WSA Browser

Glossary of WSA NonSurvey attributes (UKIDSSDR10)

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

A B C D E F G H I J K L M
N O P Q R S T U V W X Y Z

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) stellarness-of-profile 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 post-processing software based on testing the areal profiles aprof2-8 (these are set by CASU to -1 for deblended components, or positive values for non-deblended detections). We encode this in an information bit of ppErrBits for convenience when querying the merged source tables.

h2_1Ell [nspid]Source WSA NonSurvey 1-b/a, where a/b=semi-major/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 non-survey 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_1-H2_1 (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

h2_1mh2_1ExtErr [nspid]Source WSA NonSurvey Error on extended source colour H2_1-H2_1 real 4 mag -0.9999995e9 ERROR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

h2_1mh2_1Pnt [nspid]Source WSA NonSurvey Point source colour H2_1-H2_1 (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

h2_1mh2_1PntErr [nspid]Source WSA NonSurvey Error on point source colour H2_1-H2_1 real 4 mag -0.9999995e9 ERROR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

h2_1PA [nspid]Source WSA NonSurvey ellipse fit celestial orientation in H2_1 real 4 Degrees -0.9999995e9 POS_POS-ANG

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 post-processing error bits in H2_1 int 4 0 CODE_MISC

Post-processing 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 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

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 profile-fitted H2_1 mag real 4 mag -0.9999995e9 PHOT_MAG

h2_1PsfMagErr [nspid]Source WSA NonSurvey Error in point source profile-fitted 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 (profile-fitted) real 4 mag -0.9999995e9 PHOT_MAG

h2_1SerMag2DErr [nspid]Source WSA NonSurvey Error in extended source H2_1 mag (profile-fitted) 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 non-survey 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) stellarness-of-profile 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 post-processing software based on testing the areal profiles aprof2-8 (these are set by CASU to -1 for deblended components, or positive values for non-deblended detections). We encode this in an information bit of ppErrBits for convenience when querying the merged source tables.

h2_2Ell [nspid]Source WSA NonSurvey 1-b/a, where a/b=semi-major/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 non-survey 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_2-H2_2 (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

h2_2mh2_2ExtErr [nspid]Source WSA NonSurvey Error on extended source colour H2_2-H2_2 real 4 mag -0.9999995e9 ERROR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

h2_2mh2_2Pnt [nspid]Source WSA NonSurvey Point source colour H2_2-H2_2 (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

h2_2mh2_2PntErr [nspid]Source WSA NonSurvey Error on point source colour H2_2-H2_2 real 4 mag -0.9999995e9 ERROR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

h2_2PA [nspid]Source WSA NonSurvey ellipse fit celestial orientation in H2_2 real 4 Degrees -0.9999995e9 POS_POS-ANG

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 post-processing error bits in H2_2 int 4 0 CODE_MISC

Post-processing 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 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

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 profile-fitted H2_2 mag real 4 mag -0.9999995e9 PHOT_MAG

h2_2PsfMagErr [nspid]Source WSA NonSurvey Error in point source profile-fitted 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 (profile-fitted) real 4 mag -0.9999995e9 PHOT_MAG

h2_2SerMag2DErr [nspid]Source WSA NonSurvey Error in extended source H2_2 mag (profile-fitted) 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 non-survey 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, [nspid]Source WSA NonSurvey Extended source H2 aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

h2AperMag1 [nspid]SynopticSource WSA NonSurvey Extended source H2 aperture corrected mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

h2AperMag1Err [nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]Source WSA NonSurvey Error in extended 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 (0.7 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, [nspid]SynopticSource WSA NonSurvey Default point/extended 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

h2AperMag3Err [nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [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

h2AperMag3Err [nspid]Source WSA NonSurvey Error in default point source H2 mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

h2AperMag4 [nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]Source, [nspid]SynopticSource WSA NonSurvey Extended source H2 aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

h2AperMag4 [nspid]Source WSA NonSurvey Point 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, [nspid]SynopticSource WSA NonSurvey Error in extended source H2 mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

h2AperMag4Err [nspid]Source WSA NonSurvey Error in point 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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

h2aStratAst [nspid]VarFrameSetInfo WSA NonSurvey Parameter, c0 from Ferreira-Lopes & 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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

h2aStratPht [nspid]VarFrameSetInfo WSA NonSurvey Parameter, c0 from Ferreira-Lopes & 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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

h2bestAper [nspid]Variability WSA NonSurvey Best aperture (1-6) for photometric statistics in the H2 band int 4 -9999

Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)

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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

h2bStratAst [nspid]VarFrameSetInfo WSA NonSurvey Parameter, c1 from Ferreira-Lopes & 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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

h2bStratPht [nspid]VarFrameSetInfo WSA NonSurvey Parameter, c1 from Ferreira-Lopes & 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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared 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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

h2chiSqpd [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 chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

h2Class [nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]Source, [nspid]SourceRemeasurement, [nspid]SynopticSource WSA NonSurvey discrete image classification flag in H2 smallint 2 -9999 CLASS_MISC

h2ClassStat [nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]Source WSA NonSurvey S-Extractor classification statistic in H2 real 4 -0.9999995e9 STAT_PROP

h2ClassStat [nspid]Source, [nspid]SourceRemeasurement, [nspid]SynopticSource WSA NonSurvey N(0,1) stellarness-of-profile 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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

h2cStratAst [nspid]VarFrameSetInfo WSA NonSurvey Parameter, c2 from Ferreira-Lopes & 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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

h2cStratPht [nspid]VarFrameSetInfo WSA NonSurvey Parameter, c2 from Ferreira-Lopes & 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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

h2Deblend [nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]Source, [nspid]SourceRemeasurement, [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 post-processing software based on testing the areal profiles aprof2-8 (these are set by CASU to -1 for deblended components, or positive values for non-deblended 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 Ferreira-Lopes & 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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

h2dStratPht [nspid]VarFrameSetInfo WSA NonSurvey Parameter, c0 from Ferreira-Lopes & 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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

h2Ell [nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]Source, [nspid]SourceRemeasurement, [nspid]SynopticSource WSA NonSurvey 1-b/a, where a/b=semi-major/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, [nspid]SourceRemeasurement WSA NonSurvey processing warning/error bitwise flags in H2 int 4 -99999999 CODE_MISC

h2ErrBits [nspid]Source WSA NonSurvey processing warning/error bitwise flags in H2 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

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 non-survey 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]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]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 chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

h2Gausig [nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]Source, [nspid]SourceRemeasurement, [nspid]SynopticSource WSA NonSurvey RMS of axes of ellipse fit in H2 real 4 pixels -0.9999995e9 MORPH_PARAM

h2HallMag [nspid]Source WSA NonSurvey Total point source H2 mag real 4 mag -0.9999995e9 PHOT_MAG

h2HallMagErr [nspid]Source WSA NonSurvey Error in total point source H2 mag real 4 mag -0.9999995e9 ERROR

h2IntRms [nspid]Variability WSA NonSurvey Intrinsic rms 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 chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

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]VarFrameSetInfo WSA NonSurvey Use a default model for the photometric noise in H2 band. tinyint 1 0

h2Mag [nspid]SourceRemeasurement WSA NonSurvey H2 mag (as appropriate for this merged source) real 4 mag -0.9999995e9 PHOT_MAG

h2MagErr [nspid]SourceRemeasurement WSA NonSurvey Error in H2 mag real 4 mag -0.9999995e9 ERROR

h2MagMAD [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 chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

h2MagRms [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 chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

h2maxCadence [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]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 chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

h2meanMag [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 chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

h2medCadence [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]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 chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

h2mfID [nspid]JHKmergeLog, [nspid]MergeLog, [nspid]SynopticMergeLog WSA NonSurvey the UID of the relevant H2 multiframe bigint 8 ID_FRAME

h2minCadence [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]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 chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

h2mk_1 [nspid]SourceRemeasurement WSA NonSurvey Default colour H2-K (using appropriate mags) real 4 mag PHOT_COLOR

h2mk_1Err [nspid]SourceRemeasurement WSA NonSurvey Error on colour H2-K real 4 mag ERROR

h2mk_1Pnt [nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource WSA NonSurvey Point source colour H2-K (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

h2mk_1Pnt [nspid]Source WSA NonSurvey Point source colour H2-K (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

h2mk_1PntErr [nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource WSA NonSurvey Error on point source colour H2-K real 4 mag -0.9999995e9 ERROR

h2mk_1PntErr [nspid]Source WSA NonSurvey Error on point source colour H2-K real 4 mag -0.9999995e9 ERROR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

h2mkExt [nspid]Source WSA NonSurvey Extended source colour H2-K (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

h2mkExtErr [nspid]Source WSA NonSurvey Error on extended source colour H2-K real 4 mag -0.9999995e9 ERROR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

h2mkPnt [nspid]Source, [nspid]SynopticSource WSA NonSurvey Point source colour H2-K (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

h2mkPntErr [nspid]Source, [nspid]SynopticSource WSA NonSurvey Error on point source colour H2-K real 4 mag -0.9999995e9 ERROR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

h2ndof [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 chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared 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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

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 u06ah13Detection.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 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]Variability WSA NonSurvey Number of good detections in H2-band that are more than 3 sigma deviations smallint 2 -9999

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

h2Ngt3sig [nspid]Variability WSA NonSurvey Number of good detections in H2-band that are more than 3 sigma deviations (h2AperMagN < (h2MeanMag-3*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 chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

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.

h2ObjID [nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource WSA NonSurvey DEPRECATED (do not use) bigint 8 -99999999 ID_NUMBER

h2ObjID [nspid]Source, [nspid]SourceRemeasurement WSA NonSurvey DEPRECATED (do not use) bigint 8 -99999999 ID_NUMBER

This attribute is included in source tables for historical reasons, but it's use is not recommended unless you really know what you are doing. In general, if you need to look up detection table attributes for a source in a given passband that are not in the source table, you should make an SQL join between source, mergelog and detection using the primary key attribute frameSetID and combination multiframeID, extNum, seqNum to associate related rows between the three tables. See the Q&A example SQL for more information.

h2PA [nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]Source, [nspid]SourceRemeasurement, [nspid]SynopticSource WSA NonSurvey ellipse fit celestial orientation in H2 real 4 Degrees -0.9999995e9 POS_POS-ANG

h2PetroMag [nspid]Source WSA NonSurvey Extended source H2 mag (Petrosian) real 4 mag -0.9999995e9 PHOT_MAG

h2PetroMagErr [nspid]Source WSA NonSurvey Error in extended source H2 mag (Petrosian) real 4 mag -0.9999995e9 ERROR

h2ppErrBits [nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]Source, [nspid]SourceRemeasurement WSA NonSurvey additional WFAU post-processing error bits in H2 int 4 0 CODE_MISC

h2ppErrBits [nspid]Source, [nspid]SynopticSource WSA NonSurvey additional WFAU post-processing error bits in H2 int 4 0 CODE_MISC

Post-processing 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 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

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]Variability WSA NonSurvey Probability of variable from chi-square (and other data) real 4 -0.9999995e9

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

h2PsfMag [nspid]Source WSA NonSurvey Point source profile-fitted H2 mag real 4 mag -0.9999995e9 PHOT_MAG

h2PsfMagErr [nspid]Source WSA NonSurvey Error in point source profile-fitted 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

h2SeqNum [nspid]SourceRemeasurement WSA NonSurvey the running number of the H2 remeasurement int 4 -99999999 ID_NUMBER

h2SerMag2D [nspid]Source WSA NonSurvey Extended source H2 mag (profile-fitted) real 4 mag -0.9999995e9 PHOT_MAG

h2SerMag2DErr [nspid]Source WSA NonSurvey Error in extended source H2 mag (profile-fitted) real 4 mag -0.9999995e9 ERROR

h2skewness [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 chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

h2totalPeriod [nspid]Variability WSA NonSurvey total period of observations (last obs-first obs) real 4 days -0.9999995e9

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

h2VarClass [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 chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

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 non-survey 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 Half-light 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, [nspid]ListRemeasurement 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, [nspid]ListRemeasurement 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]ListRemeasurement, [nspid]UKIDSSDetection WSA NonSurvey Calibrated magnitude within circular aperture r_hall real 4 mag PHOT_INT-MAG

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

hallMagErr [nspid]Detection, [nspid]ListRemeasurement, [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, [nspid]ListRemeasurement 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, [nspid]Source, [nspid]SynopticSource WSA NonSurvey Extended source H aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

hAperMag1 [nspid]SynopticSource WSA NonSurvey Extended source H aperture corrected mag (0.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

hAperMag1Err [nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]Source, [nspid]SynopticSource WSA NonSurvey Error in extended 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 (0.7 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]SynopticSource, [nspid]YJHKsource, [nspid]ZYJHKsource WSA NonSurvey Default point/extended 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 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/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 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]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]SynopticSource, [nspid]UdsSource, [nspid]YJHKsource, [nspid]ZYJHKsource WSA NonSurvey Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

hAperMag3Err [nspid]Source WSA NonSurvey Error in default point 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]SynopticSource, [nspid]YJHKsource, [nspid]ZYJHKsource WSA NonSurvey Extended source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

hAperMag4 [nspid]Source WSA NonSurvey Point 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]SynopticSource, [nspid]UdsSource, [nspid]YJHKsource, [nspid]ZYJHKsource WSA NonSurvey Error in extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

hAperMag4Err [nspid]Source WSA NonSurvey Error in point 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 Extended source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

hAperMag6 [nspid]Source WSA NonSurvey Point 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]UdsSource, [nspid]YJHKsource, [nspid]ZYJHKsource WSA NonSurvey Error in extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

hAperMag6Err [nspid]Source WSA NonSurvey Error in point 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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

haStratAst [nspid]VarFrameSetInfo WSA NonSurvey Parameter, c0 from Ferreira-Lopes & 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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

haStratPht [nspid]VarFrameSetInfo WSA NonSurvey Parameter, c0 from Ferreira-Lopes & 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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hbestAper [nspid]Variability WSA NonSurvey Best aperture (1-6) for photometric statistics in the H band int 4 -9999

Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449)

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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hbStratAst [nspid]VarFrameSetInfo WSA NonSurvey Parameter, c1 from Ferreira-Lopes & 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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hbStratPht [nspid]VarFrameSetInfo WSA NonSurvey Parameter, c1 from Ferreira-Lopes & 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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared 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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hchiSqpd [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 chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hClass [nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]Source, [nspid]SourceRemeasurement, [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]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]Source, [nspid]SourceRemeasurement, [nspid]SynopticSource, [nspid]YJHKsource, [nspid]ZYJHKsource WSA NonSurvey N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 STAT_PROP

hClassStat [nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]Source, [nspid]UdsSource WSA NonSurvey S-Extractor 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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hcStratAst [nspid]VarFrameSetInfo WSA NonSurvey Parameter, c2 from Ferreira-Lopes & 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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hcStratPht [nspid]VarFrameSetInfo WSA NonSurvey Parameter, c2 from Ferreira-Lopes & 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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

hDeblend [nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]Source, [nspid]SourceRemeasurement, [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 post-processing software based on testing the areal profiles aprof2-8 (these are set by CASU to -1 for deblended components, or positive values for non-deblended 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 Ferreira-Lopes & 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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

hdStratPht [nspid]VarFrameSetInfo WSA NonSurvey Parameter, c0 from Ferreira-Lopes & 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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

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 camera-specific 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]SourceRemeasurement, [nspid]SynopticSource, [nspid]UdsSource, [nspid]YJHKsource, [nspid]ZYJHKsource WSA NonSurvey 1-b/a, where a/b=semi-major/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]SourceRemeasurement, [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 non-survey 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]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]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 chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hGausig [nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]Source, [nspid]SourceRemeasurement, [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]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]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]Variability WSA NonSurvey Intrinsic rms 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 chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

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]VarFrameSetInfo WSA NonSurvey Use a default model for the photometric noise in H band. tinyint 1 0

hkiWS [nspid]Variability WSA NonSurvey Welch-Stetson 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 Welch-Stetson 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 half-light radius computed from curve of growth assuming petrosian flux is 90% of total (CASU: default) real 4 arcsec -0.9999995e9 phys.angSize

hlCircRadErrAs [nspid]MapRemeasurement WSA NonSurvey Error in hlCircRadAs (CASU: default) real 4 arcsec -0.9999995e9 phys.angSize

hlCorSMjRadAs [nspid]MapRemeasurement WSA NonSurvey Seeing corrected Half-light semi-major axis (CASU: default) real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlCorSMnRadAs [nspid]MapRemeasurement WSA NonSurvey Seeing corrected Half-light semi-minor axis (CASU: default) real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hlGeoRadAs [nspid]MapRemeasurement WSA NonSurvey Geometric half-light radius (CASU: default) real 4 arcsec -0.9999995e9 phys.angSize

hlSMjRadAs [nspid]MapRemeasurement WSA NonSurvey Half-light semi-major axis (CASU: default) real 4 arcsec -0.9999995e9 phys.angSize.smajAxis

hlSMnRadAs [nspid]MapRemeasurement WSA NonSurvey Half-light semi-minor axis (CASU: default) real 4 arcsec -0.9999995e9 phys.angSize.sminAxis

hMag [nspid]FSstars WSA NonSurvey H band total magnitude on the MKO(UFTI) system real 4 mag PHOT_INT-MAG

hMag [nspid]SourceRemeasurement WSA NonSurvey H mag (as appropriate for this merged source) real 4 mag -0.9999995e9 PHOT_MAG

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

hMagErr [nspid]SourceRemeasurement WSA NonSurvey Error in H mag real 4 mag -0.9999995e9 ERROR

hMagMAD [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 chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hMagRms [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 chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hmaxCadence [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]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 chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hmeanMag [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 chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hmedCadence [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]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 chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

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]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]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 chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

hmk [nspid]SourceRemeasurement WSA NonSurvey Default colour H-K (using appropriate mags) real 4 mag PHOT_COLOR

hmk_1 [nspid]SourceRemeasurement WSA NonSurvey Default colour H-K (using appropriate mags) real 4 mag PHOT_COLOR

hmk_1Err [nspid]SourceRemeasurement WSA NonSurvey Error on colour H-K real 4 mag ERROR

hmk_1Ext [nspid]GcsPointSource, [nspid]PointSource, [nspid]ZYJHKsource WSA NonSurvey Extended source colour H-K (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

hmk_1Ext [nspid]Source WSA NonSurvey Extended source colour H-K (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmk_1ExtErr [nspid]GcsPointSource, [nspid]PointSource, [nspid]ZYJHKsource WSA NonSurvey Error on extended source colour H-K real 4 mag -0.9999995e9 ERROR

hmk_1ExtErr [nspid]Source WSA NonSurvey Error on extended source colour H-K real 4 mag -0.9999995e9 ERROR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmk_1Pnt [nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]ZYJHKsource WSA NonSurvey Point source colour H-K (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

hmk_1Pnt [nspid]Source WSA NonSurvey Point source colour H-K (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmk_1PntErr [nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]PointSource, [nspid]ZYJHKsource WSA NonSurvey Error on point source colour H-K real 4 mag -0.9999995e9 ERROR

hmk_1PntErr [nspid]Source WSA NonSurvey Error on point source colour H-K real 4 mag -0.9999995e9 ERROR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmkErr [nspid]SourceRemeasurement WSA NonSurvey Error on colour H-K real 4 mag ERROR

hmkExt [nspid]DxsSource, [nspid]ExtendedSource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]UdsSource, [nspid]YJHKsource WSA NonSurvey Extended source colour H-K (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

hmkExt [nspid]Source WSA NonSurvey Extended source colour H-K (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmkExtErr [nspid]DxsSource, [nspid]ExtendedSource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]UdsSource, [nspid]YJHKsource WSA NonSurvey Error on extended source colour H-K real 4 mag -0.9999995e9 ERROR

hmkExtErr [nspid]Source WSA NonSurvey Error on extended source colour H-K real 4 mag -0.9999995e9 ERROR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmkPnt [nspid]DxsSource, [nspid]ExtendedSource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]UdsSource, [nspid]YJHKsource WSA NonSurvey Point source colour H-K (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

hmkPnt [nspid]Source, [nspid]SynopticSource WSA NonSurvey Point source colour H-K (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hmkPntErr [nspid]DxsSource, [nspid]ExtendedSource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]UdsSource, [nspid]YJHKsource WSA NonSurvey Error on point source colour H-K real 4 mag -0.9999995e9 ERROR

hmkPntErr [nspid]Source, [nspid]SynopticSource WSA NonSurvey Error on point source colour H-K real 4 mag -0.9999995e9 ERROR

Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits.

hndof [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 chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared 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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated.

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 median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236.

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 u06ah13Detection.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 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 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 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]Variability WSA NonSurvey Number of good detections in H-band that are more than 3 sigma deviations smallint 2 -9999

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

hNgt3sig [nspid]Variability WSA NonSurvey Number of good detections in H-band that are more than 3 sigma deviations (hAperMagN < (hMeanMag-3*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 chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

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.

hObjID [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]GpsPointSource, [nspid]JHKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]YJHKsource, [nspid]ZYJHKsource WSA NonSurvey DEPRECATED (do not use) bigint 8 -99999999 ID_NUMBER

hObjID [nspid]Source, [nspid]SourceRemeasurement WSA NonSurvey DEPRECATED (do not use) bigint 8 -99999999 ID_NUMBER

This attribute is included in source tables for historical reasons, but it's use is not recommended unless you really know what you are doing. In general, if you need to look up detection table attributes for a source in a given passband that are not in the source table, you should make an SQL join between source, mergelog and detection using the primary key attribute frameSetID and combination multiframeID, extNum, seqNum to associate related rows between the three tables. See the Q&A example SQL for more information.

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]SourceRemeasurement, [nspid]SynopticSource, [nspid]UdsSource, [nspid]YJHKsource, [nspid]ZYJHKsource WSA NonSurvey ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 POS_POS-ANG

hPetroMag [nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [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]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]SourceRemeasurement, [nspid]UdsSource, [nspid]YJHKsource, [nspid]ZYJHKsource WSA NonSurvey additional WFAU post-processing error bits in H int 4 0 CODE_MISC

hppErrBits [nspid]Source, [nspid]SynopticSource WSA NonSurvey additional WFAU post-processing error bits in H int 4 0 CODE_MISC

Post-processing 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 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

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]Variability WSA NonSurvey Probability of variable from chi-square (and other data) real 4 -0.9999995e9

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

hPsfMag [nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]Source, [nspid]YJHKsource, [nspid]ZYJHKsource WSA NonSurvey Point source profile-fitted 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]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]Source, [nspid]YJHKsource, [nspid]ZYJHKsource WSA NonSurvey Error in point source profile-fitted 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

hSeqNum [nspid]SourceRemeasurement WSA NonSurvey the running number of the H remeasurement int 4 -99999999 ID_NUMBER

hSerMag2D [nspid]DxsSource, [nspid]ExtendedSource, [nspid]GcsPointSource, [nspid]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]Source, [nspid]YJHKsource, [nspid]ZYJHKsource WSA NonSurvey Extended source H mag (profile-fitted) 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]JKsource, [nspid]LasPointSource, [nspid]PointSource, [nspid]Source, [nspid]YJHKsource, [nspid]ZYJHKsource WSA NonSurvey Error in extended source H mag (profile-fitted) 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]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 chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

htmID [nspid]CurrentAstrometry, [nspid]PreviousAstrometry WSA NonSurvey Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates 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]ListRemeasurement, [nspid]MergeLog, [nspid]PointSource, [nspid]Source, [nspid]SourceRemeasurement, [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 co-ordinates bigint 8 POS_GENERAL

htmID [nspid]MapRemeasAver, [nspid]MapRemeasurement WSA NonSurvey Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 pos

htotalPeriod [nspid]Variability WSA NonSurvey total period of observations (last obs-first obs) real 4 days -0.9999995e9

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

humidity [nspid]Multiframe WSA NonSurvey Relative Humidity {image primary HDU keyword: HUMIDITY} real 4 -0.9999995e9 meta.note;obs

hVarClass [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 chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

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 non-survey 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

WFAU, Institute for Astronomy,
Royal Observatory, Blackford Hill
Edinburgh, EH9 3HJ, UK

wsa-support@roe.ac.uk
29/06/2018