WSA Browser

Glossary of WSA attributes

This Glossary alphabetically lists all attributes used in the UKIDSSDR11 database(s) held in the WSA. If you would like to have more information about the schema tables please use the UKIDSSDR11 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

J

Name Schema Table Database Description Type Length Unit Default Value Unified Content Descriptor

j_1AperMag3 lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource WSA Default point source J_1 aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

j_1AperMag3 lasSource WSA Default point source J_1 aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

j_1AperMag3Err lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA Error in default point source J_1 mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

j_1AperMag4 lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA Point source J_1 aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

j_1AperMag4Err lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA Error in point source J_1 mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

j_1AperMag6 lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA Point source J_1 aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

j_1AperMag6Err lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA Error in point source J_1 mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

j_1Class lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA discrete image classification flag in J_1 smallint 2 -9999 CLASS_MISC

j_1ClassStat lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA N(0,1) stellarness-of-profile statistic in J_1 real 4 -0.9999995e9 STAT_PROP

j_1Deblend lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource WSA placeholder flag indicating parent/child relation in J_1 int 4 -99999999 CODE_MISC

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

This CASU pipeline processing source extraction flag is a placeholder only, and is always set to zero in all passbands in the merged source lists. If you need to know when a particular image detection is a component of a deblend or not, test bit 4 of attribute ppErrBits (see corresponding glossary entry) which is set by WFAU's 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.

j_1Ell lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA 1-b/a, where a/b=semi-major/minor axes in J_1 real 4 -0.9999995e9 PHYS_ELLIPTICITY

j_1eNum lasMergeLog, lasYJHKmergeLog WSA the extension number of this J_1 frame tinyint 1 NUMBER

j_1ErrBits lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource WSA processing warning/error bitwise flags in J_1 int 4 -99999999 CODE_MISC

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

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

j_1Eta lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource WSA Offset of J_1 detection from master position (+north/-south) real 4 arcsec -0.9999995e9 POS_EQ_DEC_OFF

j_1Eta lasSource WSA Offset of J_1 detection from master position (+north/-south) real 4 arcsec -0.9999995e9 POS_EQ_DEC_OFF

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 2.0 (UKIDSS LAS and GPS; UHS; also 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.

j_1Gausig lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA RMS of axes of ellipse fit in J_1 real 4 pixels -0.9999995e9 MORPH_PARAM

j_1HallMag lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA Total point source J_1 mag real 4 mag -0.9999995e9 PHOT_MAG

j_1HallMagErr lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA Error in total point source J_1 mag real 4 mag -0.9999995e9 ERROR

j_1mfID lasMergeLog, lasYJHKmergeLog WSA the UID of the relevant J_1 multiframe bigint 8 ID_FRAME

j_1mhExt lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource WSA Extended source colour J_1-H (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

j_1mhExt lasSource WSA Extended source colour J_1-H (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.

j_1mhExtErr lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource WSA Error on extended source colour J_1-H real 4 mag -0.9999995e9 ERROR

j_1mhExtErr lasSource WSA Error on extended source colour J_1-H 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.

j_1mhPnt lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource WSA Point source colour J_1-H (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

j_1mhPnt lasSource WSA Point source colour J_1-H (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.

j_1mhPntErr lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource WSA Error on point source colour J_1-H real 4 mag -0.9999995e9 ERROR

j_1mhPntErr lasSource WSA Error on point source colour J_1-H 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.

j_1PA lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA ellipse fit celestial orientation in J_1 real 4 Degrees -0.9999995e9 POS_POS-ANG

j_1PetroMag lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA Extended source J_1 mag (Petrosian) real 4 mag -0.9999995e9 PHOT_MAG

j_1PetroMagErr lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA Error in extended source J_1 mag (Petrosian) real 4 mag -0.9999995e9 ERROR

j_1ppErrBits lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource WSA additional WFAU post-processing error bits in J_1 int 4 0 CODE_MISC

j_1ppErrBits lasSource WSA additional WFAU post-processing error bits in J_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.

j_1PsfMag lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA Point source profile-fitted J_1 mag real 4 mag -0.9999995e9 PHOT_MAG

j_1PsfMagErr lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA Error in point source profile-fitted J_1 mag real 4 mag -0.9999995e9 ERROR

j_1SeqNum lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA the running number of the J_1 detection int 4 -99999999 ID_NUMBER

j_1SerMag2D lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA Extended source J_1 mag (profile-fitted) real 4 mag -0.9999995e9 PHOT_MAG

j_1SerMag2DErr lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA Error in extended source J_1 mag (profile-fitted) real 4 mag -0.9999995e9 ERROR

j_1Xi lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource WSA Offset of J_1 detection from master position (+east/-west) real 4 arcsec -0.9999995e9 POS_EQ_RA_OFF

j_1Xi lasSource WSA Offset of J_1 detection from master position (+east/-west) real 4 arcsec -0.9999995e9 POS_EQ_RA_OFF

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 2.0 (UKIDSS LAS and GPS; UHS; also 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.

j_2AperMag3 lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource WSA Default point source J_2 aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

j_2AperMag3 lasSource WSA Default point source J_2 aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

j_2AperMag3Err lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA Error in default point source J_2 mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

j_2AperMag4 lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA Point source J_2 aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

j_2AperMag4Err lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA Error in point source J_2 mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

j_2AperMag6 lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA Point source J_2 aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

j_2AperMag6Err lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA Error in point source J_2 mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

j_2Class lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA discrete image classification flag in J_2 smallint 2 -9999 CLASS_MISC

j_2ClassStat lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA N(0,1) stellarness-of-profile statistic in J_2 real 4 -0.9999995e9 STAT_PROP

j_2Deblend lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource WSA placeholder flag indicating parent/child relation in J_2 int 4 -99999999 CODE_MISC

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

This CASU pipeline processing source extraction flag is a placeholder only, and is always set to zero in all passbands in the merged source lists. If you need to know when a particular image detection is a component of a deblend or not, test bit 4 of attribute ppErrBits (see corresponding glossary entry) which is set by WFAU's 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.

j_2Ell lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA 1-b/a, where a/b=semi-major/minor axes in J_2 real 4 -0.9999995e9 PHYS_ELLIPTICITY

j_2eNum lasMergeLog, lasYJHKmergeLog WSA the extension number of this J_2 frame tinyint 1 NUMBER

j_2ErrBits lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource WSA processing warning/error bitwise flags in J_2 int 4 -99999999 CODE_MISC

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

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

j_2Eta lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource WSA Offset of J_2 detection from master position (+north/-south) real 4 arcsec -0.9999995e9 POS_EQ_DEC_OFF

j_2Eta lasSource WSA Offset of J_2 detection from master position (+north/-south) real 4 arcsec -0.9999995e9 POS_EQ_DEC_OFF

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 2.0 (UKIDSS LAS and GPS; UHS; also 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.

j_2Gausig lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA RMS of axes of ellipse fit in J_2 real 4 pixels -0.9999995e9 MORPH_PARAM

j_2HallMag lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA Total point source J_2 mag real 4 mag -0.9999995e9 PHOT_MAG

j_2HallMagErr lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA Error in total point source J_2 mag real 4 mag -0.9999995e9 ERROR

j_2mfID lasMergeLog, lasYJHKmergeLog WSA the UID of the relevant J_2 multiframe bigint 8 ID_FRAME

j_2mhExt lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource WSA Extended source colour J_2-H (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

j_2mhExt lasSource WSA Extended source colour J_2-H (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.

j_2mhExtErr lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource WSA Error on extended source colour J_2-H real 4 mag -0.9999995e9 ERROR

j_2mhExtErr lasSource WSA Error on extended source colour J_2-H 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.

j_2mhPnt lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource WSA Point source colour J_2-H (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

j_2mhPnt lasSource WSA Point source colour J_2-H (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.

j_2mhPntErr lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource WSA Error on point source colour J_2-H real 4 mag -0.9999995e9 ERROR

j_2mhPntErr lasSource WSA Error on point source colour J_2-H 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.

j_2mrat twomass_scn 2MASS J-band average 2nd image moment ratio. real 4 FIT_PARAM_VALUE

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

j_2PA lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA ellipse fit celestial orientation in J_2 real 4 Degrees -0.9999995e9 POS_POS-ANG

j_2PetroMag lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA Extended source J_2 mag (Petrosian) real 4 mag -0.9999995e9 PHOT_MAG

j_2PetroMagErr lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA Error in extended source J_2 mag (Petrosian) real 4 mag -0.9999995e9 ERROR

j_2ppErrBits lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource WSA additional WFAU post-processing error bits in J_2 int 4 0 CODE_MISC

j_2ppErrBits lasSource WSA additional WFAU post-processing error bits in J_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.

j_2PsfMag lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA Point source profile-fitted J_2 mag real 4 mag -0.9999995e9 PHOT_MAG

j_2PsfMagErr lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA Error in point source profile-fitted J_2 mag real 4 mag -0.9999995e9 ERROR

j_2SeqNum lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA the running number of the J_2 detection int 4 -99999999 ID_NUMBER

j_2SerMag2D lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA Extended source J_2 mag (profile-fitted) real 4 mag -0.9999995e9 PHOT_MAG

j_2SerMag2DErr lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableLasPointSource WSA Error in extended source J_2 mag (profile-fitted) real 4 mag -0.9999995e9 ERROR

j_2Xi lasExtendedSource, lasPointSource, lasYJHKsource, reliableLasPointSource WSA Offset of J_2 detection from master position (+east/-west) real 4 arcsec -0.9999995e9 POS_EQ_RA_OFF

j_2Xi lasSource WSA Offset of J_2 detection from master position (+east/-west) real 4 arcsec -0.9999995e9 POS_EQ_RA_OFF

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 2.0 (UKIDSS LAS and GPS; UHS; also 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.

j_5sig_ba twomass_xsc 2MASS J minor/major axis ratio fit to the 5-sigma isophote. real 4 PHYS_AXIS-RATIO

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

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

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

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

j_bisym_chi twomass_xsc 2MASS J bi-symmetric cross-correlation chi. real 4 FIT_PARAM_VALUE

j_bisym_rat twomass_xsc 2MASS J bi-symmetric flux ratio. real 4 PHOT_FLUX_RATIO

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

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

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

j_cmsig twomass_psc 2MASS Corrected photometric uncertainty for the default J-band magnitude. real 4 mag SPECT_FLUX_VALUE

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

j_m twomass_psc 2MASS Default J-band magnitude real 4 mag SPECT_FLUX_VALUE

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

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

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

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

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

j_m_2mass allwise_sc WISE 2MASS J-band magnitude or magnitude upper limit of the associated 2MASS PSC source. This column is "null" if there is no associated 2MASS PSC source or if the 2MASS PSC J-band magnitude entry is "null". float 8 mag

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

j_m_stdap twomass_psc 2MASS J-band "standard" aperture magnitude. real 4 mag SPECT_FLUX_VALUE

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

j_mnsurfb_eff twomass_xsc 2MASS J mean surface brightness at the half-light radius. real 4 mag PHOT_SB_GENERAL

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

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

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

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

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

j_msig_2mass allwise_sc WISE 2MASS J-band corrected photometric uncertainty of the associated 2MASS PSC source. This column is "null" if there is no associated 2MASS PSC source or if the 2MASS PSC J-band uncertainty entry is "null". float 8 mag

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

j_msig_stdap twomass_psc 2MASS Uncertainty in the J-band standard aperture magnitude. real 4 mag SPECT_FLUX_VALUE

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

j_msigcom twomass_psc 2MASS Combined, or total photometric uncertainty for the default J-band magnitude. real 4 mag SPECT_FLUX_VALUE

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

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

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

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

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

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

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

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

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

j_psfchi twomass_psc 2MASS Reduced chi-squared goodness-of-fit value for the J-band profile-fit photometry made on the 1.3 s "Read_2" exposures. real 4 FIT_PARAM_VALUE

j_psp twomass_scn 2MASS J-band photometric sensitivity paramater (PSP). real 4 INST_SENSITIVITY

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

j_pts_noise twomass_scn 2MASS Base-10 logarithm of the mode of the noise distribution for all point source detections in the scan, where the noise is estimated from the measured J-band photometric errors and is expressed in units of mJy. real 4 INST_NOISE

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

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

j_r_e twomass_xsc 2MASS J Kron elliptical aperture semi-major axis. real 4 arcsec EXTENSION_RAD

j_r_eff twomass_xsc 2MASS J half-light (integrated half-flux point) radius. real 4 arcsec EXTENSION_RAD

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

j_shape_avg twomass_scn 2MASS J-band average seeing shape for scan. real 4 INST_SEEING

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

j_shape_rms twomass_scn 2MASS RMS-error of J-band average seeing shape. real 4 INST_SEEING

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

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

j_snr twomass_psc 2MASS J-band "scan" signal-to-noise ratio. real 4 mag INST_NOISE

j_snr twomass_sixx2_psc 2MASS J band "scan" signal-to-noise ratio real 4

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

j_zp_ap twomass_scn 2MASS Photometric zero-point for J-band aperture photometry. real 4 mag PHOT_ZP

j_zp_ap twomass_sixx2_scn 2MASS J band ap. calibration photometric zero-point for scan real 4 mag

jAperJky3 lasYselJSourceRemeasurement WSA Default point source J aperture corrected (2.0 arcsec aperture diameter) calibrated flux
If in doubt use this flux estimator real 4 jansky -0.9999995e9 phot.flux

jAperJky3Err lasYselJSourceRemeasurement WSA Error in default point/extended source J (2.0 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error

jAperJky4 lasYselJSourceRemeasurement WSA Point source J aperture corrected (2.8 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 phot.flux

jAperJky4Err lasYselJSourceRemeasurement WSA Error in point/extended source J (2.8 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error

jAperJky6 lasYselJSourceRemeasurement WSA Point source J aperture corrected (5.7 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 phot.flux

jAperJky6Err lasYselJSourceRemeasurement WSA Error in point/extended source J (5.7 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error

jAperJkyNoAperCorr3 lasYselJSourceRemeasurement WSA Default extended source J (2.0 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux
If in doubt use this flux estimator real 4 jansky -0.9999995e9 phot.flux

jAperJkyNoAperCorr4 lasYselJSourceRemeasurement WSA Extended source J (2.8 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux real 4 jansky -0.9999995e9 phot.flux

jAperJkyNoAperCorr6 lasYselJSourceRemeasurement WSA Extended source J (5.7 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux real 4 jansky -0.9999995e9 phot.flux

jAperLup3 lasYselJSourceRemeasurement WSA Default point source J aperture corrected (2.0 arcsec aperture diameter) luptitude
If in doubt use this flux estimator real 4 lup -0.9999995e9 phot.lup

jAperLup3Err lasYselJSourceRemeasurement WSA Error in default point/extended source J (2.0 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error

jAperLup4 lasYselJSourceRemeasurement WSA Point source J aperture corrected (2.8 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 phot.lup

jAperLup4Err lasYselJSourceRemeasurement WSA Error in point/extended source J (2.8 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error

jAperLup6 lasYselJSourceRemeasurement WSA Point source J aperture corrected (5.7 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 phot.lup

jAperLup6Err lasYselJSourceRemeasurement WSA Error in point/extended source J (5.7 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error

jAperLupNoAperCorr3 lasYselJSourceRemeasurement WSA Default extended source J (2.0 arcsec aperture diameter, but no aperture correction applied) aperture luptitude
If in doubt use this flux estimator real 4 lup -0.9999995e9 phot.lup

jAperLupNoAperCorr4 lasYselJSourceRemeasurement WSA Extended source J (2.8 arcsec aperture diameter, but no aperture correction applied) aperture luptitude real 4 lup -0.9999995e9 phot.lup

jAperLupNoAperCorr6 lasYselJSourceRemeasurement WSA Extended source J (5.7 arcsec aperture diameter, but no aperture correction applied) aperture luptitude real 4 lup -0.9999995e9 phot.lup

jAperMag1 calSynopticSource WSACalib Extended source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

jAperMag1 gpsJHKsource, gpsPointSource, reliableGpsPointSource WSA Default point source J aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

jAperMag1 gpsSource WSA Default point source J aperture corrected mag (1.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

jAperMag1Err calSynopticSource WSACalib Error in extended source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag1Err gpsJHKsource, gpsPointSource, gpsSource, reliableGpsPointSource WSA Error in point source J mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag2 calSynopticSource WSACalib Extended source J aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

jAperMag2Err calSynopticSource WSACalib Error in extended source J mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag3 calSource WSACalib Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

jAperMag3 calSynopticSource WSACalib Default point/extended source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

jAperMag3 dxsJKsource, gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, lasExtendedSource, lasPointSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource WSA Default point source J aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

jAperMag3 dxsSource, gcsSource, gpsSource, lasSource WSA Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

jAperMag3 lasYselJSourceRemeasurement WSA Default point source J aperture corrected (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMag3 reliableUdsSource WSA Default point/extended source J mag, no aperture correction applied real 4 mag -0.9999995e9 PHOT_MAG

jAperMag3 udsSource WSA Default point/extended source J mag, no aperture correction applied
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

jAperMag3 uhsSource, uhsSourceAll WSAUHS Default point source J aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

jAperMag3Err calSource, calSynopticSource WSACalib Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag3Err dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource WSA Error in default point source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag3Err lasYselJSourceRemeasurement WSA Error in default point/extended source J (2.0 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error

jAperMag3Err reliableUdsSource, udsSource WSA Error in default point/extended source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag3Err uhsSource, uhsSourceAll WSAUHS Error in default point source J mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag4 calSource, calSynopticSource WSACalib Extended source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

jAperMag4 dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource WSA Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

jAperMag4 lasYselJSourceRemeasurement WSA Point source J aperture corrected (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag4 reliableUdsSource, udsSource WSA Extended source J mag, no aperture correction applied real 4 mag -0.9999995e9 PHOT_MAG

jAperMag4 uhsSource, uhsSourceAll WSAUHS Point source J aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

jAperMag4Err calSource, calSynopticSource WSACalib Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag4Err dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource WSA Error in point source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag4Err lasYselJSourceRemeasurement WSA Error in point/extended source J (2.8 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error

jAperMag4Err reliableUdsSource, udsSource WSA Error in extended source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag4Err uhsSource, uhsSourceAll WSAUHS Error in point source J mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag5 calSynopticSource WSACalib Extended source J aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

jAperMag5Err calSynopticSource WSACalib Error in extended source J mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag6 calSource WSACalib Extended source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

jAperMag6 dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableLasPointSource WSA Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

jAperMag6 lasYselJSourceRemeasurement WSA Point source J aperture corrected (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

jAperMag6 reliableUdsSource, udsSource WSA Extended source J mag, no aperture correction applied real 4 mag -0.9999995e9 PHOT_MAG

jAperMag6 uhsSource, uhsSourceAll WSAUHS Point source J aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

jAperMag6Err calSource WSACalib Error in extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag6Err dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableLasPointSource WSA Error in point source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag6Err lasYselJSourceRemeasurement WSA Error in point/extended source J (5.7 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error

jAperMag6Err reliableUdsSource, udsSource WSA Error in extended source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMag6Err uhsSource, uhsSourceAll WSAUHS Error in point source J mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

jAperMagNoAperCorr3 lasYselJSourceRemeasurement WSA Default extended source J (2.0 arcsec aperture diameter, but no aperture correction applied) aperture magnitude
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr4 lasYselJSourceRemeasurement WSA Extended source J (2.8 arcsec aperture diameter, but no aperture correction applied) aperture magnitude real 4 mag -0.9999995e9 phot.mag

jAperMagNoAperCorr6 lasYselJSourceRemeasurement WSA Extended source J (5.7 arcsec aperture diameter, but no aperture correction applied) aperture magnitude real 4 mag -0.9999995e9 phot.mag

jaStratAst calVarFrameSetInfo WSACalib Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9

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

jaStratAst dxsVarFrameSetInfo, lasVarFrameSetInfo, udsVarFrameSetInfo WSA Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9

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

jaStratAst uhsVarFrameSetInfo WSAUHS Strateva parameter, a, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9

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

jaStratPht calVarFrameSetInfo WSACalib Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9

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

jaStratPht dxsVarFrameSetInfo, lasVarFrameSetInfo, udsVarFrameSetInfo WSA Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9

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

jaStratPht uhsVarFrameSetInfo WSAUHS Strateva parameter, a, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9

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

jAverageConf lasYselJSourceRemeasurement WSA average confidence in 2 arcsec diameter default aperture (aper3) J real 4 -0.9999995e9 stat.likelihood;em.IR.NIR

jbestAper calVariability WSACalib Best aperture (1-6) for photometric statistics in the J band int 4 -9999

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

jbestAper dxsVariability, lasVariability, udsVariability WSA Best aperture (1-6) for photometric statistics in the J band int 4 -9999

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

jbestAper uhsVariability WSAUHS Best aperture (1-6) for photometric statistics in the J band int 4 -9999

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

jbStratAst calVarFrameSetInfo WSACalib Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9

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

jbStratAst dxsVarFrameSetInfo, lasVarFrameSetInfo, udsVarFrameSetInfo WSA Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9

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

jbStratAst uhsVarFrameSetInfo WSAUHS Strateva parameter, b, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9

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

jbStratPht calVarFrameSetInfo WSACalib Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9

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

jbStratPht dxsVarFrameSetInfo, lasVarFrameSetInfo, udsVarFrameSetInfo WSA Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9

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

jbStratPht uhsVarFrameSetInfo WSAUHS Strateva parameter, b, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9

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

jchiSqAst calVarFrameSetInfo WSACalib Goodness of fit of Strateva function to astrometric data in J band real 4 -0.9999995e9

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

jchiSqAst dxsVarFrameSetInfo, lasVarFrameSetInfo, udsVarFrameSetInfo WSA Goodness of fit of Strateva function to astrometric data in J band real 4 -0.9999995e9

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

jchiSqAst uhsVarFrameSetInfo WSAUHS Goodness of fit of Strateva function to astrometric data in J band real 4 -0.9999995e9

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

jchiSqpd calVariability WSACalib Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9

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

jchiSqpd dxsVariability, lasVariability, udsVariability WSA Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9

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

jchiSqpd uhsVariability WSAUHS Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 -0.9999995e9

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

jchiSqPht calVarFrameSetInfo WSACalib Goodness of fit of Strateva function to photometric data in J band real 4 -0.9999995e9

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

jchiSqPht dxsVarFrameSetInfo, lasVarFrameSetInfo, udsVarFrameSetInfo WSA Goodness of fit of Strateva function to photometric data in J band real 4 -0.9999995e9

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

jchiSqPht uhsVarFrameSetInfo WSAUHS Goodness of fit of Strateva function to photometric data in J band real 4 -0.9999995e9

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

jClass calSource, calSynopticSource WSACalib discrete image classification flag in J smallint 2 -9999 CLASS_MISC

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

jClass lasYselJSourceRemeasurement WSA discrete image classification flag in J smallint 2 -9999 src.class

jClass uhsSource, uhsSourceAll WSAUHS discrete image classification flag in J smallint 2 -9999 CLASS_MISC

jClassStat calSource, calSynopticSource WSACalib N(0,1) stellarness-of-profile statistic in J real 4 -0.9999995e9 STAT_PROP

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

jClassStat lasYselJSourceRemeasurement WSA N(0,1) stellarness-of-profile statistic in J real 4 -0.9999995e9 stat

jClassStat reliableUdsSource, udsSource WSA S-Extractor classification statistic in J real 4 -0.9999995e9 STAT_PROP

jClassStat uhsSource, uhsSourceAll WSAUHS N(0,1) stellarness-of-profile statistic in J real 4 -0.9999995e9 STAT_PROP

jCorr twompzPhotoz TWOMPZ J 20mag/sq." isophotal fiducial ell. ap. magnitude with Galactic dust correction {image primary HDU keyword: Jcorr} real 4 mag -0.9999995e9 phot.mag;em.IR.J

jCorrErr twompzPhotoz TWOMPZ J 1-sigma uncertainty in 20mag/sq." aperture {image primary HDU keyword: j_msig_k20fe} real 4 mag -0.9999995e9

jcStratAst calVarFrameSetInfo WSACalib Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9

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

jcStratAst dxsVarFrameSetInfo, lasVarFrameSetInfo, udsVarFrameSetInfo WSA Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9

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

jcStratAst uhsVarFrameSetInfo WSAUHS Strateva parameter, c, in fit to astrometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9

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

jcStratPht calVarFrameSetInfo WSACalib Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9

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

jcStratPht dxsVarFrameSetInfo, lasVarFrameSetInfo, udsVarFrameSetInfo WSA Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9

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

jcStratPht uhsVarFrameSetInfo WSAUHS Strateva parameter, c, in fit to photometric rms vs magnitude in J band, see Sesar et al. 2007. real 4 -0.9999995e9

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

jdate twomass_psc 2MASS The Julian Date of the source measurement accurate to +-30 seconds. float 8 Julian days TIME_DATE

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

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

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

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

jDeblend calSource WSACalib placeholder flag indicating parent/child relation in J int 4 -99999999 CODE_MISC

This CASU pipeline processing source extraction flag is a placeholder only, and is always set to zero in all passbands in the merged source lists. If you need to know when a particular image detection is a component of a deblend or not, test bit 4 of attribute ppErrBits (see corresponding glossary entry) which is set by WFAU's 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.

jDeblend calSynopticSource WSACalib placeholder flag indicating parent/child relation in J int 4 -99999999 CODE_MISC

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

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

This CASU pipeline processing source extraction flag is a placeholder only, and is always set to zero in all passbands in the merged source lists. If you need to know when a particular image detection is a component of a deblend or not, test bit 4 of attribute ppErrBits (see corresponding glossary entry) which is set by WFAU's 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.

jDeblend uhsSource, uhsSourceAll WSAUHS placeholder flag indicating parent/child relation in J int 4 -99999999 CODE_MISC

This CASU pipeline processing source extraction flag is a placeholder only, and is always set to zero in all passbands in the merged source lists. If you need to know when a particular image detection is a component of a deblend or not, test bit 4 of attribute ppErrBits (see corresponding glossary entry) which is set by WFAU's 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.

jEll calSource, calSynopticSource WSACalib 1-b/a, where a/b=semi-major/minor axes in J real 4 -0.9999995e9 PHYS_ELLIPTICITY

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

jEll lasYselJSourceRemeasurement WSA 1-b/a, where a/b=semi-major/minor axes in J real 4 -0.9999995e9 src.ellipticty

jEll uhsSource, uhsSourceAll WSAUHS 1-b/a, where a/b=semi-major/minor axes in J real 4 -0.9999995e9 PHYS_ELLIPTICITY

jeNum calMergeLog, calSynopticMergeLog WSACalib the extension number of this J frame tinyint 1 NUMBER

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

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

jeNum lasYselJRemeasMergeLog WSA the extension number of this J frame tinyint 1 meta.number;em.IR.J

jeNum uhsMergeLog WSAUHS the extension number of this J frame tinyint 1 NUMBER

jErrBits calSource, calSynopticSource WSACalib processing warning/error bitwise flags in J int 4 -99999999 CODE_MISC

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

jErrBits dxsJKsource, gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, lasExtendedSource, lasPointSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource WSA processing warning/error bitwise flags in J int 4 -99999999 CODE_MISC

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

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

jErrBits lasYselJSourceRemeasurement WSA processing warning/error bitwise flags in J int 4 -99999999 meta.code

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

jErrBits udsSource WSA processing warning/error bitwise flags in J int 4 -99999999 CODE_MISC

This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows:

Bit Flag Meaning

1 The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected).

2 The object was originally blended with another

4 At least one pixel is saturated (or very close to)

8 The object is truncated (too close to an image boundary)

16 Object's aperture data are incomplete or corrupted

32 Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters.

64 Memory overflow occurred during deblending

128 Memory overflow occurred during extraction

jErrBits uhsSource, uhsSourceAll WSAUHS processing warning/error bitwise flags in J int 4 -99999999 CODE_MISC

Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture.

jEta calSource, calSynopticSource WSACalib Offset of J detection from master position (+north/-south) real 4 arcsec -0.9999995e9 POS_EQ_DEC_OFF

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 2.0 (UKIDSS LAS and GPS; UHS; also 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.

jEta dxsJKsource, gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, lasExtendedSource, lasPointSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource WSA Offset of J detection from master position (+north/-south) real 4 arcsec -0.9999995e9 POS_EQ_DEC_OFF

jEta dxsSource, gcsSource, gpsSource, lasSource, udsSource WSA Offset of J detection from master position (+north/-south) real 4 arcsec -0.9999995e9 POS_EQ_DEC_OFF

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 2.0 (UKIDSS LAS and GPS; UHS; also 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.

jEta uhsSource, uhsSourceAll WSAUHS Offset of J detection from master position (+north/-south) real 4 arcsec -0.9999995e9 POS_EQ_DEC_OFF

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 2.0 (UKIDSS LAS and GPS; UHS; also 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.

jexpML calVarFrameSetInfo WSACalib Expected magnitude limit of frameSet in this in J band. real 4 -0.9999995e9

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

jexpML dxsVarFrameSetInfo, lasVarFrameSetInfo, udsVarFrameSetInfo WSA Expected magnitude limit of frameSet in this in J band. real 4 -0.9999995e9

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

jexpML uhsVarFrameSetInfo WSAUHS Expected magnitude limit of frameSet in this in J band. real 4 -0.9999995e9

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

jExpRms calVariability WSACalib Rms calculated from polynomial fit to modal RMS as a function of magnitude in J band real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jExpRms dxsVariability, lasVariability, udsVariability WSA Rms calculated from polynomial fit to modal RMS as a function of magnitude in J band real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jExpRms uhsVariability WSAUHS Rms calculated from polynomial fit to modal RMS as a function of magnitude in J band real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jGausig calSource, calSynopticSource WSACalib RMS of axes of ellipse fit in J real 4 pixels -0.9999995e9 MORPH_PARAM

jGausig dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource, udsSource WSA RMS of axes of ellipse fit in J real 4 pixels -0.9999995e9 MORPH_PARAM

jGausig lasYselJSourceRemeasurement WSA RMS of axes of ellipse fit in J real 4 pixels -0.9999995e9 src.morph.param

jGausig uhsSource, uhsSourceAll WSAUHS RMS of axes of ellipse fit in J real 4 pixels -0.9999995e9 MORPH_PARAM

jHallMag calSource WSACalib Total point source J mag real 4 mag -0.9999995e9 PHOT_MAG

jHallMag dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource WSA Total point source J mag real 4 mag -0.9999995e9 PHOT_MAG

jHallMag reliableUdsSource, udsSource WSA Not available in SE output real 4 mag -0.9999995e9 PHOT_MAG

jHallMag uhsSource, uhsSourceAll WSAUHS Total point source J mag real 4 mag -0.9999995e9 PHOT_MAG

jHallMagErr calSource WSACalib Error in total point source J mag real 4 mag -0.9999995e9 ERROR

jHallMagErr dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource WSA Error in total point source J mag real 4 mag -0.9999995e9 ERROR

jHallMagErr reliableUdsSource, udsSource WSA Not available in SE output real 4 mag -0.9999995e9 ERROR

jHallMagErr uhsSource, uhsSourceAll WSAUHS Error in total point source J mag real 4 mag -0.9999995e9 ERROR

jhiWS calVariability WSACalib Welch-Stetson statistic between J and H. This assumes colour does not vary much and helps remove variation due to a few poor detections real 4 -0.9999995e9

The 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.

jIntRms calVariability WSACalib Intrinsic rms in J-band real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jIntRms dxsVariability, lasVariability, udsVariability WSA Intrinsic rms in J-band real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jIntRms uhsVariability WSAUHS Intrinsic rms in J-band real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jisDefAst calVarFrameSetInfo WSACalib Use a default model for the astrometric noise in J band. tinyint 1 0

jisDefAst dxsVarFrameSetInfo, lasVarFrameSetInfo, udsVarFrameSetInfo WSA Use a default model for the astrometric noise in J band. tinyint 1 0

jisDefAst uhsVarFrameSetInfo WSAUHS Use a default model for the astrometric noise in J band. tinyint 1 0

jisDefPht calVarFrameSetInfo WSACalib Use a default model for the photometric noise in J band. tinyint 1 0

jisDefPht dxsVarFrameSetInfo, lasVarFrameSetInfo, udsVarFrameSetInfo WSA Use a default model for the photometric noise in J band. tinyint 1 0

jisDefPht uhsVarFrameSetInfo WSAUHS Use a default model for the photometric noise in J band. tinyint 1 0

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

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

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

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

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

jitterX Multiframe WSA X (RA) offset in tel jitter pattern {image primary HDU keyword: JITTER_X} real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff

jitterX Multiframe WSACalib X (RA) offset in tel jitter pattern {image primary HDU keyword: JITTER_X} real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff

jitterX Multiframe WSATransit X (RA) offset in tel jitter pattern {image primary HDU keyword: JITTER_X} real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff

jitterX Multiframe WSAUHS X (RA) offset in tel jitter pattern {image primary HDU keyword: JITTER_X} real 4 arcsec -0.9999995e9 pos.eq.ra;arith.diff

jitterY Multiframe WSA Y (Dec) offset in tel jitter pattern {image primary HDU keyword: JITTER_Y} real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff

jitterY Multiframe WSACalib Y (Dec) offset in tel jitter pattern {image primary HDU keyword: JITTER_Y} real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff

jitterY Multiframe WSATransit Y (Dec) offset in tel jitter pattern {image primary HDU keyword: JITTER_Y} real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff

jitterY Multiframe WSAUHS Y (Dec) offset in tel jitter pattern {image primary HDU keyword: JITTER_Y} real 4 arcsec -0.9999995e9 pos.eq.dec;arith.diff

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

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

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

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

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

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

jMagMAD calVariability WSACalib Median Absolute Deviation of J magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jMagMAD dxsVariability, lasVariability, udsVariability WSA Median Absolute Deviation of J magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jMagMAD uhsVariability WSAUHS Median Absolute Deviation of J magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jMagRms calVariability WSACalib rms of J magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jMagRms dxsVariability, lasVariability, udsVariability WSA rms of J magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jMagRms uhsVariability WSAUHS rms of J magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jmaxCadence calVariability WSACalib maximum gap between observations real 4 days -0.9999995e9

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

jmaxCadence dxsVariability, lasVariability, udsVariability WSA maximum gap between observations real 4 days -0.9999995e9

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

jmaxCadence uhsVariability WSAUHS maximum gap between observations real 4 days -0.9999995e9

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

jMaxMag calVariability WSACalib Maximum magnitude in J band, of good detections real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jMaxMag dxsVariability, lasVariability, udsVariability WSA Maximum magnitude in J band, of good detections real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jMaxMag uhsVariability WSAUHS Maximum magnitude in J band, of good detections real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jmeanMag calVariability WSACalib Mean J magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jmeanMag dxsVariability, lasVariability, udsVariability WSA Mean J magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jmeanMag uhsVariability WSAUHS Mean J magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jmedCadence calVariability WSACalib median gap between observations real 4 days -0.9999995e9

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

jmedCadence dxsVariability, lasVariability, udsVariability WSA median gap between observations real 4 days -0.9999995e9

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

jmedCadence uhsVariability WSAUHS median gap between observations real 4 days -0.9999995e9

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

jmedianMag calVariability WSACalib Median J magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jmedianMag dxsVariability, lasVariability, udsVariability WSA Median J magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jmedianMag uhsVariability WSAUHS Median J magnitude real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jmfID calMergeLog, calSynopticMergeLog WSACalib the UID of the relevant J multiframe bigint 8 ID_FRAME

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

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

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

jmfID uhsMergeLog WSAUHS the UID of the relevant J multiframe bigint 8 ID_FRAME

jmhExt calSource WSACalib Extended source colour J-H (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.

jmhExt dxsJKsource, gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, lasExtendedSource, lasPointSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource WSA Extended source colour J-H (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

jmhExt dxsSource, gcsSource, gpsSource, lasSource, udsSource WSA Extended source colour J-H (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.

jmhExt lasYselJSourceRemeasurement WSA Extended source colour J-H (using aperMagNoAperCorr3) 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.

jmhExtErr calSource WSACalib Error on extended source colour J-H 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.

jmhExtErr dxsJKsource, gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, lasExtendedSource, lasPointSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource WSA Error on extended source colour J-H real 4 mag -0.9999995e9 ERROR

jmhExtErr dxsSource, gcsSource, gpsSource, lasSource, udsSource WSA Error on extended source colour J-H 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.

jmhExtErr lasYselJSourceRemeasurement WSA Error on extended source colour J-H real 4 mag -0.9999995e9 stat.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.

jmhExtJky lasYselJSourceRemeasurement WSA Extended source colour calibrated flux H/J (using aperJkyNoAperCorr3) real 4 jansky -0.9999995e9 phot.color

Default colours from pairs of adjacent passbands within a given set (e.g. 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.

jmhExtJkyErr lasYselJSourceRemeasurement WSA Error on extended source colour calibrated flux H/J real 4 jansky -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. 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.

jmhExtLup lasYselJSourceRemeasurement WSA Extended source colour luptitudeJ-H (using aperLupNoAperCorr3) real 4 lup -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.

jmhExtLupErr lasYselJSourceRemeasurement WSA Error on extended source colour luptitude J-H real 4 lup -0.9999995e9 stat.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.

jmhPnt calSource, calSynopticSource WSACalib Point source colour J-H (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.

jmhPnt dxsJKsource, gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, lasExtendedSource, lasPointSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource WSA Point source colour J-H (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

jmhPnt dxsSource, gcsSource, gpsSource, lasSource, udsSource WSA Point source colour J-H (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.

jmhPnt lasYselJSourceRemeasurement WSA Point source colour J-H (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.

jmhPntErr calSource, calSynopticSource WSACalib Error on point source colour J-H 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.

jmhPntErr dxsJKsource, gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, lasExtendedSource, lasPointSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource WSA Error on point source colour J-H real 4 mag -0.9999995e9 ERROR

jmhPntErr dxsSource, gcsSource, gpsSource, lasSource, udsSource WSA Error on point source colour J-H 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.

jmhPntErr lasYselJSourceRemeasurement WSA Error on point source colour J-H real 4 mag -0.9999995e9 stat.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.

jmhPntJky lasYselJSourceRemeasurement WSA Point source colour calibrated flux H/J (using aperJky3) real 4 jansky -0.9999995e9 phot.color

Default colours from pairs of adjacent passbands within a given set (e.g. 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.

jmhPntJkyErr lasYselJSourceRemeasurement WSA Error on point source colour calibrated flux H/J real 4 jansky -0.9999995e9 stat.error

Default colours from pairs of adjacent passbands within a given set (e.g. 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.

jmhPntLup lasYselJSourceRemeasurement WSA Point source colour luptitude J-H (using aperLup3) real 4 lup -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.

jmhPntLupErr lasYselJSourceRemeasurement WSA Error on point source colour luptitude J-H real 4 lup -0.9999995e9 stat.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.

jminCadence calVariability WSACalib minimum gap between observations real 4 days -0.9999995e9

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

jminCadence dxsVariability, lasVariability, udsVariability WSA minimum gap between observations real 4 days -0.9999995e9

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

jminCadence uhsVariability WSAUHS minimum gap between observations real 4 days -0.9999995e9

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

jMinMag calVariability WSACalib Minimum magnitude in J band, of good detections real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jMinMag dxsVariability, lasVariability, udsVariability WSA Minimum magnitude in J band, of good detections real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jMinMag uhsVariability WSAUHS Minimum magnitude in J band, of good detections real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jmkExt dxsJKsource, reliableDxsSource WSA Extended source colour J-K (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

jmkExt dxsSource WSA Extended source colour J-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.

jmkExt uhsSource WSAUHS Extended source colour J-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.

jmkExtErr dxsJKsource, reliableDxsSource WSA Error on extended source colour J-K real 4 mag -0.9999995e9 ERROR

jmkExtErr dxsSource WSA Error on extended source colour J-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.

jmkExtErr uhsSource WSAUHS Error on extended source colour J-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.

jmkPnt dxsJKsource, reliableDxsSource WSA Point source colour J-K (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

jmkPnt dxsSource WSA Point source colour J-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.

jmkPnt uhsSource WSAUHS Point source colour J-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.

jmkPntErr dxsJKsource, reliableDxsSource WSA Error on point source colour J-K real 4 mag -0.9999995e9 ERROR

jmkPntErr dxsSource WSA Error on point source colour J-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.

jmkPntErr uhsSource WSAUHS Error on point source colour J-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.

jndof calVariability WSACalib Number of degrees of freedom for chisquare smallint 2 -9999

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jndof dxsVariability, lasVariability, udsVariability WSA Number of degrees of freedom for chisquare smallint 2 -9999

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jndof uhsVariability WSAUHS Number of degrees of freedom for chisquare smallint 2 -9999

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jnDofAst calVarFrameSetInfo WSACalib Number of degrees of freedom of astrometric fit in J band. smallint 2 -9999

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

jnDofAst dxsVarFrameSetInfo, lasVarFrameSetInfo, udsVarFrameSetInfo WSA Number of degrees of freedom of astrometric fit in J band. smallint 2 -9999

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

jnDofAst uhsVarFrameSetInfo WSAUHS Number of degrees of freedom of astrometric fit in J band. smallint 2 -9999

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

jnDofPht calVarFrameSetInfo WSACalib Number of degrees of freedom of photometric fit in J band. smallint 2 -9999

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, 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.

jnDofPht dxsVarFrameSetInfo, lasVarFrameSetInfo, udsVarFrameSetInfo WSA Number of degrees of freedom of photometric fit in J band. smallint 2 -9999

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, 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.

jnDofPht uhsVarFrameSetInfo WSAUHS Number of degrees of freedom of photometric fit in J band. smallint 2 -9999

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, 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.

jnFlaggedObs calVariability WSACalib Number of detections in J band flagged as potentially spurious by calDetection.ppErrBits int 4 0

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

jnFlaggedObs dxsVariability WSA Number of detections in J band flagged as potentially spurious by dxsDetection.ppErrBits int 4 0

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

jnFlaggedObs lasVariability WSA Number of detections in J band flagged as potentially spurious by lasDetection.ppErrBits int 4 0

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

jnFlaggedObs udsVariability WSA Number of detections in J band flagged as potentially spurious by udsDetection.ppErrBits int 4 0

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

jnFlaggedObs uhsVariability WSAUHS Number of detections in J band flagged as potentially spurious by uhsDetection.ppErrBits int 4 0

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

jnGoodObs calVariability WSACalib Number of good detections in J band int 4 0

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

jnGoodObs dxsVariability, lasVariability, udsVariability WSA Number of good detections in J band int 4 0

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

jnGoodObs uhsVariability WSAUHS Number of good detections in J band int 4 0

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

jNgt3sig calVariability WSACalib Number of good detections in J-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.

jNgt3sig dxsVariability, lasVariability, udsVariability WSA Number of good detections in J-band that are more than 3 sigma deviations (jAperMagN < (jMeanMag-3*jMagRms) smallint 2 -9999

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jNgt3sig uhsVariability WSAUHS Number of good detections in J-band that are more than 3 sigma deviations (jAperMagN < (jMeanMag-3*jMagRms) smallint 2 -9999

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jnMissingObs calVariability WSACalib Number of J band frames that this object should have been detected on and was not int 4 0

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

jnMissingObs dxsVariability, lasVariability, udsVariability WSA Number of J band frames that this object should have been detected on and was not int 4 0

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

jnMissingObs uhsVariability WSAUHS Number of J band frames that this object should have been detected on and was not int 4 0

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

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

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

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

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

jPA calSource, calSynopticSource WSACalib ellipse fit celestial orientation in J real 4 Degrees -0.9999995e9 POS_POS-ANG

jPA dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource, udsSource WSA ellipse fit celestial orientation in J real 4 Degrees -0.9999995e9 POS_POS-ANG

jPA lasYselJSourceRemeasurement WSA ellipse fit celestial orientation in J real 4 Degrees -0.9999995e9 pos.posAng

jPA uhsSource, uhsSourceAll WSAUHS ellipse fit celestial orientation in J real 4 Degrees -0.9999995e9 POS_POS-ANG

jPetroMag calSource WSACalib Extended source J mag (Petrosian) real 4 mag -0.9999995e9 PHOT_MAG

jPetroMag dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource, udsSource WSA Extended source J mag (Petrosian) real 4 mag -0.9999995e9 PHOT_MAG

jPetroMag uhsSource, uhsSourceAll WSAUHS Extended source J mag (Petrosian) real 4 mag -0.9999995e9 PHOT_MAG

jPetroMagErr calSource WSACalib Error in extended source J mag (Petrosian) real 4 mag -0.9999995e9 ERROR

jPetroMagErr dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource, udsSource WSA Error in extended source J mag (Petrosian) real 4 mag -0.9999995e9 ERROR

jPetroMagErr uhsSource, uhsSourceAll WSAUHS Error in extended source J mag (Petrosian) real 4 mag -0.9999995e9 ERROR

jppErrBits calSource, calSynopticSource WSACalib additional WFAU post-processing error bits in J 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.

jppErrBits dxsJKsource, gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, lasExtendedSource, lasPointSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource, udsSource WSA additional WFAU post-processing error bits in J int 4 0 CODE_MISC

jppErrBits dxsSource, gcsSource, gpsSource, lasSource WSA additional WFAU post-processing error bits in J 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.

jppErrBits lasYselJSourceRemeasurement WSA additional WFAU post-processing error bits in J int 4 0 meta.code

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.

jppErrBits uhsSource, uhsSourceAll WSAUHS additional WFAU post-processing error bits in J 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.

jprobVar calVariability WSACalib 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.

jprobVar dxsVariability, lasVariability, udsVariability WSA 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.

jprobVar uhsVariability WSAUHS 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.

jPsfMag calSource WSACalib Point source profile-fitted J mag real 4 mag -0.9999995e9 PHOT_MAG

jPsfMag dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource WSA Point source profile-fitted J mag real 4 mag -0.9999995e9 PHOT_MAG

jPsfMag reliableUdsSource, udsSource WSA Not available in SE output real 4 mag -0.9999995e9 PHOT_MAG

jPsfMag uhsSource, uhsSourceAll WSAUHS Point source profile-fitted J mag real 4 mag -0.9999995e9 PHOT_MAG

jPsfMagErr calSource WSACalib Error in point source profile-fitted J mag real 4 mag -0.9999995e9 ERROR

jPsfMagErr dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource WSA Error in point source profile-fitted J mag real 4 mag -0.9999995e9 ERROR

jPsfMagErr reliableUdsSource, udsSource WSA Not available in SE output real 4 mag -0.9999995e9 ERROR

jPsfMagErr uhsSource, uhsSourceAll WSAUHS Error in point source profile-fitted J mag real 4 mag -0.9999995e9 ERROR

jSeqNum calSource, calSynopticSource WSACalib the running number of the J detection int 4 -99999999 ID_NUMBER

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

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

jSerMag2D calSource WSACalib Extended source J mag (profile-fitted) real 4 mag -0.9999995e9 PHOT_MAG

jSerMag2D dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource WSA Extended source J mag (profile-fitted) real 4 mag -0.9999995e9 PHOT_MAG

jSerMag2D reliableUdsSource, udsSource WSA Not available in SE output real 4 mag -0.9999995e9 PHOT_MAG

jSerMag2D uhsSource, uhsSourceAll WSAUHS Extended source J mag (profile-fitted) real 4 mag -0.9999995e9 PHOT_MAG

jSerMag2DErr calSource WSACalib Error in extended source J mag (profile-fitted) real 4 mag -0.9999995e9 ERROR

jSerMag2DErr dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource WSA Error in extended source J mag (profile-fitted) real 4 mag -0.9999995e9 ERROR

jSerMag2DErr reliableUdsSource, udsSource WSA Not available in SE output real 4 mag -0.9999995e9 ERROR

jSerMag2DErr uhsSource, uhsSourceAll WSAUHS Error in extended source J mag (profile-fitted) real 4 mag -0.9999995e9 ERROR

jskewness calVariability WSACalib Skewness in J band (see Sesar et al. 2007) real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jskewness dxsVariability, lasVariability, udsVariability WSA Skewness in J band (see Sesar et al. 2007) real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jskewness uhsVariability WSAUHS Skewness in J band (see Sesar et al. 2007) real 4 -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jtotalPeriod calVariability WSACalib 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.

jtotalPeriod dxsVariability, lasVariability, udsVariability WSA 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.

jtotalPeriod uhsVariability WSAUHS 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.

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

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

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

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

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

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

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

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

jVarClass calVariability WSACalib Classification of variability in this band smallint 2 -9999

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jVarClass dxsVariability, lasVariability, udsVariability WSA Classification of variability in this band smallint 2 -9999

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jVarClass uhsVariability WSAUHS Classification of variability in this band smallint 2 -9999

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The 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.

jXi calSource, calSynopticSource WSACalib Offset of J detection from master position (+east/-west) real 4 arcsec -0.9999995e9 POS_EQ_RA_OFF

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 2.0 (UKIDSS LAS and GPS; UHS; also 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.

jXi dxsJKsource, gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, lasExtendedSource, lasPointSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource WSA Offset of J detection from master position (+east/-west) real 4 arcsec -0.9999995e9 POS_EQ_RA_OFF

jXi dxsSource, gcsSource, gpsSource, lasSource, udsSource WSA Offset of J detection from master position (+east/-west) real 4 arcsec -0.9999995e9 POS_EQ_RA_OFF

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 2.0 (UKIDSS LAS and GPS; UHS; also 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.

jXi uhsSource, uhsSourceAll WSAUHS Offset of J detection from master position (+east/-west) real 4 arcsec -0.9999995e9 POS_EQ_RA_OFF

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 2.0 (UKIDSS LAS and GPS; UHS; also 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.

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

wsa-support@roe.ac.uk
17/01/2022