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

K

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

k1 catwise_2020, catwise_prelim WISE W1 photometry usage code (0: neither the ascending nor the descending scan provided a solution; 1: only the ascending scan provided a solution; 2: only the descending scan provided a solution; 3: both scans provided solutions which were combined in the relevant way) int 4

k2 catwise_2020, catwise_prelim WISE W2 photometry usage code (0: neither the ascending nor the descending scan provided a solution; 1: only the ascending scan provided a solution; 2: only the descending scan provided a solution; 3: both scans provided solutions which were combined in the relevant way) int 4

k_1AperMag1 gpsJHKsource, gpsPointSource, reliableGpsPointSource WSA Default point source K_1 aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

k_1AperMag1 gpsSource WSA Default point source K_1 aperture corrected mag (1.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

k_1AperMag1Err gpsJHKsource, gpsPointSource, gpsSource, reliableGpsPointSource WSA Error in point source K_1 mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

k_1AperMag3 gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, reliableGcsPointSource, reliableGpsPointSource WSA Default point source K_1 aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

k_1AperMag3 gcsSource, gpsSource WSA Default point source K_1 aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

k_1AperMag3Err gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, reliableGcsPointSource, reliableGpsPointSource WSA Error in default point source K_1 mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

k_1AperMag4 gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, reliableGcsPointSource, reliableGpsPointSource WSA Point source K_1 aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

k_1AperMag4Err gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, reliableGcsPointSource, reliableGpsPointSource WSA Error in point source K_1 mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

k_1AperMag6 gcsPointSource, gcsSource, gcsZYJHKsource, reliableGcsPointSource WSA Point source K_1 aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

k_1AperMag6Err gcsPointSource, gcsSource, gcsZYJHKsource, reliableGcsPointSource WSA Error in point source K_1 mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

k_1Class gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, reliableGcsPointSource, reliableGpsPointSource WSA discrete image classification flag in K_1 smallint 2 -9999 CLASS_MISC

k_1ClassStat gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, reliableGcsPointSource, reliableGpsPointSource WSA N(0,1) stellarness-of-profile statistic in K_1 real 4 -0.9999995e9 STAT_PROP

k_1Deblend gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, reliableGcsPointSource, reliableGpsPointSource WSA placeholder flag indicating parent/child relation in K_1 int 4 -99999999 CODE_MISC

k_1Deblend gcsSource, gpsSource WSA placeholder flag indicating parent/child relation in K_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.

k_1Ell gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, reliableGcsPointSource, reliableGpsPointSource WSA 1-b/a, where a/b=semi-major/minor axes in K_1 real 4 -0.9999995e9 PHYS_ELLIPTICITY

k_1eNum gcsMergeLog, gcsZYJHKmergeLog, gpsJHKmergeLog, gpsMergeLog WSA the extension number of this K_1 frame tinyint 1 NUMBER

k_1ErrBits gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, reliableGcsPointSource, reliableGpsPointSource WSA processing warning/error bitwise flags in K_1 int 4 -99999999 CODE_MISC

k_1ErrBits gcsSource, gpsSource WSA processing warning/error bitwise flags in K_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.

k_1Eta gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, reliableGcsPointSource, reliableGpsPointSource WSA Offset of K_1 detection from master position (+north/-south) real 4 arcsec -0.9999995e9 POS_EQ_DEC_OFF

k_1Eta gcsSource, gpsSource WSA Offset of K_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.

k_1Gausig gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, reliableGcsPointSource, reliableGpsPointSource WSA RMS of axes of ellipse fit in K_1 real 4 pixels -0.9999995e9 MORPH_PARAM

k_1HallMag gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, reliableGcsPointSource, reliableGpsPointSource WSA Total point source K_1 mag real 4 mag -0.9999995e9 PHOT_MAG

k_1HallMagErr gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, reliableGcsPointSource, reliableGpsPointSource WSA Error in total point source K_1 mag real 4 mag -0.9999995e9 ERROR

k_1mfID gcsMergeLog, gcsZYJHKmergeLog, gpsJHKmergeLog, gpsMergeLog WSA the UID of the relevant K_1 multiframe bigint 8 ID_FRAME

k_1PA gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, reliableGcsPointSource, reliableGpsPointSource WSA ellipse fit celestial orientation in K_1 real 4 Degrees -0.9999995e9 POS_POS-ANG

k_1PetroMag gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, reliableGcsPointSource, reliableGpsPointSource WSA Extended source K_1 mag (Petrosian) real 4 mag -0.9999995e9 PHOT_MAG

k_1PetroMagErr gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, reliableGcsPointSource, reliableGpsPointSource WSA Error in extended source K_1 mag (Petrosian) real 4 mag -0.9999995e9 ERROR

k_1ppErrBits gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, reliableGcsPointSource, reliableGpsPointSource WSA additional WFAU post-processing error bits in K_1 int 4 0 CODE_MISC

k_1ppErrBits gcsSource, gpsSource WSA additional WFAU post-processing error bits in K_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.

k_1PsfMag gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, reliableGcsPointSource, reliableGpsPointSource WSA Point source profile-fitted K_1 mag real 4 mag -0.9999995e9 PHOT_MAG

k_1PsfMagErr gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, reliableGcsPointSource, reliableGpsPointSource WSA Error in point source profile-fitted K_1 mag real 4 mag -0.9999995e9 ERROR

k_1SeqNum gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, reliableGcsPointSource, reliableGpsPointSource WSA the running number of the K_1 detection int 4 -99999999 ID_NUMBER

k_1SerMag2D gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, reliableGcsPointSource, reliableGpsPointSource WSA Extended source K_1 mag (profile-fitted) real 4 mag -0.9999995e9 PHOT_MAG

k_1SerMag2DErr gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, reliableGcsPointSource, reliableGpsPointSource WSA Error in extended source K_1 mag (profile-fitted) real 4 mag -0.9999995e9 ERROR

k_1Xi gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, reliableGcsPointSource, reliableGpsPointSource WSA Offset of K_1 detection from master position (+east/-west) real 4 arcsec -0.9999995e9 POS_EQ_RA_OFF

k_1Xi gcsSource, gpsSource WSA Offset of K_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.

k_2AperMag1 gpsJHKsource, gpsPointSource, reliableGpsPointSource WSA Default point source K_2 aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

k_2AperMag1 gpsSource WSA Default point source K_2 aperture corrected mag (1.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

k_2AperMag1Err gpsJHKsource, gpsPointSource, gpsSource, reliableGpsPointSource WSA Error in point source K_2 mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

k_2AperMag3 gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, reliableGcsPointSource, reliableGpsPointSource WSA Default point source K_2 aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

k_2AperMag3 gcsSource, gpsSource WSA Default point source K_2 aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

k_2AperMag3Err gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, reliableGcsPointSource, reliableGpsPointSource WSA Error in default point source K_2 mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

k_2AperMag4 gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, reliableGcsPointSource, reliableGpsPointSource WSA Point source K_2 aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

k_2AperMag4Err gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, reliableGcsPointSource, reliableGpsPointSource WSA Error in point source K_2 mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

k_2AperMag6 gcsPointSource, gcsSource, gcsZYJHKsource, reliableGcsPointSource WSA Point source K_2 aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

k_2AperMag6Err gcsPointSource, gcsSource, gcsZYJHKsource, reliableGcsPointSource WSA Error in point source K_2 mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

k_2Class gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, reliableGcsPointSource, reliableGpsPointSource WSA discrete image classification flag in K_2 smallint 2 -9999 CLASS_MISC

k_2ClassStat gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, reliableGcsPointSource, reliableGpsPointSource WSA N(0,1) stellarness-of-profile statistic in K_2 real 4 -0.9999995e9 STAT_PROP

k_2Deblend gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, reliableGcsPointSource, reliableGpsPointSource WSA placeholder flag indicating parent/child relation in K_2 int 4 -99999999 CODE_MISC

k_2Deblend gcsSource, gpsSource WSA placeholder flag indicating parent/child relation in K_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.

k_2Ell gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, reliableGcsPointSource, reliableGpsPointSource WSA 1-b/a, where a/b=semi-major/minor axes in K_2 real 4 -0.9999995e9 PHYS_ELLIPTICITY

k_2eNum gcsMergeLog, gcsZYJHKmergeLog, gpsJHKmergeLog, gpsMergeLog WSA the extension number of this K_2 frame tinyint 1 NUMBER

k_2ErrBits gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, reliableGcsPointSource, reliableGpsPointSource WSA processing warning/error bitwise flags in K_2 int 4 -99999999 CODE_MISC

k_2ErrBits gcsSource, gpsSource WSA processing warning/error bitwise flags in K_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.

k_2Eta gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, reliableGcsPointSource, reliableGpsPointSource WSA Offset of K_2 detection from master position (+north/-south) real 4 arcsec -0.9999995e9 POS_EQ_DEC_OFF

k_2Eta gcsSource, gpsSource WSA Offset of K_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.

k_2Gausig gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, reliableGcsPointSource, reliableGpsPointSource WSA RMS of axes of ellipse fit in K_2 real 4 pixels -0.9999995e9 MORPH_PARAM

k_2HallMag gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, reliableGcsPointSource, reliableGpsPointSource WSA Total point source K_2 mag real 4 mag -0.9999995e9 PHOT_MAG

k_2HallMagErr gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, reliableGcsPointSource, reliableGpsPointSource WSA Error in total point source K_2 mag real 4 mag -0.9999995e9 ERROR

k_2mfID gcsMergeLog, gcsZYJHKmergeLog, gpsJHKmergeLog, gpsMergeLog WSA the UID of the relevant K_2 multiframe bigint 8 ID_FRAME

k_2mrat twomass_scn 2MASS Ks-band average 2nd image moment ratio. real 4 FIT_PARAM_VALUE

k_2mrat twomass_sixx2_scn 2MASS K band average 2nd image moment ratio for scan real 4

k_2PA gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, reliableGcsPointSource, reliableGpsPointSource WSA ellipse fit celestial orientation in K_2 real 4 Degrees -0.9999995e9 POS_POS-ANG

k_2PetroMag gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, reliableGcsPointSource, reliableGpsPointSource WSA Extended source K_2 mag (Petrosian) real 4 mag -0.9999995e9 PHOT_MAG

k_2PetroMagErr gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, reliableGcsPointSource, reliableGpsPointSource WSA Error in extended source K_2 mag (Petrosian) real 4 mag -0.9999995e9 ERROR

k_2ppErrBits gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, reliableGcsPointSource, reliableGpsPointSource WSA additional WFAU post-processing error bits in K_2 int 4 0 CODE_MISC

k_2ppErrBits gcsSource, gpsSource WSA additional WFAU post-processing error bits in K_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.

k_2PsfMag gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, reliableGcsPointSource, reliableGpsPointSource WSA Point source profile-fitted K_2 mag real 4 mag -0.9999995e9 PHOT_MAG

k_2PsfMagErr gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, reliableGcsPointSource, reliableGpsPointSource WSA Error in point source profile-fitted K_2 mag real 4 mag -0.9999995e9 ERROR

k_2SeqNum gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, reliableGcsPointSource, reliableGpsPointSource WSA the running number of the K_2 detection int 4 -99999999 ID_NUMBER

k_2SerMag2D gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, reliableGcsPointSource, reliableGpsPointSource WSA Extended source K_2 mag (profile-fitted) real 4 mag -0.9999995e9 PHOT_MAG

k_2SerMag2DErr gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, reliableGcsPointSource, reliableGpsPointSource WSA Error in extended source K_2 mag (profile-fitted) real 4 mag -0.9999995e9 ERROR

k_2Xi gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, reliableGcsPointSource, reliableGpsPointSource WSA Offset of K_2 detection from master position (+east/-west) real 4 arcsec -0.9999995e9 POS_EQ_RA_OFF

k_2Xi gcsSource, gpsSource WSA Offset of K_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.

k_5sig_ba twomass_xsc 2MASS K minor/major axis ratio fit to the 5-sigma isophote. real 4 PHYS_AXIS-RATIO

k_5sig_phi twomass_xsc 2MASS K angle to 5-sigma major axis (E of N). smallint 2 degrees ERROR

k_5surf twomass_xsc 2MASS K central surface brightness (r<=5). real 4 mag PHOT_SB_GENERAL

k_ba twomass_sixx2_xsc 2MASS K minor/major axis ratio fit to the 3-sigma isophote real 4

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

k_back twomass_xsc 2MASS K coadd median background. real 4 CODE_MISC

k_bisym_chi twomass_xsc 2MASS K bi-symmetric cross-correlation chi. real 4 FIT_PARAM_VALUE

k_bisym_rat twomass_xsc 2MASS K bi-symmetric flux ratio. real 4 PHOT_FLUX_RATIO

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

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

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

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

k_con_indx twomass_xsc 2MASS K concentration index r_75%/r_25%. real 4 PHYS_CONCENT_INDEX

k_d_area twomass_xsc 2MASS K 5-sigma to 3-sigma differential area. smallint 2 FIT_RESIDUAL

k_flg_10 twomass_xsc 2MASS K confusion flag for 10 arcsec circular ap. mag. smallint 2 CODE_MISC

k_flg_15 twomass_xsc 2MASS K confusion flag for 15 arcsec circular ap. mag. smallint 2 CODE_MISC

k_flg_20 twomass_xsc 2MASS K confusion flag for 20 arcsec circular ap. mag. smallint 2 CODE_MISC

k_flg_25 twomass_xsc 2MASS K confusion flag for 25 arcsec circular ap. mag. smallint 2 CODE_MISC

k_flg_30 twomass_xsc 2MASS K confusion flag for 30 arcsec circular ap. mag. smallint 2 CODE_MISC

k_flg_40 twomass_xsc 2MASS K confusion flag for 40 arcsec circular ap. mag. smallint 2 CODE_MISC

k_flg_5 twomass_xsc 2MASS K confusion flag for 5 arcsec circular ap. mag. smallint 2 CODE_MISC

k_flg_50 twomass_xsc 2MASS K confusion flag for 50 arcsec circular ap. mag. smallint 2 CODE_MISC

k_flg_60 twomass_xsc 2MASS K confusion flag for 60 arcsec circular ap. mag. smallint 2 CODE_MISC

k_flg_7 twomass_sixx2_xsc 2MASS K confusion flag for 7 arcsec circular ap. mag smallint 2

k_flg_7 twomass_xsc 2MASS K confusion flag for 7 arcsec circular ap. mag. smallint 2 CODE_MISC

k_flg_70 twomass_xsc 2MASS K confusion flag for 70 arcsec circular ap. mag. smallint 2 CODE_MISC

k_flg_c twomass_xsc 2MASS K confusion flag for Kron circular mag. smallint 2 CODE_MISC

k_flg_e twomass_xsc 2MASS K confusion flag for Kron elliptical mag. smallint 2 CODE_MISC

k_flg_fc twomass_xsc 2MASS K confusion flag for fiducial Kron circ. mag. smallint 2 CODE_MISC

k_flg_fe twomass_xsc 2MASS K confusion flag for fiducial Kron ell. mag. smallint 2 CODE_MISC

k_flg_i20c twomass_xsc 2MASS K confusion flag for 20mag/sq." iso. circ. mag. smallint 2 CODE_MISC

k_flg_i20e twomass_xsc 2MASS K confusion flag for 20mag/sq." iso. ell. mag. smallint 2 CODE_MISC

k_flg_i21c twomass_xsc 2MASS K confusion flag for 21mag/sq." iso. circ. mag. smallint 2 CODE_MISC

k_flg_i21e twomass_xsc 2MASS K confusion flag for 21mag/sq." iso. ell. mag. smallint 2 CODE_MISC

k_flg_j21fc twomass_xsc 2MASS K confusion flag for 21mag/sq." iso. fid. circ. mag. smallint 2 CODE_MISC

k_flg_j21fe twomass_xsc 2MASS K confusion flag for 21mag/sq." iso. fid. ell. mag. smallint 2 CODE_MISC

k_flg_k20fc twomass_xsc 2MASS K confusion flag for 20mag/sq." iso. fid. circ. mag. smallint 2 CODE_MISC

k_flg_k20fe twomass_sixx2_xsc 2MASS K confusion flag for 20mag/sq.″ iso. fid. ell. mag smallint 2

k_flg_k20fe twomass_xsc 2MASS K confusion flag for 20mag/sq." iso. fid. ell. mag. smallint 2 CODE_MISC

k_m twomass_psc 2MASS Default Ks-band magnitude real 4 mag SPECT_FLUX_VALUE

k_m twomass_sixx2_psc 2MASS K selected "default" magnitude real 4 mag

k_m_10 twomass_xsc 2MASS K 10 arcsec radius circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

k_m_15 twomass_xsc 2MASS K 15 arcsec radius circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

k_m_20 twomass_xsc 2MASS K 20 arcsec radius circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

k_m_25 twomass_xsc 2MASS K 25 arcsec radius circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

k_m_2mass allwise_sc WISE 2MASS K_s-band magnitude of the associated 2MASS PSC source. This column is "null" if there is no associated 2MASS PSC source or if the 2MASS PSC K_s-band magnitude entry is "null". float 8 mag

k_m_2mass wise_allskysc WISE 2MASS Ks-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 Ks-band magnitude entry is default. real 4 mag -0.9999995e9

k_m_2mass wise_prelimsc WISE 2MASS Ks-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 Ks-band magnitude entry is default real 4 mag -0.9999995e9

k_m_30 twomass_xsc 2MASS K 30 arcsec radius circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

k_m_40 twomass_xsc 2MASS K 40 arcsec radius circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

k_m_5 twomass_xsc 2MASS K 5 arcsec radius circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

k_m_50 twomass_xsc 2MASS K 50 arcsec radius circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

k_m_60 twomass_xsc 2MASS K 60 arcsec radius circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

k_m_7 twomass_sixx2_xsc 2MASS K 7 arcsec radius circular aperture magnitude real 4 mag

k_m_7 twomass_xsc 2MASS K 7 arcsec radius circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

k_m_70 twomass_xsc 2MASS K 70 arcsec radius circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

k_m_c twomass_xsc 2MASS K Kron circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

k_m_e twomass_xsc 2MASS K Kron elliptical aperture magnitude. real 4 mag SPECT_FLUX_VALUE

k_m_ext twomass_sixx2_xsc 2MASS K mag from fit extrapolation real 4 mag

k_m_ext twomass_xsc 2MASS K mag from fit extrapolation. real 4 mag SPECT_FLUX_VALUE

k_m_fc twomass_xsc 2MASS K fiducial Kron circular magnitude. real 4 mag SPECT_FLUX_VALUE

k_m_fe twomass_xsc 2MASS K fiducial Kron ell. mag aperture magnitude. real 4 mag SPECT_FLUX_VALUE

k_m_i20c twomass_xsc 2MASS K 20mag/sq." isophotal circular ap. magnitude. real 4 mag SPECT_FLUX_VALUE

k_m_i20e twomass_xsc 2MASS K 20mag/sq." isophotal elliptical ap. magnitude. real 4 mag SPECT_FLUX_VALUE

k_m_i21c twomass_xsc 2MASS K 21mag/sq." isophotal circular ap. magnitude. real 4 mag SPECT_FLUX_VALUE

k_m_i21e twomass_xsc 2MASS K 21mag/sq." isophotal elliptical ap. magnitude. real 4 mag SPECT_FLUX_VALUE

k_m_j21fc twomass_xsc 2MASS K 21mag/sq." isophotal fiducial circ. ap. mag. real 4 mag SPECT_FLUX_VALUE

k_m_j21fe twomass_xsc 2MASS K 21mag/sq." isophotal fiducial ell. ap. magnitude. real 4 mag SPECT_FLUX_VALUE

k_m_k20fc twomass_xsc 2MASS K 20mag/sq." isophotal fiducial circ. ap. mag. real 4 mag SPECT_FLUX_VALUE

k_m_k20fe twomass_sixx2_xsc 2MASS K 20mag/sq.″ isophotal fiducial ell. ap. magnitude real 4 mag

k_m_k20fe twomass_xsc 2MASS K 20mag/sq." isophotal fiducial ell. ap. magnitude. real 4 mag SPECT_FLUX_VALUE

k_m_stdap twomass_psc 2MASS Ks-band "standard" aperture magnitude. real 4 mag SPECT_FLUX_VALUE

k_m_sys twomass_xsc 2MASS K system photometry magnitude. real 4 mag SPECT_FLUX_VALUE

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

k_msig twomass_sixx2_psc 2MASS K "default" mag uncertainty real 4 mag

k_msig_10 twomass_xsc 2MASS K 1-sigma uncertainty in 10 arcsec circular ap. mag. real 4 mag ERROR

k_msig_15 twomass_xsc 2MASS K 1-sigma uncertainty in 15 arcsec circular ap. mag. real 4 mag ERROR

k_msig_20 twomass_xsc 2MASS K 1-sigma uncertainty in 20 arcsec circular ap. mag. real 4 mag ERROR

k_msig_25 twomass_xsc 2MASS K 1-sigma uncertainty in 25 arcsec circular ap. mag. real 4 mag ERROR

k_msig_2mass allwise_sc WISE 2MASS K_s-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 K_s-band uncertainty entry is "null". float 8 mag

k_msig_2mass wise_allskysc WISE 2MASS Ks-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 Ks-band uncertainty entry is default. real 4 mag -0.9999995e9

k_msig_2mass wise_prelimsc WISE 2MASS Ks-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 Ks-band uncertainty entry is default real 4 mag -0.9999995e9

k_msig_30 twomass_xsc 2MASS K 1-sigma uncertainty in 30 arcsec circular ap. mag. real 4 mag ERROR

k_msig_40 twomass_xsc 2MASS K 1-sigma uncertainty in 40 arcsec circular ap. mag. real 4 mag ERROR

k_msig_5 twomass_xsc 2MASS K 1-sigma uncertainty in 5 arcsec circular ap. mag. real 4 mag ERROR

k_msig_50 twomass_xsc 2MASS K 1-sigma uncertainty in 50 arcsec circular ap. mag. real 4 mag ERROR

k_msig_60 twomass_xsc 2MASS K 1-sigma uncertainty in 60 arcsec circular ap. mag. real 4 mag ERROR

k_msig_7 twomass_sixx2_xsc 2MASS K 1-sigma uncertainty in 7 arcsec circular ap. mag real 4 mag

k_msig_7 twomass_xsc 2MASS K 1-sigma uncertainty in 7 arcsec circular ap. mag. real 4 mag ERROR

k_msig_70 twomass_xsc 2MASS K 1-sigma uncertainty in 70 arcsec circular ap. mag. real 4 mag ERROR

k_msig_c twomass_xsc 2MASS K 1-sigma uncertainty in Kron circular mag. real 4 mag ERROR

k_msig_e twomass_xsc 2MASS K 1-sigma uncertainty in Kron elliptical mag. real 4 mag ERROR

k_msig_ext twomass_sixx2_xsc 2MASS K 1-sigma uncertainty in mag from fit extrapolation real 4 mag

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

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

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

k_msig_i20c twomass_xsc 2MASS K 1-sigma uncertainty in 20mag/sq." iso. circ. mag. real 4 mag ERROR

k_msig_i20e twomass_xsc 2MASS K 1-sigma uncertainty in 20mag/sq." iso. ell. mag. real 4 mag ERROR

k_msig_i21c twomass_xsc 2MASS K 1-sigma uncertainty in 21mag/sq." iso. circ. mag. real 4 mag ERROR

k_msig_i21e twomass_xsc 2MASS K 1-sigma uncertainty in 21mag/sq." iso. ell. mag. real 4 mag ERROR

k_msig_j21fc twomass_xsc 2MASS K 1-sigma uncertainty in 21mag/sq." iso.fid.circ.mag. real 4 mag ERROR

k_msig_j21fe twomass_xsc 2MASS K 1-sigma uncertainty in 21mag/sq." iso.fid.ell.mag. real 4 mag ERROR

k_msig_k20fc twomass_xsc 2MASS K 1-sigma uncertainty in 20mag/sq." iso.fid.circ. mag. real 4 mag ERROR

k_msig_k20fe twomass_sixx2_xsc 2MASS K 1-sigma uncertainty in 20mag/sq.″ iso.fid.ell.mag real 4 mag

k_msig_k20fe twomass_xsc 2MASS K 1-sigma uncertainty in 20mag/sq." iso.fid.ell.mag. real 4 mag ERROR

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

k_msig_sys twomass_xsc 2MASS K 1-sigma uncertainty in system photometry mag. real 4 mag ERROR

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

k_msigcom twomass_sixx2_psc 2MASS combined (total) K band photometric uncertainty real 4 mag

k_msnr10 twomass_scn 2MASS The estimated Ks-band magnitude at which SNR=10 is achieved for this scan. real 4 mag SPECT_FLUX_VALUE

k_msnr10 twomass_sixx2_scn 2MASS K mag at which SNR=10 is achieved, from k_psp and k_zp_ap real 4 mag

k_n_snr10 twomass_scn 2MASS Number of point sources at Ks-band with SNR>10 (instrumental mag <=14.3) int 4 NUMBER

k_n_snr10 twomass_sixx2_scn 2MASS number of K point sources with SNR>10 (instrumental m<=14.3) int 4

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

k_peak twomass_xsc 2MASS K peak pixel brightness. real 4 mag PHOT_SB_GENERAL

k_perc_darea twomass_xsc 2MASS K 5-sigma to 3-sigma percent area change. smallint 2 FIT_PARAM

k_phi twomass_sixx2_xsc 2MASS K angle to 3-sigma major axis (E of N) smallint 2 deg

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

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

k_psp twomass_scn 2MASS Ks-band photometric sensitivity paramater (PSP). real 4 INST_SENSITIVITY

k_psp twomass_sixx2_scn 2MASS K photometric sensitivity param: k_shape_avg*(k_fbg_avg^.29) real 4

k_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 Ks-band photometric errors and is expressed in units of mJy. real 4 INST_NOISE

k_pts_noise twomass_sixx2_scn 2MASS log10 of K band modal point src noise estimate real 4 logmJy

k_r_c twomass_xsc 2MASS K Kron circular aperture radius. real 4 arcsec EXTENSION_RAD

k_r_e twomass_xsc 2MASS K Kron elliptical aperture semi-major axis. real 4 arcsec EXTENSION_RAD

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

k_r_i20c twomass_xsc 2MASS K 20mag/sq." isophotal circular aperture radius. real 4 arcsec EXTENSION_RAD

k_r_i20e twomass_xsc 2MASS K 20mag/sq." isophotal elliptical ap. semi-major axis. real 4 arcsec EXTENSION_RAD

k_r_i21c twomass_xsc 2MASS K 21mag/sq." isophotal circular aperture radius. real 4 arcsec EXTENSION_RAD

k_r_i21e twomass_xsc 2MASS K 21mag/sq." isophotal elliptical ap. semi-major axis. real 4 arcsec EXTENSION_RAD

k_resid_ann twomass_xsc 2MASS K residual annulus background median. real 4 DN CODE_MISC

k_sc_1mm twomass_xsc 2MASS K 1st moment (score) (LCSB: super blk 2,4,8 SNR). real 4 CODE_MISC

k_sc_2mm twomass_xsc 2MASS K 2nd moment (score) (LCSB: SNRMAX - super SNR max). real 4 CODE_MISC

k_sc_msh twomass_xsc 2MASS K median shape score. real 4 CODE_MISC

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

k_sc_r1 twomass_xsc 2MASS K r1 (score). real 4 CODE_MISC

k_sc_r23 twomass_xsc 2MASS K r23 (score) (LCSB: TSNR - integrated SNR for r=15). real 4 CODE_MISC

k_sc_sh twomass_xsc 2MASS K shape (score). real 4 CODE_MISC

k_sc_vint twomass_xsc 2MASS K vint (score). real 4 CODE_MISC

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

k_seetrack twomass_xsc 2MASS K band seetracking score. real 4 CODE_MISC

k_sh0 twomass_xsc 2MASS K ridge shape (LCSB: BSNR limit). real 4 FIT_PARAM

k_shape_avg twomass_scn 2MASS Ks-band average seeing shape for scan. real 4 INST_SEEING

k_shape_avg twomass_sixx2_scn 2MASS K band average seeing shape for scan real 4

k_shape_rms twomass_scn 2MASS RMS-error of Ks-band average seeing shape. real 4 INST_SEEING

k_shape_rms twomass_sixx2_scn 2MASS rms of K band avg seeing shape for scan real 4

k_sig_sh0 twomass_xsc 2MASS K ridge shape sigma (LCSB: B2SNR limit). real 4 FIT_PARAM

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

k_snr twomass_sixx2_psc 2MASS K band "scan" signal-to-noise ratio real 4

k_subst2 twomass_xsc 2MASS K residual background #2 (score). real 4 CODE_MISC

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

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

k_zperr_ap twomass_scn 2MASS RMS-error of zero-point for Ks-band aperture photometry real 4 mag FIT_ERROR

k_zperr_ap twomass_sixx2_scn 2MASS K band ap. calibration rms error of zero-point for scan real 4 mag

ka catwise_2020, catwise_prelim WISE astrometry usage code (0: neither the ascending nor the descending scan provided a solution; 1: only the ascending scan provided a solution; 2: only the descending scan provided a solution; 3: both scans provided solutions which were combined in the relevant way) int 4

kAperJky3 lasYselJSourceRemeasurement WSA Default point source K aperture corrected (2.0 arcsec aperture diameter) calibrated flux
If in doubt use this flux estimator real 4 jansky -0.9999995e9 phot.flux

kAperJky3Err lasYselJSourceRemeasurement WSA Error in default point/extended source K (2.0 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error

kAperJky4 lasYselJSourceRemeasurement WSA Point source K aperture corrected (2.8 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 phot.flux

kAperJky4Err lasYselJSourceRemeasurement WSA Error in point/extended source K (2.8 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error

kAperJky6 lasYselJSourceRemeasurement WSA Point source K aperture corrected (5.7 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 phot.flux

kAperJky6Err lasYselJSourceRemeasurement WSA Error in point/extended source K (5.7 arcsec aperture diameter) calibrated flux real 4 jansky -0.9999995e9 stat.error

kAperJkyNoAperCorr3 lasYselJSourceRemeasurement WSA Default extended source K (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

kAperJkyNoAperCorr4 lasYselJSourceRemeasurement WSA Extended source K (2.8 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux real 4 jansky -0.9999995e9 phot.flux

kAperJkyNoAperCorr6 lasYselJSourceRemeasurement WSA Extended source K (5.7 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux real 4 jansky -0.9999995e9 phot.flux

kAperLup3 lasYselJSourceRemeasurement WSA Default point source K aperture corrected (2.0 arcsec aperture diameter) luptitude
If in doubt use this flux estimator real 4 lup -0.9999995e9 phot.lup

kAperLup3Err lasYselJSourceRemeasurement WSA Error in default point/extended source K (2.0 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error

kAperLup4 lasYselJSourceRemeasurement WSA Point source K aperture corrected (2.8 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 phot.lup

kAperLup4Err lasYselJSourceRemeasurement WSA Error in point/extended source K (2.8 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error

kAperLup6 lasYselJSourceRemeasurement WSA Point source K aperture corrected (5.7 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 phot.lup

kAperLup6Err lasYselJSourceRemeasurement WSA Error in point/extended source K (5.7 arcsec aperture diameter) luptitude real 4 lup -0.9999995e9 stat.error

kAperLupNoAperCorr3 lasYselJSourceRemeasurement WSA Default extended source K (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

kAperLupNoAperCorr4 lasYselJSourceRemeasurement WSA Extended source K (2.8 arcsec aperture diameter, but no aperture correction applied) aperture luptitude real 4 lup -0.9999995e9 phot.lup

kAperLupNoAperCorr6 lasYselJSourceRemeasurement WSA Extended source K (5.7 arcsec aperture diameter, but no aperture correction applied) aperture luptitude real 4 lup -0.9999995e9 phot.lup

kAperMag1 calSynopticSource WSACalib Extended source K aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

kAperMag1 gpsJHKsource, gpsPointSource, reliableGpsPointSource WSA Default point source K aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

kAperMag1 gpsSource WSA Default point source K aperture corrected mag (1.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

kAperMag1Err calSynopticSource WSACalib Error in extended source K mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

kAperMag1Err gpsJHKsource, gpsPointSource, gpsSource, reliableGpsPointSource WSA Error in point source K mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

kAperMag2 calSynopticSource WSACalib Extended source K aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

kAperMag2Err calSynopticSource WSACalib Error in extended source K mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

kAperMag3 calSource WSACalib Default point/extended source K aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

kAperMag3 calSynopticSource WSACalib Default point/extended source K aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

kAperMag3 dxsJKsource, gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, lasExtendedSource, lasPointSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource WSA Default point source K aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

kAperMag3 dxsSource, gcsSource, gpsSource, lasSource WSA Default point source K aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

kAperMag3 lasYselJSourceRemeasurement WSA Default point source K aperture corrected (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 phot.mag

kAperMag3 reliableUdsSource WSA Default point/extended source K mag, no aperture correction applied real 4 mag -0.9999995e9 PHOT_MAG

kAperMag3 udsSource WSA Default point/extended source K mag, no aperture correction applied
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

kAperMag3 uhsSource, uhsSourceAll WSAUHS Default point source K aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

kAperMag3Err calSource, calSynopticSource WSACalib Error in default point/extended source K mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

kAperMag3Err dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource WSA Error in default point source K mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

kAperMag3Err lasYselJSourceRemeasurement WSA Error in default point/extended source K (2.0 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error

kAperMag3Err reliableUdsSource, udsSource WSA Error in default point/extended source K mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

kAperMag3Err uhsSource, uhsSourceAll WSAUHS Error in default point source K mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

kAperMag4 calSource, calSynopticSource WSACalib Extended source K aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

kAperMag4 dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource WSA Point source K aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

kAperMag4 lasYselJSourceRemeasurement WSA Point source K aperture corrected (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

kAperMag4 reliableUdsSource, udsSource WSA Extended source K mag, no aperture correction applied real 4 mag -0.9999995e9 PHOT_MAG

kAperMag4 uhsSource, uhsSourceAll WSAUHS Point source K aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

kAperMag4Err calSource, calSynopticSource WSACalib Error in extended source K mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

kAperMag4Err dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource WSA Error in point source K mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

kAperMag4Err lasYselJSourceRemeasurement WSA Error in point/extended source K (2.8 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error

kAperMag4Err reliableUdsSource, udsSource WSA Error in extended source K mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

kAperMag4Err uhsSource, uhsSourceAll WSAUHS Error in point source K mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

kAperMag5 calSynopticSource WSACalib Extended source K aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

kAperMag5Err calSynopticSource WSACalib Error in extended source K mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

kAperMag6 calSource WSACalib Extended source K aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

kAperMag6 dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableLasPointSource WSA Point source K aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

kAperMag6 lasYselJSourceRemeasurement WSA Point source K aperture corrected (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 phot.mag

kAperMag6 reliableUdsSource, udsSource WSA Extended source K mag, no aperture correction applied real 4 mag -0.9999995e9 PHOT_MAG

kAperMag6 uhsSource, uhsSourceAll WSAUHS Point source K aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

kAperMag6Err calSource WSACalib Error in extended source K mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

kAperMag6Err dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableLasPointSource WSA Error in point source K mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

kAperMag6Err lasYselJSourceRemeasurement WSA Error in point/extended source K (5.7 arcsec aperture diameter) magnitude real 4 mag -0.9999995e9 stat.error

kAperMag6Err reliableUdsSource, udsSource WSA Error in extended source K mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

kAperMag6Err uhsSource, uhsSourceAll WSAUHS Error in point source K mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

kAperMagNoAperCorr3 lasYselJSourceRemeasurement WSA Default extended source K (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

kAperMagNoAperCorr4 lasYselJSourceRemeasurement WSA Extended source K (2.8 arcsec aperture diameter, but no aperture correction applied) aperture magnitude real 4 mag -0.9999995e9 phot.mag

kAperMagNoAperCorr6 lasYselJSourceRemeasurement WSA Extended source K (5.7 arcsec aperture diameter, but no aperture correction applied) aperture magnitude real 4 mag -0.9999995e9 phot.mag

kaStratAst calVarFrameSetInfo WSACalib Strateva parameter, a, in fit to astrometric rms vs magnitude in K 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.

kaStratAst dxsVarFrameSetInfo, gcsVarFrameSetInfo, gpsVarFrameSetInfo, udsVarFrameSetInfo WSA Strateva parameter, a, in fit to astrometric rms vs magnitude in K 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.

kaStratPht calVarFrameSetInfo WSACalib Strateva parameter, a, in fit to photometric rms vs magnitude in K 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.

kaStratPht dxsVarFrameSetInfo, gcsVarFrameSetInfo, gpsVarFrameSetInfo, udsVarFrameSetInfo WSA Strateva parameter, a, in fit to photometric rms vs magnitude in K 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.

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

kbestAper calVariability WSACalib Best aperture (1-6) for photometric statistics in the K 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)

kbestAper dxsVariability, gcsVariability, gpsVariability, udsVariability WSA Best aperture (1-6) for photometric statistics in the K 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)

kbStratAst calVarFrameSetInfo WSACalib Strateva parameter, b, in fit to astrometric rms vs magnitude in K 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.

kbStratAst dxsVarFrameSetInfo, gcsVarFrameSetInfo, gpsVarFrameSetInfo, udsVarFrameSetInfo WSA Strateva parameter, b, in fit to astrometric rms vs magnitude in K 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.

kbStratPht calVarFrameSetInfo WSACalib Strateva parameter, b, in fit to photometric rms vs magnitude in K 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.

kbStratPht dxsVarFrameSetInfo, gcsVarFrameSetInfo, gpsVarFrameSetInfo, udsVarFrameSetInfo WSA Strateva parameter, b, in fit to photometric rms vs magnitude in K 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.

kchiSqAst calVarFrameSetInfo WSACalib Goodness of fit of Strateva function to astrometric data in K 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.

kchiSqAst dxsVarFrameSetInfo, gcsVarFrameSetInfo, gpsVarFrameSetInfo, udsVarFrameSetInfo WSA Goodness of fit of Strateva function to astrometric data in K 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.

kchiSqpd 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.

kchiSqpd dxsVariability, gcsVariability, gpsVariability, 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.

kchiSqPht calVarFrameSetInfo WSACalib Goodness of fit of Strateva function to photometric data in K 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.

kchiSqPht dxsVarFrameSetInfo, gcsVarFrameSetInfo, gpsVarFrameSetInfo, udsVarFrameSetInfo WSA Goodness of fit of Strateva function to photometric data in K 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.

kClass calSource, calSynopticSource WSACalib discrete image classification flag in K smallint 2 -9999 CLASS_MISC

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

kClass lasYselJSourceRemeasurement WSA discrete image classification flag in K smallint 2 -9999 src.class

kClass uhsSource, uhsSourceAll WSAUHS discrete image classification flag in K smallint 2 -9999 CLASS_MISC

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

kClassStat 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 K real 4 -0.9999995e9 STAT_PROP

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

kClassStat reliableUdsSource, udsSource WSA S-Extractor classification statistic in K real 4 -0.9999995e9 STAT_PROP

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

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

kCorrErr twompzPhotoz TWOMPZ K 1-sigma uncertainty in 20mag/sq." aperture {image primary HDU keyword: k_msig_k20fe} real 4 mag -0.9999995e9

kcStratAst calVarFrameSetInfo WSACalib Strateva parameter, c, in fit to astrometric rms vs magnitude in K 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.

kcStratAst dxsVarFrameSetInfo, gcsVarFrameSetInfo, gpsVarFrameSetInfo, udsVarFrameSetInfo WSA Strateva parameter, c, in fit to astrometric rms vs magnitude in K 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.

kcStratPht calVarFrameSetInfo WSACalib Strateva parameter, c, in fit to photometric rms vs magnitude in K 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.

kcStratPht dxsVarFrameSetInfo, gcsVarFrameSetInfo, gpsVarFrameSetInfo, udsVarFrameSetInfo WSA Strateva parameter, c, in fit to photometric rms vs magnitude in K 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.

kDeblend calSource WSACalib placeholder flag indicating parent/child relation in K 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.

kDeblend calSynopticSource WSACalib placeholder flag indicating parent/child relation in K int 4 -99999999 CODE_MISC

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

kDeblend dxsSource, gcsSource, gpsSource, lasSource WSA placeholder flag indicating parent/child relation in K 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.

kDeblend uhsSource, uhsSourceAll WSAUHS placeholder flag indicating parent/child relation in K 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.

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

kEll 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 K real 4 -0.9999995e9 PHYS_ELLIPTICITY

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

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

keNum calMergeLog, calSynopticMergeLog WSACalib the extension number of this K frame tinyint 1 NUMBER

keNum dxsJKmergeLog, dxsMergeLog, gcsMergeLog, gcsZYJHKmergeLog, gpsJHKmergeLog, gpsMergeLog, lasMergeLog, lasYJHKmergeLog, udsMergeLog WSA the extension number of this K frame tinyint 1 NUMBER

keNum lasYselJRemeasMergeLog WSA the extension number of this K frame tinyint 1 meta.number;em.IR.K

keNum uhsMergeLog WSAUHS the extension number of this K frame tinyint 1 NUMBER

kErrBits calSource, calSynopticSource WSACalib processing warning/error bitwise flags in K 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.

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

kErrBits dxsSource, gcsSource, gpsSource, lasSource WSA processing warning/error bitwise flags in K 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.

kErrBits lasYselJSourceRemeasurement WSA processing warning/error bitwise flags in K 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.

kErrBits udsSource WSA processing warning/error bitwise flags in K 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

kErrBits uhsSource, uhsSourceAll WSAUHS processing warning/error bitwise flags in K 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.

kEta calSource, calSynopticSource WSACalib Offset of K 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.

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

kEta dxsSource, gcsSource, gpsSource, lasSource, udsSource WSA Offset of K 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.

kEta uhsSource, uhsSourceAll WSAUHS Offset of K 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.

kexpML calVarFrameSetInfo WSACalib Expected magnitude limit of frameSet in this in K 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.

kexpML dxsVarFrameSetInfo, gcsVarFrameSetInfo, gpsVarFrameSetInfo, udsVarFrameSetInfo WSA Expected magnitude limit of frameSet in this in K 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.

kExpRms calVariability WSACalib Rms calculated from polynomial fit to modal RMS as a function of magnitude in K 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.

kExpRms dxsVariability, gcsVariability, gpsVariability, udsVariability WSA Rms calculated from polynomial fit to modal RMS as a function of magnitude in K 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.

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

kGausig 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 K real 4 pixels -0.9999995e9 MORPH_PARAM

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

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

kHallMag calSource WSACalib Total point source K mag real 4 mag -0.9999995e9 PHOT_MAG

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

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

kHallMag uhsSource, uhsSourceAll WSAUHS Total point source K mag real 4 mag -0.9999995e9 PHOT_MAG

kHallMagErr calSource WSACalib Error in total point source K mag real 4 mag -0.9999995e9 ERROR

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

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

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

kIntRms calVariability WSACalib Intrinsic rms in K-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.

kIntRms dxsVariability, gcsVariability, gpsVariability, udsVariability WSA Intrinsic rms in K-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.

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

kisDefAst dxsVarFrameSetInfo, gcsVarFrameSetInfo, gpsVarFrameSetInfo, udsVarFrameSetInfo WSA Use a default model for the astrometric noise in K band. tinyint 1 0

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

kisDefPht dxsVarFrameSetInfo, gcsVarFrameSetInfo, gpsVarFrameSetInfo, udsVarFrameSetInfo WSA Use a default model for the photometric noise in K band. tinyint 1 0

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

km catwise_2020, catwise_prelim WISE proper motion usage code (0: neither the ascending nor the descending scan provided a solution; 1: only the ascending scan provided a solution; 2: only the descending scan provided a solution; 3: both scans provided solutions which were combined in the relevant way) int 4

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

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

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

kMagErr ukirtFSstars WSA K band magnitude error real 4 mag stat.error

kMagErr ukirtFSstars WSACalib K band magnitude error real 4 mag stat.error

kMagErr ukirtFSstars WSAUHS K band magnitude error real 4 mag stat.error

kMagMAD calVariability WSACalib Median Absolute Deviation of K 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.

kMagMAD dxsVariability, gcsVariability, gpsVariability, udsVariability WSA Median Absolute Deviation of K 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.

kMagRms calVariability WSACalib rms of K 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.

kMagRms dxsVariability, gcsVariability, gpsVariability, udsVariability WSA rms of K 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.

kmaxCadence 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.

kmaxCadence dxsVariability, gcsVariability, gpsVariability, 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.

kMaxMag calVariability WSACalib Maximum magnitude in K 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.

kMaxMag dxsVariability, gcsVariability, gpsVariability, udsVariability WSA Maximum magnitude in K 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.

kmeanMag calVariability WSACalib Mean K 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.

kmeanMag dxsVariability, gcsVariability, gpsVariability, udsVariability WSA Mean K 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.

kmedCadence 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.

kmedCadence dxsVariability, gcsVariability, gpsVariability, 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.

kmedianMag calVariability WSACalib Median K 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.

kmedianMag dxsVariability, gcsVariability, gpsVariability, udsVariability WSA Median K 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.

kmfID calMergeLog, calSynopticMergeLog WSACalib the UID of the relevant K multiframe bigint 8 ID_FRAME

kmfID dxsJKmergeLog, dxsMergeLog, gcsMergeLog, gcsZYJHKmergeLog, gpsJHKmergeLog, gpsMergeLog, lasMergeLog, lasYJHKmergeLog, udsMergeLog WSA the UID of the relevant K multiframe bigint 8 ID_FRAME

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

kmfID uhsMergeLog WSAUHS the UID of the relevant K multiframe bigint 8 ID_FRAME

kminCadence 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.

kminCadence dxsVariability, gcsVariability, gpsVariability, 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.

kMinMag calVariability WSACalib Minimum magnitude in K 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.

kMinMag dxsVariability, gcsVariability, gpsVariability, udsVariability WSA Minimum magnitude in K 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.

kndof 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.

kndof dxsVariability, gcsVariability, gpsVariability, 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.

knDofAst calVarFrameSetInfo WSACalib Number of degrees of freedom of astrometric fit in K 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.

knDofAst dxsVarFrameSetInfo, gcsVarFrameSetInfo, gpsVarFrameSetInfo, udsVarFrameSetInfo WSA Number of degrees of freedom of astrometric fit in K 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.

knDofPht calVarFrameSetInfo WSACalib Number of degrees of freedom of photometric fit in K 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.

knDofPht dxsVarFrameSetInfo, gcsVarFrameSetInfo, gpsVarFrameSetInfo, udsVarFrameSetInfo WSA Number of degrees of freedom of photometric fit in K 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.

knFlaggedObs calVariability WSACalib Number of detections in K 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.

knFlaggedObs dxsVariability WSA Number of detections in K 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.

knFlaggedObs gcsVariability WSA Number of detections in K band flagged as potentially spurious by gcsDetection.ppErrBits int 4 0

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

knFlaggedObs gpsVariability WSA Number of detections in K band flagged as potentially spurious by gpsDetection.ppErrBits int 4 0

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

knFlaggedObs udsVariability WSA Number of detections in K 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.

knGoodObs calVariability WSACalib Number of good detections in K 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.

knGoodObs dxsVariability, gcsVariability, gpsVariability, udsVariability WSA Number of good detections in K 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.

kNgt3sig calVariability WSACalib Number of good detections in K-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.

kNgt3sig dxsVariability, gcsVariability, gpsVariability, udsVariability WSA Number of good detections in K-band that are more than 3 sigma deviations (kAperMagN < (kMeanMag-3*kMagRms) 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.

knMissingObs calVariability WSACalib Number of K 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.

knMissingObs dxsVariability, gcsVariability, gpsVariability, udsVariability WSA Number of K 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.

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

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

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

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

kPetroMag calSource WSACalib Extended source K mag (Petrosian) real 4 mag -0.9999995e9 PHOT_MAG

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

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

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

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

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

kppErrBits calSource, calSynopticSource WSACalib additional WFAU post-processing error bits in K 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.

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

kppErrBits dxsSource, gcsSource, gpsSource, lasSource WSA additional WFAU post-processing error bits in K 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.

kppErrBits lasYselJSourceRemeasurement WSA additional WFAU post-processing error bits in K 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.

kppErrBits uhsSource, uhsSourceAll WSAUHS additional WFAU post-processing error bits in K 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.

kprobVar 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.

kprobVar dxsVariability, gcsVariability, gpsVariability, 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.

kPsfMag calSource WSACalib Point source profile-fitted K mag real 4 mag -0.9999995e9 PHOT_MAG

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

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

kPsfMag uhsSource, uhsSourceAll WSAUHS Point source profile-fitted K mag real 4 mag -0.9999995e9 PHOT_MAG

kPsfMagErr calSource WSACalib Error in point source profile-fitted K mag real 4 mag -0.9999995e9 ERROR

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

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

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

kronFlux Detection PS1DR2 Kron (1980) flux. real 4 Janskys -999

kronFlux UKIDSSDetection WSA flux within circular aperture to k × r_k ; k = 2 real 4 ADU PHOT_INTENSITY_ADU

kronFlux calDetection WSACalib flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU PHOT_INTENSITY_ADU

kronFlux dxsDetection, gcsDetection, gpsDetection, lasDetection WSA flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU PHOT_INTENSITY_ADU

kronFlux lasMapRemeasurement WSA flux within Kron radius circular aperture (SE: FLUX_AUTO; CASU: default) {catalogue TType keyword: Kron_flux} real 4 ADU phot.count

kronFlux ptsDetection WSATransit flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU PHOT_INTENSITY_ADU

kronFlux udsDetection WSA flux within Kron radius circular aperture (SE: FLUX_AUTO) {catalogue TType keyword: Kron_flux} real 4 ADU PHOT_INTENSITY_ADU

kronFlux uhsDetection, uhsDetectionAll WSAUHS flux within circular aperture to k × r_k ; k = 2 {catalogue TType keyword: Kron_flux} real 4 ADU PHOT_INTENSITY_ADU

kronFluxErr Detection PS1DR2 Error on Kron (1980) flux. real 4 Janskys -999

kronFluxErr UKIDSSDetection WSA error on Kron flux real 4 ADU ERROR

kronFluxErr calDetection WSACalib error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU ERROR

kronFluxErr dxsDetection, gcsDetection, gpsDetection, lasDetection WSA error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU ERROR

kronFluxErr lasMapRemeasurement WSA error on Kron flux (SE: FLUXERR_AUTO; CASU: default) {catalogue TType keyword: Kron_flux_err} real 4 ADU stat.error

kronFluxErr ptsDetection WSATransit error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU ERROR

kronFluxErr udsDetection WSA error on Kron flux (SE: FLUXERR_AUTO) {catalogue TType keyword: Kron_flux_err} real 4 ADU ERROR

kronFluxErr uhsDetection, uhsDetectionAll WSAUHS error on Kron flux {catalogue TType keyword: Kron_flux_err} real 4 ADU ERROR

kronJky lasMapRemeasurement WSA Calibrated Kron flux within aperture r_k (CASU: default) real 4 jansky phot.mag

kronJkyErr lasMapRemeasurement WSA error on calibrated Kron flux real 4 jansky (CASU: default) stat.error

kronLup lasMapRemeasurement WSA Calibrated Kron luptitude within aperture r_k (CASU: default) real 4 lup phot.mag

kronLupErr lasMapRemeasurement WSA error on calibrated Kron luptitude real 4 lup (CASU: default) stat.error

kronMag dxsDetection, gcsDetection, gpsDetection, lasDetection, UKIDSSDetection, udsDetection WSA Calibrated Kron magnitude within circular aperture r_k real 4 mag PHOT_INT-MAG

kronMag calDetection WSACalib Calibrated Kron magnitude within circular aperture r_k real 4 mag PHOT_INT-MAG

kronMag lasMapRemeasurement WSA Calibrated Kron magnitude within aperture r_k (CASU: default) real 4 mag phot.mag

kronMag ptsDetection WSATransit Calibrated Kron magnitude within circular aperture r_k real 4 mag PHOT_INT-MAG

kronMag uhsDetection, uhsDetectionAll WSAUHS Calibrated Kron magnitude within circular aperture r_k real 4 mag PHOT_INT-MAG

kronMagErr dxsDetection, gcsDetection, gpsDetection, lasDetection, UKIDSSDetection, udsDetection WSA error on calibrated Kron magnitude real 4 mag ERROR

kronMagErr calDetection WSACalib error on calibrated Kron magnitude real 4 mag ERROR

kronMagErr lasMapRemeasurement WSA error on calibrated Kron magnitude real 4 mag (CASU: default) stat.error

kronMagErr ptsDetection WSATransit error on calibrated Kron magnitude real 4 mag ERROR

kronMagErr uhsDetection, uhsDetectionAll WSAUHS error on calibrated Kron magnitude real 4 mag ERROR

kronRad Detection PS1DR2 Kron (1980) radius. real 4 arcsec -999

kronRad UKIDSSDetection WSA r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 real 4 pixels EXTENSION_RAD

kronRad calDetection WSACalib r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels EXTENSION_RAD

kronRad dxsDetection, gcsDetection, gpsDetection, lasDetection WSA r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels EXTENSION_RAD

kronRad lasMapRemeasurement WSA Kron radius as defined in SE by Graham and Driver (2005) (SE: KRON_RADIUS*A_IMAGE; CASU: default) {catalogue TType keyword: Kron_radius}
r_k = ∑R² I(R) / ∑R I(R) real 4 pixels phys.angSize

Since <FLUX>_RADIUS is expressed in multiples of the major axis, <FLUX>_RADIUS is multiplied by A_IMAGE to convert to pixels.

kronRad ptsDetection WSATransit r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels EXTENSION_RAD

kronRad udsDetection WSA Kron radius as defined in SE by Graham and Driver (2005) (SE: KRON_RADIUS*A_IMAGE) {catalogue TType keyword: Kron_radius}
r_k = ∑R² I(R) / ∑R I(R) real 4 pixels EXTENSION_RAD

Since <FLUX>_RADIUS is expressed in multiples of the major axis, <FLUX>_RADIUS is multiplied by A_IMAGE to convert to pixels.

kronRad uhsDetection, uhsDetectionAll WSAUHS r_k as defined in Bertin and Arnouts 1996 A&A Supp 117 393 {catalogue TType keyword: Kron_radius} real 4 pixels EXTENSION_RAD

kSeqNum calSource, calSynopticSource WSACalib the running number of the K detection int 4 -99999999 ID_NUMBER

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

kSeqNum uhsSource, uhsSourceAll WSAUHS the running number of the K detection int 4 -99999999 ID_NUMBER

kSerMag2D calSource WSACalib Extended source K mag (profile-fitted) real 4 mag -0.9999995e9 PHOT_MAG

kSerMag2D dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource WSA Extended source K mag (profile-fitted) real 4 mag -0.9999995e9 PHOT_MAG

kSerMag2D reliableUdsSource, udsSource WSA Not available in SE output real 4 mag -0.9999995e9 PHOT_MAG

kSerMag2D uhsSource, uhsSourceAll WSAUHS Extended source K mag (profile-fitted) real 4 mag -0.9999995e9 PHOT_MAG

kSerMag2DErr calSource WSACalib Error in extended source K mag (profile-fitted) real 4 mag -0.9999995e9 ERROR

kSerMag2DErr dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource WSA Error in extended source K mag (profile-fitted) real 4 mag -0.9999995e9 ERROR

kSerMag2DErr reliableUdsSource, udsSource WSA Not available in SE output real 4 mag -0.9999995e9 ERROR

kSerMag2DErr uhsSource, uhsSourceAll WSAUHS Error in extended source K mag (profile-fitted) real 4 mag -0.9999995e9 ERROR

kskewness calVariability WSACalib Skewness in K 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.

kskewness dxsVariability, gcsVariability, gpsVariability, udsVariability WSA Skewness in K 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.

ktotalPeriod 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.

ktotalPeriod dxsVariability, gcsVariability, gpsVariability, 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.

kurtosis phot_variable_time_series_g_fov_statistical_parameters GAIADR1 Standardized unweighted kurtosis of the G-band time series values float 8 stat.value

kVarClass 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.

kVarClass dxsVariability, gcsVariability, gpsVariability, 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.

kXi calSource, calSynopticSource WSACalib Offset of K 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.

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

kXi dxsSource, gcsSource, gpsSource, lasSource, udsSource WSA Offset of K 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.

kXi uhsSource, uhsSourceAll WSAUHS Offset of K 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