
Error in extended source J mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
ERROR 
jskewness 
calVariability 
WSACalib 
Skewness in J band (see Sesar et al. 2007) 
real 
4 

0.9999995e9 

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

0.9999995e9 

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

0.9999995e9 

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

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
jtotalPeriod 
dxsVariability, lasVariability, udsVariability 
WSA 
total period of observations (last obsfirst obs) 
real 
4 
days 
0.9999995e9 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
jtotalPeriod 
uhsVariability 
WSAUHS 
total period of observations (last obsfirst obs) 
real 
4 
days 
0.9999995e9 

The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. 
julianDayNum 
Multiframe 
WSA 
the Julian Day number of the UKIRT night 
int 
4 
Julian days 

time.epoch 
julianDayNum 
Multiframe 
WSACalib 
the Julian Day number of the UKIRT night 
int 
4 
Julian days 

time.epoch 
julianDayNum 
Multiframe 
WSATransit 
the Julian Day number of the UKIRT night 
int 
4 
Julian days 

time.epoch 
julianDayNum 
Multiframe 
WSAUHS 
the Julian Day number of the UKIRT night 
int 
4 
Julian days 

time.epoch 
julianDayNum 
MultiframeDetector 
WSA 
the Julian Day number of the UKIRT night {image primary HDU keyword: UTDATE} 
int 
4 
Julian days 

time.epoch 
julianDayNum 
MultiframeDetector 
WSACalib 
the Julian Day number of the UKIRT night {image primary HDU keyword: UTDATE} 
int 
4 
Julian days 

time.epoch 
julianDayNum 
MultiframeDetector 
WSATransit 
the Julian Day number of the UKIRT night {image primary HDU keyword: UTDATE} 
int 
4 
Julian days 

time.epoch 
julianDayNum 
MultiframeDetector 
WSAUHS 
the Julian Day number of the UKIRT night {image primary HDU keyword: UTDATE} 
int 
4 
Julian days 

time.epoch 
jVarClass 
calVariability 
WSACalib 
Classification of variability in this band 
smallint 
2 

9999 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
jVarClass 
dxsVariability, lasVariability, udsVariability 
WSA 
Classification of variability in this band 
smallint 
2 

9999 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
jVarClass 
uhsVariability 
WSAUHS 
Classification of variability in this band 
smallint 
2 

9999 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
jXi 
calSource, calSynopticSource 
WSACalib 
Offset of J detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
POS_EQ_RA_OFF 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 2.0 (UKIDSS LAS and GPS; UHS; also nonsurvey programmes) or 1.0 (UKIDSS GPS, DXS and UDS) arcseconds is used, the higher value enabling pairing of moving sources when epoch separations may be several years. 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 LAS, you might wish to insist that the offsets in the selected sample are all below 1 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. 
jXi 
dxsJKsource, gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, lasExtendedSource, lasPointSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource 
WSA 
Offset of J detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
POS_EQ_RA_OFF 
jXi 
dxsSource, gcsSource, gpsSource, lasSource, udsSource 
WSA 
Offset of J detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
POS_EQ_RA_OFF 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 2.0 (UKIDSS LAS and GPS; UHS; also nonsurvey programmes) or 1.0 (UKIDSS GPS, DXS and UDS) arcseconds is used, the higher value enabling pairing of moving sources when epoch separations may be several years. 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 LAS, you might wish to insist that the offsets in the selected sample are all below 1 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. 
jXi 
uhsSource, uhsSourceAll 
WSAUHS 
Offset of J detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
POS_EQ_RA_OFF 
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 2.0 (UKIDSS LAS and GPS; UHS; also nonsurvey programmes) or 1.0 (UKIDSS GPS, DXS and UDS) arcseconds is used, the higher value enabling pairing of moving sources when epoch separations may be several years. 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 LAS, you might wish to insist that the offsets in the selected sample are all below 1 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. 