H 
Name  Schema Table  Database  Description  Type  Length  Unit  Default Value  Unified Content Descriptor 
h2_1AperMag3 
[nspid]Source 
WSA NonSurvey 
Default point source H2_1 aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
h2_1AperMag3Err 
[nspid]Source 
WSA NonSurvey 
Error in default point source H2_1 mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
h2_1AperMag4 
[nspid]Source 
WSA NonSurvey 
Point source H2_1 aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
h2_1AperMag4Err 
[nspid]Source 
WSA NonSurvey 
Error in point source H2_1 mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
h2_1AperMag6 
[nspid]Source 
WSA NonSurvey 
Point source H2_1 aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
h2_1AperMag6Err 
[nspid]Source 
WSA NonSurvey 
Error in point source H2_1 mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
h2_1Class 
[nspid]Source 
WSA NonSurvey 
discrete image classification flag in H2_1 
smallint 
2 

9999 
CLASS_MISC 
h2_1ClassStat 
[nspid]Source 
WSA NonSurvey 
N(0,1) stellarnessofprofile statistic in H2_1 
real 
4 

0.9999995e9 
STAT_PROP 
h2_1Deblend 
[nspid]Source 
WSA NonSurvey 
placeholder flag indicating parent/child relation in H2_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. 
h2_1Ell 
[nspid]Source 
WSA NonSurvey 
1b/a, where a/b=semimajor/minor axes in H2_1 
real 
4 

0.9999995e9 
PHYS_ELLIPTICITY 
h2_1eNum 
[nspid]MergeLog 
WSA NonSurvey 
the extension number of this H2_1 frame 
tinyint 
1 


NUMBER 
h2_1ErrBits 
[nspid]Source 
WSA NonSurvey 
processing warning/error bitwise flags in H2_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. 
h2_1Eta 
[nspid]Source 
WSA NonSurvey 
Offset of H2_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. 
h2_1Gausig 
[nspid]Source 
WSA NonSurvey 
RMS of axes of ellipse fit in H2_1 
real 
4 
pixels 
0.9999995e9 
MORPH_PARAM 
h2_1HallMag 
[nspid]Source 
WSA NonSurvey 
Total point source H2_1 mag 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
h2_1HallMagErr 
[nspid]Source 
WSA NonSurvey 
Error in total point source H2_1 mag 
real 
4 
mag 
0.9999995e9 
ERROR 
h2_1mfID 
[nspid]MergeLog 
WSA NonSurvey 
the UID of the relevant H2_1 multiframe 
bigint 
8 


ID_FRAME 
h2_1mh2_1Ext 
[nspid]Source 
WSA NonSurvey 
Extended source colour H2_1H2_1 (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. 
h2_1mh2_1ExtErr 
[nspid]Source 
WSA NonSurvey 
Error on extended source colour H2_1H2_1 
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. 
h2_1mh2_1Pnt 
[nspid]Source 
WSA NonSurvey 
Point source colour H2_1H2_1 (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. 
h2_1mh2_1PntErr 
[nspid]Source 
WSA NonSurvey 
Error on point source colour H2_1H2_1 
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. 
h2_1PA 
[nspid]Source 
WSA NonSurvey 
ellipse fit celestial orientation in H2_1 
real 
4 
Degrees 
0.9999995e9 
POS_POSANG 
h2_1PetroMag 
[nspid]Source 
WSA NonSurvey 
Extended source H2_1 mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
h2_1PetroMagErr 
[nspid]Source 
WSA NonSurvey 
Error in extended source H2_1 mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
ERROR 
h2_1ppErrBits 
[nspid]Source 
WSA NonSurvey 
additional WFAU postprocessing error bits in H2_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. 
h2_1PsfMag 
[nspid]Source 
WSA NonSurvey 
Point source profilefitted H2_1 mag 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
h2_1PsfMagErr 
[nspid]Source 
WSA NonSurvey 
Error in point source profilefitted H2_1 mag 
real 
4 
mag 
0.9999995e9 
ERROR 
h2_1SeqNum 
[nspid]Source 
WSA NonSurvey 
the running number of the H2_1 detection 
int 
4 

99999999 
ID_NUMBER 
h2_1SerMag2D 
[nspid]Source 
WSA NonSurvey 
Extended source H2_1 mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
h2_1SerMag2DErr 
[nspid]Source 
WSA NonSurvey 
Error in extended source H2_1 mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
ERROR 
h2_1Xi 
[nspid]Source 
WSA NonSurvey 
Offset of H2_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. 
h2_2AperMag3 
[nspid]Source 
WSA NonSurvey 
Default point source H2_2 aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
h2_2AperMag3Err 
[nspid]Source 
WSA NonSurvey 
Error in default point source H2_2 mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
h2_2AperMag4 
[nspid]Source 
WSA NonSurvey 
Point source H2_2 aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
h2_2AperMag4Err 
[nspid]Source 
WSA NonSurvey 
Error in point source H2_2 mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
h2_2AperMag6 
[nspid]Source 
WSA NonSurvey 
Point source H2_2 aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
h2_2AperMag6Err 
[nspid]Source 
WSA NonSurvey 
Error in point source H2_2 mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
h2_2Class 
[nspid]Source 
WSA NonSurvey 
discrete image classification flag in H2_2 
smallint 
2 

9999 
CLASS_MISC 
h2_2ClassStat 
[nspid]Source 
WSA NonSurvey 
N(0,1) stellarnessofprofile statistic in H2_2 
real 
4 

0.9999995e9 
STAT_PROP 
h2_2Deblend 
[nspid]Source 
WSA NonSurvey 
placeholder flag indicating parent/child relation in H2_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. 
h2_2Ell 
[nspid]Source 
WSA NonSurvey 
1b/a, where a/b=semimajor/minor axes in H2_2 
real 
4 

0.9999995e9 
PHYS_ELLIPTICITY 
h2_2eNum 
[nspid]MergeLog 
WSA NonSurvey 
the extension number of this H2_2 frame 
tinyint 
1 


NUMBER 
h2_2ErrBits 
[nspid]Source 
WSA NonSurvey 
processing warning/error bitwise flags in H2_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. 
h2_2Eta 
[nspid]Source 
WSA NonSurvey 
Offset of H2_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. 
h2_2Gausig 
[nspid]Source 
WSA NonSurvey 
RMS of axes of ellipse fit in H2_2 
real 
4 
pixels 
0.9999995e9 
MORPH_PARAM 
h2_2HallMag 
[nspid]Source 
WSA NonSurvey 
Total point source H2_2 mag 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
h2_2HallMagErr 
[nspid]Source 
WSA NonSurvey 
Error in total point source H2_2 mag 
real 
4 
mag 
0.9999995e9 
ERROR 
h2_2mfID 
[nspid]MergeLog 
WSA NonSurvey 
the UID of the relevant H2_2 multiframe 
bigint 
8 


ID_FRAME 
h2_2mh2_2Ext 
[nspid]Source 
WSA NonSurvey 
Extended source colour H2_2H2_2 (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. 
h2_2mh2_2ExtErr 
[nspid]Source 
WSA NonSurvey 
Error on extended source colour H2_2H2_2 
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. 
h2_2mh2_2Pnt 
[nspid]Source 
WSA NonSurvey 
Point source colour H2_2H2_2 (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. 
h2_2mh2_2PntErr 
[nspid]Source 
WSA NonSurvey 
Error on point source colour H2_2H2_2 
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. 
h2_2PA 
[nspid]Source 
WSA NonSurvey 
ellipse fit celestial orientation in H2_2 
real 
4 
Degrees 
0.9999995e9 
POS_POSANG 
h2_2PetroMag 
[nspid]Source 
WSA NonSurvey 
Extended source H2_2 mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
h2_2PetroMagErr 
[nspid]Source 
WSA NonSurvey 
Error in extended source H2_2 mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
ERROR 
h2_2ppErrBits 
[nspid]Source 
WSA NonSurvey 
additional WFAU postprocessing error bits in H2_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. 
h2_2PsfMag 
[nspid]Source 
WSA NonSurvey 
Point source profilefitted H2_2 mag 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
h2_2PsfMagErr 
[nspid]Source 
WSA NonSurvey 
Error in point source profilefitted H2_2 mag 
real 
4 
mag 
0.9999995e9 
ERROR 
h2_2SeqNum 
[nspid]Source 
WSA NonSurvey 
the running number of the H2_2 detection 
int 
4 

99999999 
ID_NUMBER 
h2_2SerMag2D 
[nspid]Source 
WSA NonSurvey 
Extended source H2_2 mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
h2_2SerMag2DErr 
[nspid]Source 
WSA NonSurvey 
Error in extended source H2_2 mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
ERROR 
h2_2Xi 
[nspid]Source 
WSA NonSurvey 
Offset of H2_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. 
h2AperMag1 
[nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource 
WSA NonSurvey 
Default point source H2 aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
h2AperMag1 
[nspid]Source 
WSA NonSurvey 
Default point source H2 aperture corrected mag (1.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
h2AperMag1 
[nspid]SynopticSource 
WSA NonSurvey 
Extended source H2 aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
h2AperMag1Err 
[nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]Source 
WSA NonSurvey 
Error in point source H2 mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
h2AperMag1Err 
[nspid]SynopticSource 
WSA NonSurvey 
Error in extended source H2 mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
h2AperMag2 
[nspid]SynopticSource 
WSA NonSurvey 
Extended source H2 aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
h2AperMag2Err 
[nspid]SynopticSource 
WSA NonSurvey 
Error in extended source H2 mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
h2AperMag3 
[nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource 
WSA NonSurvey 
Default point source H2 aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
h2AperMag3 
[nspid]Source 
WSA NonSurvey 
Default point/extended source H2 aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
h2AperMag3 
[nspid]Source 
WSA NonSurvey 
Default point source H2 aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
h2AperMag3 
[nspid]SynopticSource 
WSA NonSurvey 
Default point/extended source H2 aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
h2AperMag3Err 
[nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]Source 
WSA NonSurvey 
Error in default point source H2 mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
h2AperMag3Err 
[nspid]Source, [nspid]SynopticSource 
WSA NonSurvey 
Error in default point/extended source H2 mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
h2AperMag4 
[nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]Source 
WSA NonSurvey 
Point source H2 aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
h2AperMag4 
[nspid]Source, [nspid]SynopticSource 
WSA NonSurvey 
Extended source H2 aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
h2AperMag4Err 
[nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]Source 
WSA NonSurvey 
Error in point source H2 mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
h2AperMag4Err 
[nspid]Source, [nspid]SynopticSource 
WSA NonSurvey 
Error in extended source H2 mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
h2AperMag5 
[nspid]SynopticSource 
WSA NonSurvey 
Extended source H2 aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
h2AperMag5Err 
[nspid]SynopticSource 
WSA NonSurvey 
Error in extended source H2 mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
h2AperMag6 
[nspid]Source 
WSA NonSurvey 
Extended source H2 aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
h2AperMag6 
[nspid]Source 
WSA NonSurvey 
Point source H2 aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
h2AperMag6Err 
[nspid]Source 
WSA NonSurvey 
Error in extended source H2 mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
h2AperMag6Err 
[nspid]Source 
WSA NonSurvey 
Error in point source H2 mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
h2aStratAst 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Strateva parameter, a, in fit to astrometric rms vs magnitude in H2 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. 
h2aStratAst 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Parameter, c0 from FerreiraLopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in H2 band. 
real 
4 

0.9999995e9 
stat.fit.param 
The best fit solution to the expected RMS position around the mean 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. 
h2aStratPht 
[nspid]CompMapVarFrameSetInfo, [nspid]QsoMapVarFrameSetInfo 
WSA NonSurvey 
Strateva parameter, a, in fit to photometric rms vs magnitude in H2 band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param 
The best fit solution to the expected RMS brightness (in magnitudes) 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. 
h2aStratPht 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Strateva parameter, a, in fit to photometric rms vs magnitude in H2 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. 
h2aStratPht 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Parameter, c0 from FerreiraLopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in H2 band. 
real 
4 

0.9999995e9 
stat.fit.param 
The best fit solution to the expected RMS brightness (in magnitudes) 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. 
h2bestAper 
[nspid]CompMapVariability, [nspid]QsoMapVariability 
WSA NonSurvey 
Best aperture (13) for photometric statistics in the H2 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) 
h2bestAper 
[nspid]Variability 
WSA NonSurvey 
Best aperture (16) for photometric statistics in the H2 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) 
h2bStratAst 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Strateva parameter, b, in fit to astrometric rms vs magnitude in H2 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. 
h2bStratAst 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Parameter, c1 from FerreiraLopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in H2 band. 
real 
4 

0.9999995e9 
stat.fit.param 
The best fit solution to the expected RMS position around the mean 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. 
h2bStratPht 
[nspid]CompMapVarFrameSetInfo, [nspid]QsoMapVarFrameSetInfo 
WSA NonSurvey 
Strateva parameter, b, in fit to photometric rms vs magnitude in H2 band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param 
The best fit solution to the expected RMS brightness (in magnitudes) 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. 
h2bStratPht 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Strateva parameter, b, in fit to photometric rms vs magnitude in H2 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. 
h2bStratPht 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Parameter, c1 from FerreiraLopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in H2 band. 
real 
4 

0.9999995e9 
stat.fit.param 
The best fit solution to the expected RMS brightness (in magnitudes) 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. 
h2chiSqAst 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Goodness of fit of Strateva function to astrometric data in H2 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. 
h2chiSqAst 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Goodness of fit of Strateva function to astrometric data in H2 band 
real 
4 

0.9999995e9 
stat.fit.goodness 
The best fit solution to the expected RMS position around the mean 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. 
h2chiSqpd 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
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. 
h2chiSqPht 
[nspid]CompMapVarFrameSetInfo, [nspid]QsoMapVarFrameSetInfo 
WSA NonSurvey 
Goodness of fit of Strateva function to photometric data in H2 band 
real 
4 

0.9999995e9 
stat.fit.goodness 
The best fit solution to the expected RMS brightness (in magnitudes) 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. 
h2chiSqPht 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Goodness of fit of Strateva function to photometric data in H2 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. 
h2Class 
[nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]Source, [nspid]SynopticSource 
WSA NonSurvey 
discrete image classification flag in H2 
smallint 
2 

9999 
CLASS_MISC 
h2ClassStat 
[nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]Source, [nspid]SynopticSource 
WSA NonSurvey 
N(0,1) stellarnessofprofile statistic in H2 
real 
4 

0.9999995e9 
STAT_PROP 
h2cStratAst 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Strateva parameter, c, in fit to astrometric rms vs magnitude in H2 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. 
h2cStratAst 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Parameter, c2 from FerreiraLopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in H2 band. 
real 
4 

0.9999995e9 
stat.fit.param 
The best fit solution to the expected RMS position around the mean 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. 
h2cStratPht 
[nspid]CompMapVarFrameSetInfo, [nspid]QsoMapVarFrameSetInfo 
WSA NonSurvey 
Strateva parameter, c, in fit to photometric rms vs magnitude in H2 band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 
stat.fit.param 
The best fit solution to the expected RMS brightness (in magnitudes) 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. 
h2cStratPht 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Strateva parameter, c, in fit to photometric rms vs magnitude in H2 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. 
h2cStratPht 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Parameter, c2 from FerreiraLopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in H2 band. 
real 
4 

0.9999995e9 
stat.fit.param 
The best fit solution to the expected RMS brightness (in magnitudes) 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. 
h2Deblend 
[nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]SynopticSource 
WSA NonSurvey 
placeholder flag indicating parent/child relation in H2 
int 
4 

99999999 
CODE_MISC 
h2Deblend 
[nspid]Source 
WSA NonSurvey 
placeholder flag indicating parent/child relation in H2 
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. 
h2dStratAst 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Parameter, c3 from FerreiraLopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in H2 band. 
real 
4 

0.9999995e9 
stat.fit.param 
The best fit solution to the expected RMS position around the mean 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. 
h2dStratPht 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Parameter, c0 from FerreiraLopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in H2 band. 
real 
4 

0.9999995e9 
stat.fit.param 
The best fit solution to the expected RMS brightness (in magnitudes) 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. 
h2Ell 
[nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]Source, [nspid]SynopticSource 
WSA NonSurvey 
1b/a, where a/b=semimajor/minor axes in H2 
real 
4 

0.9999995e9 
PHYS_ELLIPTICITY 
h2eNum 
[nspid]JHKmergeLog, [nspid]MergeLog, [nspid]SynopticMergeLog 
WSA NonSurvey 
the extension number of this H2 frame 
tinyint 
1 


NUMBER 
h2ErrBits 
[nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource 
WSA NonSurvey 
processing warning/error bitwise flags in H2 
int 
4 

99999999 
CODE_MISC 
h2ErrBits 
[nspid]Source, [nspid]SynopticSource 
WSA NonSurvey 
processing warning/error bitwise flags in H2 
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. 
h2Eta 
[nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource 
WSA NonSurvey 
Offset of H2 detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
POS_EQ_DEC_OFF 
h2Eta 
[nspid]Source, [nspid]SynopticSource 
WSA NonSurvey 
Offset of H2 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. 
h2expML 
[nspid]CompMapVarFrameSetInfo, [nspid]QsoMapVarFrameSetInfo 
WSA NonSurvey 
Expected magnitude limit of frameSet in this in H2 band. 
real 
4 
mag 
0.9999995e9 
phot.mag;stat.max 
h2expML 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Expected magnitude limit of frameSet in this in H2 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. 
h2ExpRms 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in H2 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. 
h2Gausig 
[nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]Source, [nspid]SynopticSource 
WSA NonSurvey 
RMS of axes of ellipse fit in H2 
real 
4 
pixels 
0.9999995e9 
MORPH_PARAM 
h2HallMag 
[nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]Source 
WSA NonSurvey 
Total point source H2 mag 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
h2HallMagErr 
[nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]Source 
WSA NonSurvey 
Error in total point source H2 mag 
real 
4 
mag 
0.9999995e9 
ERROR 
h2IntRms 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
Intrinsic rms in H2band 
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. 
h2isDefAst 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Use a default model for the astrometric noise in H2 band. 
tinyint 
1 

0 

h2isDefAst 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Use a default model for the astrometric noise in H2 band. 
tinyint 
1 

0 
meta.code 
h2isDefPht 
[nspid]CompMapVarFrameSetInfo, [nspid]QsoMapVarFrameSetInfo 
WSA NonSurvey 
Use a default model for the photometric noise in H2 band. 
tinyint 
1 

0 
meta.code 
h2isDefPht 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Use a default model for the photometric noise in H2 band. 
tinyint 
1 

0 

h2MagMAD 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
Median Absolute Deviation of H2 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. 
h2MagRms 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
rms of H2 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. 
h2maxCadence 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
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. 
h2MaxMag 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
Maximum magnitude in H2 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. 
h2meanMag 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
Mean H2 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. 
h2medCadence 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
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. 
h2medianMag 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
Median H2 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. 
h2mfID 
[nspid]JHKmergeLog, [nspid]MergeLog, [nspid]SynopticMergeLog 
WSA NonSurvey 
the UID of the relevant H2 multiframe 
bigint 
8 


ID_FRAME 
h2minCadence 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
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. 
h2MinMag 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
Minimum magnitude in H2 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. 
h2mkExt 
[nspid]Source 
WSA NonSurvey 
Extended source colour H2K (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. 
h2mkExtErr 
[nspid]Source 
WSA NonSurvey 
Error on extended source colour H2K 
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. 
h2mkPnt 
[nspid]Source, [nspid]SynopticSource 
WSA NonSurvey 
Point source colour H2K (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. 
h2mkPntErr 
[nspid]Source, [nspid]SynopticSource 
WSA NonSurvey 
Error on point source colour H2K 
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. 
h2ndof 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
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. 
h2nDofAst 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Number of degrees of freedom of astrometric fit in H2 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. 
h2nDofAst 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Number of degrees of freedom of astrometric fit in H2 band. 
smallint 
2 

9999 
stat.fit.dof;stat.param 
The best fit solution to the expected RMS position around the mean 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. 
h2nDofPht 
[nspid]CompMapVarFrameSetInfo, [nspid]QsoMapVarFrameSetInfo 
WSA NonSurvey 
Number of degrees of freedom of photometric fit in H2 band. 
smallint 
2 

9999 
stat.fit.dof;stat.param 
The best fit solution to the expected RMS brightness (in magnitudes) 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. 
h2nDofPht 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Number of degrees of freedom of photometric fit in H2 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. 
h2nFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H2 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. 
h2nFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H2 band flagged as potentially spurious by u05b19Detection.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. 
h2nFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H2 band flagged as potentially spurious by u05bh53Detection.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. 
h2nFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H2 band flagged as potentially spurious by u06ad5Detection.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. 
h2nFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H2 band flagged as potentially spurious by u09b8Detection.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. 
h2nFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H2 band flagged as potentially spurious by u10a2Detection.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. 
h2nFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H2 band flagged as potentially spurious by u10a9Detection.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. 
h2nFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H2 band flagged as potentially spurious by u10bd03Detection.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. 
h2nFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H2 band flagged as potentially spurious by u12bkasi1Detection.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. 
h2nFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H2 band flagged as potentially spurious by u13a01Detection.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. 
h2nFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H2 band flagged as potentially spurious by u15bua11Detection.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. 
h2nFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H2 band flagged as potentially spurious by u15bua19Detection.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. 
h2nFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H2 band flagged as potentially spurious by u16ah08Detection.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. 
h2nFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H2 band flagged as potentially spurious by u16aua18Detection.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. 
h2nFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H2 band flagged as potentially spurious by u16bua17Detection.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. 
h2nFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H2 band flagged as potentially spurious by u17buo01Detection.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. 
h2nFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H2 band flagged as potentially spurious by userv1721Detection.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. 
h2nFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H2 band flagged as potentially spurious by userv1802Detection.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. 
h2nFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H2 band flagged as potentially spurious by wserv6Detection.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. 
h2nGoodObs 
[nspid]Variability 
WSA NonSurvey 
Number of good detections in H2 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. 
h2Ngt3sig 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
Number of good detections in H2band that are more than 3 sigma deviations (h2AperMagN < (h2MeanMag3*h2MagRms) 
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. 
h2Ngt3sig 
[nspid]Variability 
WSA NonSurvey 
Number of good detections in H2band 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. 
h2nMissingObs 
[nspid]Variability 
WSA NonSurvey 
Number of H2 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. 
h2nNegFlagObs 
[nspid]CompMapVariability, [nspid]QsoMapVariability 
WSA NonSurvey 
Number of flagged negative measurements in H2 band by wserv1000MapRemeasurement.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. 
h2nNegObs 
[nspid]CompMapVariability, [nspid]QsoMapVariability 
WSA NonSurvey 
Number of unflagged negative measurements H2 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. 
h2nPosFlagObs 
[nspid]CompMapVariability, [nspid]QsoMapVariability 
WSA NonSurvey 
Number of flagged positive measurements in H2 band by wserv1000MapRemeasurement.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. 
h2nPosObs 
[nspid]CompMapVariability, [nspid]QsoMapVariability 
WSA NonSurvey 
Number of unflagged positive measurements in H2 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. 
h2PA 
[nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]Source, [nspid]SynopticSource 
WSA NonSurvey 
ellipse fit celestial orientation in H2 
real 
4 
Degrees 
0.9999995e9 
POS_POSANG 
h2PetroMag 
[nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]Source 
WSA NonSurvey 
Extended source H2 mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
h2PetroMagErr 
[nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]Source 
WSA NonSurvey 
Error in extended source H2 mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
ERROR 
h2ppErrBits 
[nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource 
WSA NonSurvey 
additional WFAU postprocessing error bits in H2 
int 
4 

0 
CODE_MISC 
h2ppErrBits 
[nspid]Source, [nspid]SynopticSource 
WSA NonSurvey 
additional WFAU postprocessing error bits in H2 
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. 
h2probVar 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
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. 
h2PsfMag 
[nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]Source 
WSA NonSurvey 
Point source profilefitted H2 mag 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
h2PsfMagErr 
[nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]Source 
WSA NonSurvey 
Error in point source profilefitted H2 mag 
real 
4 
mag 
0.9999995e9 
ERROR 
h2SeqNum 
[nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]Source, [nspid]SynopticSource 
WSA NonSurvey 
the running number of the H2 detection 
int 
4 

99999999 
ID_NUMBER 
h2SerMag2D 
[nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]Source 
WSA NonSurvey 
Extended source H2 mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
h2SerMag2DErr 
[nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]Source 
WSA NonSurvey 
Error in extended source H2 mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
ERROR 
h2skewness 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
Skewness in H2 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. 
h2totalPeriod 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
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. 
h2VarClass 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
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. 
h2Xi 
[nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource 
WSA NonSurvey 
Offset of H2 detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
POS_EQ_RA_OFF 
h2Xi 
[nspid]Source, [nspid]SynopticSource 
WSA NonSurvey 
Offset of H2 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. 
halfRad 
[nspid]MapRemeasurement 
WSA NonSurvey 
Halflight radius (SE: FRAC_RADIUS, calcuated assuming Kron flux is total flux; CASU: default) {catalogue TType keyword: Half_radius} 
real 
4 
pixels 

phys.angSize 
hallFlux 
[nspid]Detection 
WSA NonSurvey 
Not available in SE output {catalogue TType keyword: Hall_flux} 
real 
4 



hallFlux 
[nspid]Detection 
WSA NonSurvey 
flux within circular aperture to k × r_h; k = 5; alternative total flux {catalogue TType keyword: Hall_flux} 
real 
4 
ADU 

PHOT_INTENSITY_ADU 
hallFlux 
[nspid]UKIDSSDetection 
WSA NonSurvey 
flux within circular aperture to k × r_h; k = 5; alternative total flux 
real 
4 
ADU 

PHOT_INTENSITY_ADU 
hallFluxErr 
[nspid]Detection 
WSA NonSurvey 
Not available in SE output {catalogue TType keyword: Hall_flux_err} 
real 
4 



hallFluxErr 
[nspid]Detection 
WSA NonSurvey 
error on Hall flux {catalogue TType keyword: Hall_flux_err} 
real 
4 
ADU 

ERROR 
hallFluxErr 
[nspid]UKIDSSDetection 
WSA NonSurvey 
error on Hall flux 
real 
4 
ADU 

ERROR 
hallMag 
[nspid]Detection 
WSA NonSurvey 
Not available in SE output 
real 
4 



hallMag 
[nspid]Detection, [nspid]UKIDSSDetection 
WSA NonSurvey 
Calibrated magnitude within circular aperture r_hall 
real 
4 
mag 

PHOT_INTMAG 
hallMagErr 
[nspid]Detection 
WSA NonSurvey 
Not available in SE output 
real 
4 



hallMagErr 
[nspid]Detection, [nspid]UKIDSSDetection 
WSA NonSurvey 
Calibrated error on Hall magnitude 
real 
4 
mag 

ERROR 
hallRad 
[nspid]Detection 
WSA NonSurvey 
Not available in SE output {catalogue TType keyword: Hall_radius} 
real 
4 
pixels 

EXTENSION_RAD 
hallRad 
[nspid]Detection 
WSA NonSurvey 
r_h image scale radius eg. Hall & Mackay 1984 MNRAS 210 979 {catalogue TType keyword: Hall_radius} 
real 
4 
pixels 

EXTENSION_RAD 
hallRad 
[nspid]UKIDSSDetection 
WSA NonSurvey 
r_h image scale radius eg. Hall & Mackay 1984 MNRAS 210 979 
real 
4 
pixels 

EXTENSION_RAD 
hAperMag1 
[nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource 
WSA NonSurvey 
Default point source H aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
hAperMag1 
[nspid]Source 
WSA NonSurvey 
Default point source H aperture corrected mag (1.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
hAperMag1 
[nspid]SynopticSource 
WSA NonSurvey 
Extended source H aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
hAperMag1Err 
[nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]Source 
WSA NonSurvey 
Error in point source H mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
hAperMag1Err 
[nspid]SynopticSource 
WSA NonSurvey 
Error in extended source H mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
hAperMag2 
[nspid]SynopticSource 
WSA NonSurvey 
Extended source H aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
hAperMag2Err 
[nspid]SynopticSource 
WSA NonSurvey 
Error in extended source H mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
hAperMag3 
[nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]YJHKsource, [nspid]ZYJHKsource 
WSA NonSurvey 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
hAperMag3 
[nspid]Source 
WSA NonSurvey 
Default point/extended source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
hAperMag3 
[nspid]Source 
WSA NonSurvey 
Default point/extended source H mag, no aperture correction applied If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
hAperMag3 
[nspid]Source 
WSA NonSurvey 
Default point source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
hAperMag3 
[nspid]SynopticSource 
WSA NonSurvey 
Default point/extended source H aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
hAperMag3 
[nspid]UdsSource 
WSA NonSurvey 
Default point/extended source H mag, no aperture correction applied 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
hAperMag3Err 
[nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]Source, [nspid]YJHKsource, [nspid]ZYJHKsource 
WSA NonSurvey 
Error in default point source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
hAperMag3Err 
[nspid]Source, [nspid]SynopticSource, [nspid]UdsSource 
WSA NonSurvey 
Error in default point/extended source H mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
hAperMag4 
[nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]Source, [nspid]YJHKsource, [nspid]ZYJHKsource 
WSA NonSurvey 
Point source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
hAperMag4 
[nspid]Source, [nspid]SynopticSource 
WSA NonSurvey 
Extended source H aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
hAperMag4 
[nspid]Source, [nspid]UdsSource 
WSA NonSurvey 
Extended source H mag, no aperture correction applied 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
hAperMag4Err 
[nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]Source, [nspid]YJHKsource, [nspid]ZYJHKsource 
WSA NonSurvey 
Error in point source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
hAperMag4Err 
[nspid]Source, [nspid]SynopticSource, [nspid]UdsSource 
WSA NonSurvey 
Error in extended source H mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
hAperMag5 
[nspid]SynopticSource 
WSA NonSurvey 
Extended source H aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
hAperMag5Err 
[nspid]SynopticSource 
WSA NonSurvey 
Error in extended source H mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
hAperMag6 
[nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]Source, [nspid]YJHKsource, [nspid]ZYJHKsource 
WSA NonSurvey 
Point source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
hAperMag6 
[nspid]Source 
WSA NonSurvey 
Extended source H aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
hAperMag6 
[nspid]Source, [nspid]UdsSource 
WSA NonSurvey 
Extended source H mag, no aperture correction applied 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
hAperMag6Err 
[nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]Source, [nspid]YJHKsource, [nspid]ZYJHKsource 
WSA NonSurvey 
Error in point source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
hAperMag6Err 
[nspid]Source, [nspid]UdsSource 
WSA NonSurvey 
Error in extended source H mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
haStratAst 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Strateva parameter, a, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

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

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

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

0.9999995e9 

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

0.9999995e9 
stat.fit.param;em.IR.H 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hbestAper 
[nspid]CompMapVariability, [nspid]QsoMapVariability 
WSA NonSurvey 
Best aperture (13) for photometric statistics in the H band 
int 
4 

9999 

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

9999 

Aperture magnitude (16) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) 
hbStratAst 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Strateva parameter, b, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

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

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

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

0.9999995e9 

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

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

0.9999995e9 

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

0.9999995e9 
stat.fit.goodness;em.IR.H 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hchiSqpd 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
Chi square (per degree of freedom) fit to data (mean and expected rms) 
real 
4 

0.9999995e9 

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

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

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hClass 
[nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]Source, [nspid]SynopticSource, [nspid]UdsSource, [nspid]YJHKsource, [nspid]ZYJHKsource 
WSA NonSurvey 
discrete image classification flag in H 
smallint 
2 

9999 
CLASS_MISC 
hClassStat 
[nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]Source, [nspid]SynopticSource, [nspid]YJHKsource, [nspid]ZYJHKsource 
WSA NonSurvey 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
STAT_PROP 
hClassStat 
[nspid]Source, [nspid]UdsSource 
WSA NonSurvey 
SExtractor classification statistic in H 
real 
4 

0.9999995e9 
STAT_PROP 
hcStratAst 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Strateva parameter, c, in fit to astrometric rms vs magnitude in H band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

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

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

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

0.9999995e9 

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

0.9999995e9 
stat.fit.param;em.IR.H 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hDeblend 
[nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]Source, [nspid]SynopticSource, [nspid]UdsSource, [nspid]YJHKsource, [nspid]ZYJHKsource 
WSA NonSurvey 
placeholder flag indicating parent/child relation in H 
int 
4 

99999999 
CODE_MISC 
hDeblend 
[nspid]Source 
WSA NonSurvey 
placeholder flag indicating parent/child relation in H 
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. 
hdStratAst 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Parameter, c3 from FerreiraLopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in H band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hdStratPht 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Parameter, c0 from FerreiraLopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in H band. 
real 
4 

0.9999995e9 
stat.fit.param;em.IR.H 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hdtFile 
[nspid]Multiframe 
WSA NonSurvey 
Name of global hdt file {image primary HDU keyword: HDTFILE} 
varchar 
32 

NONE 

hdtFileExt 
[nspid]MultiframeDetector 
WSA NonSurvey 
Name of cameraspecific hdt file {image extension keyword: HDTFILE2} 
varchar 
32 

NONE 
?? 
hEll 
[nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]Source, [nspid]SynopticSource, [nspid]UdsSource, [nspid]YJHKsource, [nspid]ZYJHKsource 
WSA NonSurvey 
1b/a, where a/b=semimajor/minor axes in H 
real 
4 

0.9999995e9 
PHYS_ELLIPTICITY 
heNum 
[nspid]JHKmergeLog, [nspid]JKmergeLog, [nspid]MergeLog, [nspid]SynopticMergeLog, [nspid]YJHKmergeLog, [nspid]ZYJHKmergeLog 
WSA NonSurvey 
the extension number of this H frame 
tinyint 
1 


NUMBER 
hErrBits 
[nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]UdsSource, [nspid]YJHKsource, [nspid]ZYJHKsource 
WSA NonSurvey 
processing warning/error bitwise flags in H 
int 
4 

99999999 
CODE_MISC 
hErrBits 
[nspid]Source 
WSA NonSurvey 
processing warning/error bitwise flags in H 
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  

hErrBits 
[nspid]Source, [nspid]SynopticSource 
WSA NonSurvey 
processing warning/error bitwise flags in H 
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. 
hEta 
[nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]UdsSource, [nspid]YJHKsource, [nspid]ZYJHKsource 
WSA NonSurvey 
Offset of H detection from master position (+north/south) 
real 
4 
arcsec 
0.9999995e9 
POS_EQ_DEC_OFF 
hEta 
[nspid]Source, [nspid]SynopticSource 
WSA NonSurvey 
Offset of H 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. 
hexpML 
[nspid]CompMapVarFrameSetInfo, [nspid]QsoMapVarFrameSetInfo 
WSA NonSurvey 
Expected magnitude limit of frameSet in this in H band. 
real 
4 
mag 
0.9999995e9 
phot.mag;em.IR.H;stat.max 
hexpML 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Expected magnitude limit of frameSet in this in H 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. 
hExpRms 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in H band 
real 
4 
mag 
0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hGausig 
[nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]Source, [nspid]SynopticSource, [nspid]UdsSource, [nspid]YJHKsource, [nspid]ZYJHKsource 
WSA NonSurvey 
RMS of axes of ellipse fit in H 
real 
4 
pixels 
0.9999995e9 
MORPH_PARAM 
hHallMag 
[nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]Source, [nspid]YJHKsource, [nspid]ZYJHKsource 
WSA NonSurvey 
Total point source H mag 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
hHallMag 
[nspid]Source, [nspid]UdsSource 
WSA NonSurvey 
Not available in SE output 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
hHallMagErr 
[nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]Source, [nspid]YJHKsource, [nspid]ZYJHKsource 
WSA NonSurvey 
Error in total point source H mag 
real 
4 
mag 
0.9999995e9 
ERROR 
hHallMagErr 
[nspid]Source, [nspid]UdsSource 
WSA NonSurvey 
Not available in SE output 
real 
4 
mag 
0.9999995e9 
ERROR 
hIntRms 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
Intrinsic rms in Hband 
real 
4 
mag 
0.9999995e9 

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

0 

hisDefAst 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Use a default model for the astrometric noise in H band. 
tinyint 
1 

0 
meta.code;em.IR.H 
hisDefPht 
[nspid]CompMapVarFrameSetInfo, [nspid]QsoMapVarFrameSetInfo 
WSA NonSurvey 
Use a default model for the photometric noise in H band. 
tinyint 
1 

0 
meta.code;em.IR.H 
hisDefPht 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Use a default model for the photometric noise in H band. 
tinyint 
1 

0 

hkiWS 
[nspid]Variability 
WSA NonSurvey 
WelchStetson statistic between H and K. 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. 
hlCircRadAs 
[nspid]MapRemeasurement 
WSA NonSurvey 
Circular halflight radius computed from curve of growth assuming petrosian flux is 90% of total (CASU: default) 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCircRadErrAs 
[nspid]MapRemeasurement 
WSA NonSurvey 
Error in hlCircRadAs (CASU: default) 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlCorSMjRadAs 
[nspid]MapRemeasurement 
WSA NonSurvey 
Seeing corrected Halflight semimajor axis (CASU: default) 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCorSMnRadAs 
[nspid]MapRemeasurement 
WSA NonSurvey 
Seeing corrected Halflight semiminor axis (CASU: default) 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlGeoRadAs 
[nspid]MapRemeasurement 
WSA NonSurvey 
Geometric halflight radius (CASU: default) 
real 
4 
arcsec 
0.9999995e9 
phys.angSize 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMjRadAs 
[nspid]MapRemeasurement 
WSA NonSurvey 
Halflight semimajor axis (CASU: default) 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.smajAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hlSMnRadAs 
[nspid]MapRemeasurement 
WSA NonSurvey 
Halflight semiminor axis (CASU: default) 
real 
4 
arcsec 
0.9999995e9 
phys.angSize.sminAxis 
hlCircRad is computed from the curve of growth of the 13 aperture fluxes and the Petrosian flux, assuming that this contains 90% of the light of the galaxy. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is calculated from the covariance matrix with half the pixel size added in quadrature. The semimajor axis is calculated using hlSmjRad/hlCircRad=1.824/((1+(r/0.3091)^2)^0.2430) where r=1ellipticity. This moffat profile provides a good correction to all Sersic profiles, with a maximum of 10% deviation at high ellipticities (>0.9) for Sersic incices between 1 and 6. The hlSmnRad is calculated as (1ellipticity)*hlSmjRad and hlGeoRad is sqrt(hlSmnRad*hlSmjRad). The hlCorSmjRad and hlCorSmnRad are calculated from the prescription in the appendix of Driver et al. 2005, MNRAS, 360, 81, using an eta value of 0.5. A quadratic function is fitted to the 5 data closest to the first aperture with more than 50% of the flux to smooth out any bad points. This is fit using a singular value decomposition of the linear least squares matrix. The error hlCircRadErr is not calculated for deep stack catalogues by SExtractor, but for intermediate catalogues it is calculated from the covariance matrix with half the pixel size added in quadrature. 
hMag 
[nspid]FSstars 
WSA NonSurvey 
H band total magnitude on the MKO(UFTI) system 
real 
4 
mag 

phot.mag 
hMagErr 
[nspid]FSstars 
WSA NonSurvey 
H band magnitude error 
real 
4 
mag 

stat.error 
hMagMAD 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
Median Absolute Deviation of H 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. 
hMagRms 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
rms of H 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. 
hmaxCadence 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
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. 
hMaxMag 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
Maximum magnitude in H 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. 
hmeanMag 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
Mean H 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. 
hmedCadence 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
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. 
hmedianMag 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
Median H 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. 
hmfID 
[nspid]JHKmergeLog, [nspid]JKmergeLog, [nspid]MergeLog, [nspid]SynopticMergeLog, [nspid]YJHKmergeLog, [nspid]ZYJHKmergeLog 
WSA NonSurvey 
the UID of the relevant H multiframe 
bigint 
8 


ID_FRAME 
hminCadence 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
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. 
hMinMag 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
Minimum magnitude in H 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. 
hmk_1Ext 
[nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]ZYJHKsource 
WSA NonSurvey 
Extended source colour HK_1 (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
hmk_1Ext 
[nspid]Source 
WSA NonSurvey 
Extended source colour HK_1 (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. 
hmk_1ExtErr 
[nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]ZYJHKsource 
WSA NonSurvey 
Error on extended source colour HK_1 
real 
4 
mag 
0.9999995e9 
ERROR 
hmk_1ExtErr 
[nspid]Source 
WSA NonSurvey 
Error on extended source colour HK_1 
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. 
hmk_1Pnt 
[nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]ZYJHKsource 
WSA NonSurvey 
Point source colour HK_1 (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
hmk_1Pnt 
[nspid]Source 
WSA NonSurvey 
Point source colour HK_1 (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. 
hmk_1PntErr 
[nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]ZYJHKsource 
WSA NonSurvey 
Error on point source colour HK_1 
real 
4 
mag 
0.9999995e9 
ERROR 
hmk_1PntErr 
[nspid]Source 
WSA NonSurvey 
Error on point source colour HK_1 
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. 
hmk_2Ext 
[nspid]GcsPointSource, [nspid]PointSource, [nspid]ZYJHKsource 
WSA NonSurvey 
Extended source colour HK_2 (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
hmk_2Ext 
[nspid]Source 
WSA NonSurvey 
Extended source colour HK_2 (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. 
hmk_2ExtErr 
[nspid]GcsPointSource, [nspid]PointSource, [nspid]ZYJHKsource 
WSA NonSurvey 
Error on extended source colour HK_2 
real 
4 
mag 
0.9999995e9 
ERROR 
hmk_2ExtErr 
[nspid]Source 
WSA NonSurvey 
Error on extended source colour HK_2 
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. 
hmk_2Pnt 
[nspid]GcsPointSource, [nspid]PointSource, [nspid]ZYJHKsource 
WSA NonSurvey 
Point source colour HK_2 (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
hmk_2Pnt 
[nspid]Source 
WSA NonSurvey 
Point source colour HK_2 (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. 
hmk_2PntErr 
[nspid]GcsPointSource, [nspid]PointSource, [nspid]ZYJHKsource 
WSA NonSurvey 
Error on point source colour HK_2 
real 
4 
mag 
0.9999995e9 
ERROR 
hmk_2PntErr 
[nspid]Source 
WSA NonSurvey 
Error on point source colour HK_2 
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. 
hmkExt 
[nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]UdsSource, [nspid]YJHKsource, [nspid]ZYJHKsource 
WSA NonSurvey 
Extended source colour HK (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
hmkExt 
[nspid]Source 
WSA NonSurvey 
Extended source colour HK (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. 
hmkExtErr 
[nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]UdsSource, [nspid]YJHKsource, [nspid]ZYJHKsource 
WSA NonSurvey 
Error on extended source colour HK 
real 
4 
mag 
0.9999995e9 
ERROR 
hmkExtErr 
[nspid]Source 
WSA NonSurvey 
Error on extended source colour HK 
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. 
hmkPnt 
[nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]UdsSource, [nspid]YJHKsource, [nspid]ZYJHKsource 
WSA NonSurvey 
Point source colour HK (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
hmkPnt 
[nspid]Source, [nspid]SynopticSource 
WSA NonSurvey 
Point source colour HK (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. 
hmkPntErr 
[nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]UdsSource, [nspid]YJHKsource, [nspid]ZYJHKsource 
WSA NonSurvey 
Error on point source colour HK 
real 
4 
mag 
0.9999995e9 
ERROR 
hmkPntErr 
[nspid]Source, [nspid]SynopticSource 
WSA NonSurvey 
Error on point source colour HK 
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. 
hndof 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
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. 
hnDofAst 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Number of degrees of freedom of astrometric fit in H 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. 
hnDofAst 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Number of degrees of freedom of astrometric fit in H band. 
smallint 
2 

9999 
stat.fit.dof;stat.param;em.IR.H 
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. 
hnDofPht 
[nspid]CompMapVarFrameSetInfo, [nspid]QsoMapVarFrameSetInfo 
WSA NonSurvey 
Number of degrees of freedom of photometric fit in H band. 
smallint 
2 

9999 
stat.fit.dof;stat.param;em.IR.H 
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hnDofPht 
[nspid]VarFrameSetInfo 
WSA NonSurvey 
Number of degrees of freedom of photometric fit in H 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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H 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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H 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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u05b13Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u05b17Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u05bh24Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u06a3Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u06b30Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u06b40Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u06bj5Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u07a24Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u07ad2Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u07ah16Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u07ah30Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u07ah51Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u07b11Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u07b13Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u07b17Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u07b6Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u08ah61Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u08bh2Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u09a1Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u09a5Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u09ah33Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u09b1Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u09b7Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u09bd1Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u09bh14Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u09bh15Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u09bh50Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u09bk2Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u10a6Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u10ad6Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u10ah99Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u10aj2Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u10aj5Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u10ak1Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u10ak2Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u10ak4Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u10b11Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u10b8Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u10bj2Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u10bk1Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u10bk2Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u11ak3Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u11bd2Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u11bk1Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u11bk2Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u11bk3Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u11bk4Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u11bk4bDetection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u11bk5Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u12ah17bDetection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u12ak1Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u12ak2Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u12ak3Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u12ak5Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u12bd1Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u12bd2Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u12bd3Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u12bd7Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u12bk3Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u12bk4Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u13a01Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u13ad1Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u13ah28bDetection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u13akasi1Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u13akasi2Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u13akasi3Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u14bua06Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u14bua16Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u14bua17Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u15ana05Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u15aua12aDetection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u15bh01Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u15bh02Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u15bua02aDetection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u15bua12aDetection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u15bua13aDetection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u15bua19Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u16ah04Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u16ah08Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u16aua08aDetection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u16aua18Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u16bh03Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u16bua02Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u17ah04Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u17bh03Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u17buo01Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u18aeap008Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u18ah02aDetection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u18ah02bDetection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u18ah03Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u18ancu02Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by u18ancu03Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by ucmp4Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H 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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by userv1675Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by userv1677Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by userv1735Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by userv1736Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by userv1747Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by userv1759Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by userv1762Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by userv1799Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by userv1876Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by wserv11Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by wserv12Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by wserv1Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by wserv3Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by wserv5Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by wserv7Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by wserv8Detection.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. 
hnFlaggedObs 
[nspid]Variability 
WSA NonSurvey 
Number of detections in H band flagged as potentially spurious by wserv9Detection.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. 
hnGoodObs 
[nspid]Variability 
WSA NonSurvey 
Number of good detections in H 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. 
hNgt3sig 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
Number of good detections in Hband that are more than 3 sigma deviations (hAperMagN < (hMeanMag3*hMagRms) 
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. 
hNgt3sig 
[nspid]Variability 
WSA NonSurvey 
Number of good detections in Hband 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. 
hnMissingObs 
[nspid]Variability 
WSA NonSurvey 
Number of H 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. 
hnNegFlagObs 
[nspid]CompMapVariability, [nspid]QsoMapVariability 
WSA NonSurvey 
Number of flagged negative measurements in H band by wserv1000MapRemeasurement.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. 
hnNegObs 
[nspid]CompMapVariability, [nspid]QsoMapVariability 
WSA NonSurvey 
Number of unflagged negative measurements H 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. 
hnPosFlagObs 
[nspid]CompMapVariability, [nspid]QsoMapVariability 
WSA NonSurvey 
Number of flagged positive measurements in H band by wserv1000MapRemeasurement.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. 
hnPosObs 
[nspid]CompMapVariability, [nspid]QsoMapVariability 
WSA NonSurvey 
Number of unflagged positive measurements in H 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. 
hourAngle 
[nspid]Multiframe 
WSA NonSurvey 
Hour angle {image primary HDU keyword: HABASE} 
real 
4 
degrees 
0.9999995e9 

hourAngle 
[nspid]SatelliteDetection 
WSA NonSurvey 
Local Hour angle (hours W of meridean) 
float 
8 
hours 


hPA 
[nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]Source, [nspid]SynopticSource, [nspid]UdsSource, [nspid]YJHKsource, [nspid]ZYJHKsource 
WSA NonSurvey 
ellipse fit celestial orientation in H 
real 
4 
Degrees 
0.9999995e9 
POS_POSANG 
hPetroMag 
[nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]Source, [nspid]UdsSource, [nspid]YJHKsource, [nspid]ZYJHKsource 
WSA NonSurvey 
Extended source H mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
hPetroMagErr 
[nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]Source, [nspid]UdsSource, [nspid]YJHKsource, [nspid]ZYJHKsource 
WSA NonSurvey 
Error in extended source H mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
ERROR 
hppErrBits 
[nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]Source, [nspid]UdsSource, [nspid]YJHKsource, [nspid]ZYJHKsource 
WSA NonSurvey 
additional WFAU postprocessing error bits in H 
int 
4 

0 
CODE_MISC 
hppErrBits 
[nspid]Source, [nspid]SynopticSource 
WSA NonSurvey 
additional WFAU postprocessing error bits in H 
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. 
hprobVar 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
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. 
hPsfMag 
[nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]Source, [nspid]YJHKsource, [nspid]ZYJHKsource 
WSA NonSurvey 
Point source profilefitted H mag 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
hPsfMag 
[nspid]Source, [nspid]UdsSource 
WSA NonSurvey 
Not available in SE output 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
hPsfMagErr 
[nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]Source, [nspid]YJHKsource, [nspid]ZYJHKsource 
WSA NonSurvey 
Error in point source profilefitted H mag 
real 
4 
mag 
0.9999995e9 
ERROR 
hPsfMagErr 
[nspid]Source, [nspid]UdsSource 
WSA NonSurvey 
Not available in SE output 
real 
4 
mag 
0.9999995e9 
ERROR 
hSeqNum 
[nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]Source, [nspid]SynopticSource, [nspid]UdsSource, [nspid]YJHKsource, [nspid]ZYJHKsource 
WSA NonSurvey 
the running number of the H detection 
int 
4 

99999999 
ID_NUMBER 
hSerMag2D 
[nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]Source, [nspid]YJHKsource, [nspid]ZYJHKsource 
WSA NonSurvey 
Extended source H mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
hSerMag2D 
[nspid]Source, [nspid]UdsSource 
WSA NonSurvey 
Not available in SE output 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
hSerMag2DErr 
[nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]Source, [nspid]YJHKsource, [nspid]ZYJHKsource 
WSA NonSurvey 
Error in extended source H mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
ERROR 
hSerMag2DErr 
[nspid]Source, [nspid]UdsSource 
WSA NonSurvey 
Not available in SE output 
real 
4 
mag 
0.9999995e9 
ERROR 
hskewness 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
Skewness in H 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. 
htmID 
[nspid]CurrentAstrometry, [nspid]PreviousAstrometry 
WSA NonSurvey 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates of device centre 
bigint 
8 

99999999 
pos.eq 
htmID 
[nspid]Detection, [nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKmergeLog, [nspid]JHKsource, [nspid]JKmergeLog, [nspid]JKsource, [nspid]LasPointSource, [nspid]MergeLog, [nspid]PointSource, [nspid]Source, [nspid]SynopticMergeLog, [nspid]SynopticSource, [nspid]UKIDSSDetection, [nspid]UdsSource, [nspid]YJHKmergeLog, [nspid]YJHKsource, [nspid]ZYJHKmergeLog, [nspid]ZYJHKsource 
WSA NonSurvey 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


POS_GENERAL 
htmID 
[nspid]MapRemeasAver, [nspid]MapRemeasurement 
WSA NonSurvey 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


pos 
htotalPeriod 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
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. 
humidity 
[nspid]Multiframe 
WSA NonSurvey 
Relative Humidity {image primary HDU keyword: HUMIDITY} 
real 
4 

0.9999995e9 
meta.note;obs 
hVarClass 
[nspid]CompMapVariability, [nspid]QsoMapVariability, [nspid]Variability 
WSA NonSurvey 
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. 
hXi 
[nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]UdsSource, [nspid]YJHKsource, [nspid]ZYJHKsource 
WSA NonSurvey 
Offset of H detection from master position (+east/west) 
real 
4 
arcsec 
0.9999995e9 
POS_EQ_RA_OFF 
hXi 
[nspid]Source, [nspid]SynopticSource 
WSA NonSurvey 
Offset of H 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. 
hz10cd 
[nspid]Multiframe 
WSA NonSurvey 
Trefoil: HZ10CD {image primary HDU keyword: HZ10CD} 
real 
4 

0.9999995e9 

hz10ch 
[nspid]Multiframe 
WSA NonSurvey 
Trefoil: HZ10CH {image primary HDU keyword: HZ10CH} 
real 
4 

0.9999995e9 

hz10sd 
[nspid]Multiframe 
WSA NonSurvey 
Trefoil: HZ10SD {image primary HDU keyword: HZ10SD} 
real 
4 

0.9999995e9 

hz10sh 
[nspid]Multiframe 
WSA NonSurvey 
Trefoil: HZ10SH {image primary HDU keyword: HZ10SH} 
real 
4 

0.9999995e9 

hz5cd 
[nspid]Multiframe 
WSA NonSurvey 
Astigmatism: HZ5CD {image primary HDU keyword: HZ5CD} 
real 
4 

0.9999995e9 

hz5ch 
[nspid]Multiframe 
WSA NonSurvey 
Astigmatism: HZ5CH {image primary HDU keyword: HZ5CH} 
real 
4 

0.9999995e9 

hz5sd 
[nspid]Multiframe 
WSA NonSurvey 
Astigmatism: HZ5SD {image primary HDU keyword: HZ5SD} 
real 
4 

0.9999995e9 

hz5sh 
[nspid]Multiframe 
WSA NonSurvey 
Astigmatism: HZ5SH {image primary HDU keyword: HZ5SH} 
real 
4 

0.9999995e9 

hz6cd 
[nspid]Multiframe 
WSA NonSurvey 
Astigmatism: HZ6CD {image primary HDU keyword: HZ6CD} 
real 
4 

0.9999995e9 

hz6ch 
[nspid]Multiframe 
WSA NonSurvey 
Astigmatism: HZ6CH {image primary HDU keyword: HZ6CH} 
real 
4 

0.9999995e9 

hz6sd 
[nspid]Multiframe 
WSA NonSurvey 
Astigmatism: HZ6SD {image primary HDU keyword: HZ6SD} 
real 
4 

0.9999995e9 

hz6sh 
[nspid]Multiframe 
WSA NonSurvey 
Astigmatism: HZ6SH {image primary HDU keyword: HZ6SH} 
real 
4 

0.9999995e9 

hz9cd 
[nspid]Multiframe 
WSA NonSurvey 
Trefoil: HZ9CD {image primary HDU keyword: HZ9CD} 
real 
4 

0.9999995e9 

hz9ch 
[nspid]Multiframe 
WSA NonSurvey 
Trefoil: HZ9CH {image primary HDU keyword: HZ9CH} 
real 
4 

0.9999995e9 

hz9sd 
[nspid]Multiframe 
WSA NonSurvey 
Trefoil: HZ9SD {image primary HDU keyword: HZ9SD} 
real 
4 

0.9999995e9 

hz9sh 
[nspid]Multiframe 
WSA NonSurvey 
Trefoil: HZ9SH {image primary HDU keyword: HZ9SH} 
real 
4 

0.9999995e9 
