WSA Browser

Glossary of WSA attributes

This Glossary alphabetically lists all attributes used in the UKIDSSDR9 database(s) held in the WSA. If you would like to have more information about the schema tables please use the UKIDSSDR9 Schema Browser (other Browser versions).

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

H

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

h2AperMag1 calSynopticSource WSACalib Extended source H2 aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

h2AperMag1 gpsJHKsource, gpsPointSource, gpsSource, reliableGpsPointSource WSA Extended source H2 aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

h2AperMag1Err calSynopticSource WSACalib Error in extended source H2 mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

h2AperMag1Err gpsJHKsource, gpsPointSource, gpsSource, reliableGpsPointSource WSA Error in extended source H2 mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

h2AperMag2 calSynopticSource WSACalib Extended source H2 aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

h2AperMag2Err calSynopticSource WSACalib Error in extended source H2 mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

h2AperMag3 calSource WSACalib Default point/extended source H2 aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

h2AperMag3 calSynopticSource WSACalib Default point/extended source H2 aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

h2AperMag3 gpsJHKsource, gpsPointSource, reliableGpsPointSource WSA Default point/extended source H2 aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

h2AperMag3 gpsSource WSA Default point/extended source H2 aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

h2AperMag3Err calSource, calSynopticSource WSACalib Error in default point/extended source H2 mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

h2AperMag3Err gpsJHKsource, gpsPointSource, gpsSource, reliableGpsPointSource WSA Error in default point/extended source H2 mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

h2AperMag4 calSource, calSynopticSource WSACalib Extended source H2 aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

h2AperMag4 gpsJHKsource, gpsPointSource, gpsSource, reliableGpsPointSource WSA Extended source H2 aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

h2AperMag4Err calSource, calSynopticSource WSACalib Error in extended source H2 mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

h2AperMag4Err gpsJHKsource, gpsPointSource, gpsSource, reliableGpsPointSource WSA Error in extended source H2 mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

h2AperMag5 calSynopticSource WSACalib Extended source H2 aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

h2AperMag5Err calSynopticSource WSACalib Error in extended source H2 mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

h2AperMag6 calSource WSACalib Extended source H2 aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

h2AperMag6Err calSource WSACalib Error in extended source H2 mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

h2aStratAst calVarFrameSetInfo WSACalib Strateva parameter, a, in fit to astrometric rms vs magnitude in H2 band, see Sesar et al. 2007. real 4 -0.9999995e9

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

h2aStratPht calVarFrameSetInfo WSACalib Strateva parameter, a, in fit to photmetric rms vs magnitude in H2 band, see Sesar et al. 2007. real 4 -0.9999995e9

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

h2bestAper calVariability WSACalib Best aperture (1-6) for photometric statistics in the H2 band int 4 -9999

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

h2bStratAst calVarFrameSetInfo WSACalib Strateva parameter, b, in fit to astrometric rms vs magnitude in H2 band, see Sesar et al. 2007. real 4 -0.9999995e9

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

h2bStratPht calVarFrameSetInfo WSACalib Strateva parameter, b, in fit to photometric rms vs magnitude in H2 band, see Sesar et al. 2007. real 4 -0.9999995e9

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

h2chiSqAst calVarFrameSetInfo WSACalib Goodness of fit of Strateva function to astrometric data in H2 band real 4 -0.9999995e9

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

h2chiSqpd 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.

h2chiSqPht calVarFrameSetInfo WSACalib Goodness of fit of Strateva function to photometric data in H2 band real 4 -0.9999995e9

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

h2Class calSource, calSourceRemeasurement, calSynopticSource WSACalib discrete image classification flag in H2 smallint 2 -9999 CLASS_MISC

h2Class gpsJHKsource, gpsPointSource, gpsSource, gpsSourceRemeasurement, reliableGpsPointSource WSA discrete image classification flag in H2 smallint 2 -9999 CLASS_MISC

h2ClassStat calSource, calSourceRemeasurement, calSynopticSource WSACalib N(0,1) stellarness-of-profile statistic in H2 real 4 -0.9999995e9 STAT_PROP

h2ClassStat gpsJHKsource, gpsPointSource, gpsSource, reliableGpsPointSource WSA S-Extractor classification statistic in H2 real 4 -0.9999995e9 STAT_PROP

h2ClassStat gpsSourceRemeasurement WSA N(0,1) stellarness-of-profile statistic in H2 real 4 -0.9999995e9 STAT_PROP

h2cStratAst calVarFrameSetInfo WSACalib Strateva parameter, c, in fit to astrometric rms vs magnitude in H2 band, see Sesar et al. 2007. real 4 -0.9999995e9

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

h2cStratPht calVarFrameSetInfo WSACalib Strateva parameter, c, in fit to photometric rms vs magnitude in H2 band, see Sesar et al. 2007. real 4 -0.9999995e9

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

h2Deblend calSource WSACalib placeholder flag indicating parent/child relation in H2 int 4 -99999999 CODE_MISC

This CASU pipeline processing source extraction flag is a placeholder only, and is always set to zero in all passbands in the merged source lists. If you need to know when a particular image detection is a component of a deblend or not, test bit 4 of attribute ppErrBits (see corresponding glossary entry) which is set by WFAU's post-processing software based on testing the areal profiles aprof2-8 (these are set by CASU to -1 for deblended components, or positive values for non-deblended detections). We encode this in an information bit of ppErrBits for convenience when querying the merged source tables.

h2Deblend calSourceRemeasurement, calSynopticSource WSACalib placeholder flag indicating parent/child relation in H2 int 4 -99999999 CODE_MISC

h2Deblend gpsJHKsource, gpsPointSource, gpsSource, gpsSourceRemeasurement, reliableGpsPointSource WSA placeholder flag indicating parent/child relation in H2 int 4 -99999999 CODE_MISC

h2Ell calSource, calSourceRemeasurement, calSynopticSource WSACalib 1-b/a, where a/b=semi-major/minor axes in H2 real 4 -0.9999995e9 PHYS_ELLIPTICITY

h2Ell gpsJHKsource, gpsPointSource, gpsSource, gpsSourceRemeasurement, reliableGpsPointSource WSA 1-b/a, where a/b=semi-major/minor axes in H2 real 4 -0.9999995e9 PHYS_ELLIPTICITY

h2eNum calMergeLog, calSynopticMergeLog WSACalib the extension number of this H2 frame tinyint 1 NUMBER

h2eNum gpsJHKmergeLog, gpsMergeLog WSA the extension number of this H2 frame tinyint 1 NUMBER

h2ErrBits calSource, calSynopticSource WSACalib processing warning/error bitwise flags in H2 int 4 -99999999 CODE_MISC

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

h2ErrBits calSourceRemeasurement WSACalib processing warning/error bitwise flags in H2 int 4 -99999999 CODE_MISC

h2ErrBits gpsJHKsource, gpsPointSource, gpsSourceRemeasurement, reliableGpsPointSource WSA processing warning/error bitwise flags in H2 int 4 -99999999 CODE_MISC

h2ErrBits gpsSource WSA processing warning/error bitwise flags in H2 int 4 -99999999 CODE_MISC

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

Bit Flag Meaning

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

2 The object was originally blended with another

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

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

16 Object's aperture data are incomplete or corrupted

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

64 Memory overflow occurred during deblending

128 Memory overflow occurred during extraction

h2Eta calSource, calSynopticSource WSACalib Offset of H2 detection from master position (+north/-south) real 4 arcsec -0.9999995e9 POS_EQ_DEC_OFF

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

h2Eta gpsJHKsource, gpsPointSource, reliableGpsPointSource WSA Offset of H2 detection from master position (+north/-south) real 4 arcsec -0.9999995e9 POS_EQ_DEC_OFF

h2Eta gpsSource WSA Offset of H2 detection from master position (+north/-south) real 4 arcsec -0.9999995e9 POS_EQ_DEC_OFF

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 2.0 (UKIDSS LAS and GPS; also non-survey programmes) or 1.0 (UKIDSS GPS, DXS and UDS) arcseconds is used, the higher value enabling pairing of moving sources when epoch separations may be several years. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the LAS, you might wish to insist that the offsets in the selected sample are all below 1 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

h2expML calVarFrameSetInfo WSACalib Expected magnitude limit of frameSet in this in H2 band. real 4 -0.9999995e9

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

h2ExpRms calVariability WSACalib Rms calculated from polynomial fit to modal RMS as a function of magnitude in H2 band real 4 mag -0.9999995e9

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

h2Gausig calSource, calSourceRemeasurement, calSynopticSource WSACalib RMS of axes of ellipse fit in H2 real 4 pixels -0.9999995e9 MORPH_PARAM

h2Gausig gpsJHKsource, gpsPointSource, gpsSource, gpsSourceRemeasurement, reliableGpsPointSource WSA RMS of axes of ellipse fit in H2 real 4 pixels -0.9999995e9 MORPH_PARAM

h2HallMag calSource WSACalib Total point source H2 mag real 4 mag -0.9999995e9 PHOT_MAG

h2HallMagErr calSource WSACalib Error in total point source H2 mag real 4 mag -0.9999995e9 ERROR

h2IntRms calVariability WSACalib Intrinsic rms in H2-band real 4 mag -0.9999995e9

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

h2Mag calSourceRemeasurement WSACalib H2 mag (as appropriate for this merged source) real 4 mag -0.9999995e9 PHOT_MAG

h2Mag gpsSourceRemeasurement WSA H2 mag (as appropriate for this merged source) real 4 mag -0.9999995e9 PHOT_MAG

h2MagErr calSourceRemeasurement WSACalib Error in H2 mag real 4 mag -0.9999995e9 ERROR

h2MagErr gpsSourceRemeasurement WSA Error in H2 mag real 4 mag -0.9999995e9 ERROR

h2MagMAD calVariability WSACalib Median Absolute Deviation of H2 magnitude real 4 mag -0.9999995e9

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

h2MagRms calVariability WSACalib rms of H2 magnitude real 4 mag -0.9999995e9

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

h2maxCadence 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.

h2MaxMag calVariability WSACalib Maximum magnitude in H2 band, of good detections real 4 -0.9999995e9

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

h2mbrPnt calSynopticSource WSACalib Point source colour H2-Br (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

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

h2mbrPntErr calSynopticSource WSACalib Error on point source colour H2-Br real 4 mag -0.9999995e9 ERROR

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

h2meanMag calVariability WSACalib Mean H2 magnitude real 4 mag -0.9999995e9

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

h2medCadence 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.

h2medianMag calVariability WSACalib Median H2 magnitude real 4 mag -0.9999995e9

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

h2mfID calMergeLog, calSynopticMergeLog WSACalib the UID of the relevant H2 multiframe bigint 8 ID_FRAME

h2mfID gpsJHKmergeLog, gpsMergeLog WSA the UID of the relevant H2 multiframe bigint 8 ID_FRAME

h2minCadence 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.

h2MinMag calVariability WSACalib real 4 -0.9999995e9

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

h2mk_1 gpsSourceRemeasurement WSA Default colour H2-K (using appropriate mags) real 4 mag PHOT_COLOR

h2mk_1Err gpsSourceRemeasurement WSA Error on colour H2-K real 4 mag ERROR

h2mk_1Pnt gpsJHKsource, gpsPointSource, reliableGpsPointSource WSA Point source colour H2-K (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

h2mk_1Pnt gpsSource WSA Point source colour H2-K (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

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

h2mk_1PntErr gpsJHKsource, gpsPointSource, reliableGpsPointSource WSA Error on point source colour H2-K real 4 mag -0.9999995e9 ERROR

h2mk_1PntErr gpsSource WSA Error on point source colour H2-K real 4 mag -0.9999995e9 ERROR

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

h2mkPnt calSynopticSource WSACalib Point source colour H2-K (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

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

h2mkPntErr calSynopticSource WSACalib Error on point source colour H2-K real 4 mag -0.9999995e9 ERROR

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

h2ndof calVariability WSACalib Number of degrees of freedom for chisquare int 4 -99999999

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

h2nDofAst calVarFrameSetInfo WSACalib Number of degrees of freedom of astrometric fit in H2 band. smallint 2 -9999

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

h2nDofPht calVarFrameSetInfo WSACalib Number of degrees of freedom of photometric fit in H2 band. smallint 2 -9999

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

h2nFlaggedObs calVariability WSACalib Number of detections in H2 band flagged as potentially spurious by calDetection.ppErrBits int 4 0

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

h2nGoodObs calVariability WSACalib Number of good detections in H2 band int 4 0

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

h2Ngt3sig calVariability WSACalib Number of good detections in H2-band that are more than 3 sigma deviations smallint 2 -9999

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

h2nMissingObs calVariability WSACalib Number of H2 band frames that this object should have been detected on and was not int 4 0

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

h2ObjID calSource, calSourceRemeasurement, calSynopticSource WSACalib DEPRECATED (do not use) bigint 8 -99999999 ID_NUMBER

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

h2ObjID gpsJHKsource, gpsPointSource, reliableGpsPointSource WSA DEPRECATED (do not use) bigint 8 -99999999 ID_NUMBER

h2ObjID gpsSource, gpsSourceRemeasurement WSA DEPRECATED (do not use) bigint 8 -99999999 ID_NUMBER

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

h2PA calSource, calSourceRemeasurement, calSynopticSource WSACalib ellipse fit celestial orientation in H2 real 4 Degrees -0.9999995e9 POS_POS-ANG

h2PA gpsJHKsource, gpsPointSource, gpsSource, gpsSourceRemeasurement, reliableGpsPointSource WSA ellipse fit celestial orientation in H2 real 4 Degrees -0.9999995e9 POS_POS-ANG

h2PetroMag calSource WSACalib Extended source H2 mag (Petrosian) real 4 mag -0.9999995e9 PHOT_MAG

h2PetroMagErr calSource WSACalib Error in extended source H2 mag (Petrosian) real 4 mag -0.9999995e9 ERROR

h2ppErrBits calSource, calSynopticSource WSACalib additional WFAU post-processing error bits in H2 int 4 0 CODE_MISC

Post-processing error quality bit flags assigned (NB: from UKIDSS DR2 release onwards) in the WSA curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

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

1 15 Source in poor flat field region 32768 0x00008000 All but mosaics

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues (though deeps excluded prior to DR8)

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 GPS only

2 19 Possible crosstalk artefact/contamination 524288 0x00080000 All but GPS

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All but mosaics

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all K band sources in the LAS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

h2ppErrBits calSourceRemeasurement WSACalib additional WFAU post-processing error bits in H2 int 4 0 CODE_MISC

h2ppErrBits gpsJHKsource, gpsPointSource, gpsSource, gpsSourceRemeasurement, reliableGpsPointSource WSA additional WFAU post-processing error bits in H2 int 4 0 CODE_MISC

h2probVar 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.

h2PsfMag calSource WSACalib Point source profile-fitted H2 mag real 4 mag -0.9999995e9 PHOT_MAG

h2PsfMagErr calSource WSACalib Error in point source profile-fitted H2 mag real 4 mag -0.9999995e9 ERROR

h2SeqNum calSource, calSynopticSource WSACalib the running number of the H2 detection int 4 -99999999 ID_NUMBER

h2SeqNum calSourceRemeasurement WSACalib the running number of the H2 remeasurement int 4 -99999999 ID_NUMBER

h2SeqNum gpsJHKsource, gpsPointSource, gpsSource, reliableGpsPointSource WSA the running number of the H2 detection int 4 -99999999 ID_NUMBER

h2SeqNum gpsSourceRemeasurement WSA the running number of the H2 remeasurement int 4 -99999999 ID_NUMBER

h2SerMag2D calSource WSACalib Extended source H2 mag (profile-fitted) real 4 mag -0.9999995e9 PHOT_MAG

h2SerMag2DErr calSource WSACalib Error in extended source H2 mag (profile-fitted) real 4 mag -0.9999995e9 ERROR

h2skewness calVariability WSACalib Skewness in H2 band (see Sesar et al. 2007) real 4 -0.9999995e9

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

h2totalPeriod 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.

h2VarClass 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.

h2Xi calSource, calSynopticSource WSACalib Offset of H2 detection from master position (+east/-west) real 4 arcsec -0.9999995e9 POS_EQ_RA_OFF

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

h2Xi gpsJHKsource, gpsPointSource, reliableGpsPointSource WSA Offset of H2 detection from master position (+east/-west) real 4 arcsec -0.9999995e9 POS_EQ_RA_OFF

h2Xi gpsSource WSA Offset of H2 detection from master position (+east/-west) real 4 arcsec -0.9999995e9 POS_EQ_RA_OFF

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

h_2mrat twomass_scn 2MASS H-band average 2nd image moment ratio. real 4 FIT_PARAM_VALUE

h_2mrat twomass_sixx2_scn 2MASS H band average 2nd image moment ratio for scan real 4

h_5sig_ba twomass_xsc 2MASS H minor/major axis ratio fit to the 5-sigma isophote. real 4 PHYS_AXIS-RATIO

h_5sig_phi twomass_xsc 2MASS H angle to 5-sigma major axis (E of N). smallint 2 degrees ERROR

h_5surf twomass_xsc 2MASS H central surface brightness (r<=5). real 4 mag PHOT_SB_GENERAL

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

h_back twomass_xsc 2MASS H coadd median background. real 4 CODE_MISC

h_bisym_chi twomass_xsc 2MASS H bi-symmetric cross-correlation chi. real 4 FIT_PARAM_VALUE

h_bisym_rat twomass_xsc 2MASS H bi-symmetric flux ratio. real 4 PHOT_FLUX_RATIO

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

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

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

h_con_indx twomass_xsc 2MASS H concentration index r_75%/r_25%. real 4 PHYS_CONCENT_INDEX

h_d_area twomass_xsc 2MASS H 5-sigma to 3-sigma differential area. smallint 2 FIT_RESIDUAL

h_flg_10 twomass_xsc 2MASS H confusion flag for 10 arcsec circular ap. mag. smallint 2 CODE_MISC

h_flg_15 twomass_xsc 2MASS H confusion flag for 15 arcsec circular ap. mag. smallint 2 CODE_MISC

h_flg_20 twomass_xsc 2MASS H confusion flag for 20 arcsec circular ap. mag. smallint 2 CODE_MISC

h_flg_25 twomass_xsc 2MASS H confusion flag for 25 arcsec circular ap. mag. smallint 2 CODE_MISC

h_flg_30 twomass_xsc 2MASS H confusion flag for 30 arcsec circular ap. mag. smallint 2 CODE_MISC

h_flg_40 twomass_xsc 2MASS H confusion flag for 40 arcsec circular ap. mag. smallint 2 CODE_MISC

h_flg_5 twomass_xsc 2MASS H confusion flag for 5 arcsec circular ap. mag. smallint 2 CODE_MISC

h_flg_50 twomass_xsc 2MASS H confusion flag for 50 arcsec circular ap. mag. smallint 2 CODE_MISC

h_flg_60 twomass_xsc 2MASS H confusion flag for 60 arcsec circular ap. mag. smallint 2 CODE_MISC

h_flg_7 twomass_sixx2_xsc 2MASS H confusion flag for 7 arcsec circular ap. mag smallint 2

h_flg_7 twomass_xsc 2MASS H confusion flag for 7 arcsec circular ap. mag. smallint 2 CODE_MISC

h_flg_70 twomass_xsc 2MASS H confusion flag for 70 arcsec circular ap. mag. smallint 2 CODE_MISC

h_flg_c twomass_xsc 2MASS H confusion flag for Kron circular mag. smallint 2 CODE_MISC

h_flg_e twomass_xsc 2MASS H confusion flag for Kron elliptical mag. smallint 2 CODE_MISC

h_flg_fc twomass_xsc 2MASS H confusion flag for fiducial Kron circ. mag. smallint 2 CODE_MISC

h_flg_fe twomass_xsc 2MASS H confusion flag for fiducial Kron ell. mag. smallint 2 CODE_MISC

h_flg_i20c twomass_xsc 2MASS H confusion flag for 20mag/sq." iso. circ. mag. smallint 2 CODE_MISC

h_flg_i20e twomass_xsc 2MASS H confusion flag for 20mag/sq." iso. ell. mag. smallint 2 CODE_MISC

h_flg_i21c twomass_xsc 2MASS H confusion flag for 21mag/sq." iso. circ. mag. smallint 2 CODE_MISC

h_flg_i21e twomass_xsc 2MASS H confusion flag for 21mag/sq." iso. ell. mag. smallint 2 CODE_MISC

h_flg_j21fc twomass_xsc 2MASS H confusion flag for 21mag/sq." iso. fid. circ. mag. smallint 2 CODE_MISC

h_flg_j21fe twomass_xsc 2MASS H confusion flag for 21mag/sq." iso. fid. ell. mag. smallint 2 CODE_MISC

h_flg_k20fc twomass_xsc 2MASS H confusion flag for 20mag/sq." iso. fid. circ. mag. smallint 2 CODE_MISC

h_flg_k20fe twomass_sixx2_xsc 2MASS H confusion flag for 20mag/sq.″ iso. fid. ell. mag smallint 2

h_flg_k20fe twomass_xsc 2MASS H confusion flag for 20mag/sq." iso. fid. ell. mag. smallint 2 CODE_MISC

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

h_m twomass_psc 2MASS Default H-band magnitude real 4 mag SPECT_FLUX_VALUE

h_m twomass_sixx2_psc 2MASS H selected "default" magnitude real 4 mag

h_m_10 twomass_xsc 2MASS H 10 arcsec radius circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

h_m_15 twomass_xsc 2MASS H 15 arcsec radius circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

h_m_20 twomass_xsc 2MASS H 20 arcsec radius circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

h_m_25 twomass_xsc 2MASS H 25 arcsec radius circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

h_m_2mass wise_prelimsc WISE 2MASS H-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 H-band magnitude entry is default real 4 mag -0.9999995e9

h_m_30 twomass_xsc 2MASS H 30 arcsec radius circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

h_m_40 twomass_xsc 2MASS H 40 arcsec radius circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

h_m_5 twomass_xsc 2MASS H 5 arcsec radius circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

h_m_50 twomass_xsc 2MASS H 50 arcsec radius circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

h_m_60 twomass_xsc 2MASS H 60 arcsec radius circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

h_m_7 twomass_sixx2_xsc 2MASS H 7 arcsec radius circular aperture magnitude real 4 mag

h_m_7 twomass_xsc 2MASS H 7 arcsec radius circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

h_m_70 twomass_xsc 2MASS H 70 arcsec radius circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

h_m_c twomass_xsc 2MASS H Kron circular aperture magnitude. real 4 mag SPECT_FLUX_VALUE

h_m_e twomass_xsc 2MASS H Kron elliptical aperture magnitude. real 4 mag SPECT_FLUX_VALUE

h_m_ext twomass_sixx2_xsc 2MASS H mag from fit extrapolation real 4 mag

h_m_ext twomass_xsc 2MASS H mag from fit extrapolation. real 4 mag SPECT_FLUX_VALUE

h_m_fc twomass_xsc 2MASS H fiducial Kron circular magnitude. real 4 mag SPECT_FLUX_VALUE

h_m_fe twomass_xsc 2MASS H fiducial Kron ell. mag aperture magnitude. real 4 mag SPECT_FLUX_VALUE

h_m_i20c twomass_xsc 2MASS H 20mag/sq." isophotal circular ap. magnitude. real 4 mag SPECT_FLUX_VALUE

h_m_i20e twomass_xsc 2MASS H 20mag/sq." isophotal elliptical ap. magnitude. real 4 mag SPECT_FLUX_VALUE

h_m_i21c twomass_xsc 2MASS H 21mag/sq." isophotal circular ap. magnitude. real 4 mag SPECT_FLUX_VALUE

h_m_i21e twomass_xsc 2MASS H 21mag/sq." isophotal elliptical ap. magnitude. real 4 mag SPECT_FLUX_VALUE

h_m_j21fc twomass_xsc 2MASS H 21mag/sq." isophotal fiducial circ. ap. mag. real 4 mag SPECT_FLUX_VALUE

h_m_j21fe twomass_xsc 2MASS H 21mag/sq." isophotal fiducial ell. ap. magnitude. real 4 mag SPECT_FLUX_VALUE

h_m_k20fc twomass_xsc 2MASS H 20mag/sq." isophotal fiducial circ. ap. mag. real 4 mag SPECT_FLUX_VALUE

h_m_k20fe twomass_sixx2_xsc 2MASS H 20mag/sq.″ isophotal fiducial ell. ap. magnitude real 4 mag

h_m_k20fe twomass_xsc 2MASS H 20mag/sq." isophotal fiducial ell. ap. magnitude. real 4 mag SPECT_FLUX_VALUE

h_m_stdap twomass_psc 2MASS H-band "standard" aperture magnitude. real 4 mag SPECT_FLUX_VALUE

h_m_sys twomass_xsc 2MASS H system photometry magnitude. real 4 mag SPECT_FLUX_VALUE

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

h_msig twomass_sixx2_psc 2MASS H "default" mag uncertainty real 4 mag

h_msig_10 twomass_xsc 2MASS H 1-sigma uncertainty in 10 arcsec circular ap. mag. real 4 mag ERROR

h_msig_15 twomass_xsc 2MASS H 1-sigma uncertainty in 15 arcsec circular ap. mag. real 4 mag ERROR

h_msig_20 twomass_xsc 2MASS H 1-sigma uncertainty in 20 arcsec circular ap. mag. real 4 mag ERROR

h_msig_25 twomass_xsc 2MASS H 1-sigma uncertainty in 25 arcsec circular ap. mag. real 4 mag ERROR

h_msig_2mass wise_prelimsc WISE 2MASS H-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 H-band uncertainty entry is default real 4 mag -0.9999995e9

h_msig_30 twomass_xsc 2MASS H 1-sigma uncertainty in 30 arcsec circular ap. mag. real 4 mag ERROR

h_msig_40 twomass_xsc 2MASS H 1-sigma uncertainty in 40 arcsec circular ap. mag. real 4 mag ERROR

h_msig_5 twomass_xsc 2MASS H 1-sigma uncertainty in 5 arcsec circular ap. mag. real 4 mag ERROR

h_msig_50 twomass_xsc 2MASS H 1-sigma uncertainty in 50 arcsec circular ap. mag. real 4 mag ERROR

h_msig_60 twomass_xsc 2MASS H 1-sigma uncertainty in 60 arcsec circular ap. mag. real 4 mag ERROR

h_msig_7 twomass_sixx2_xsc 2MASS H 1-sigma uncertainty in 7 arcsec circular ap. mag real 4 mag

h_msig_7 twomass_xsc 2MASS H 1-sigma uncertainty in 7 arcsec circular ap. mag. real 4 mag ERROR

h_msig_70 twomass_xsc 2MASS H 1-sigma uncertainty in 70 arcsec circular ap. mag. real 4 mag ERROR

h_msig_c twomass_xsc 2MASS H 1-sigma uncertainty in Kron circular mag. real 4 mag ERROR

h_msig_e twomass_xsc 2MASS H 1-sigma uncertainty in Kron elliptical mag. real 4 mag ERROR

h_msig_ext twomass_sixx2_xsc 2MASS H 1-sigma uncertainty in mag from fit extrapolation real 4 mag

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

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

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

h_msig_i20c twomass_xsc 2MASS H 1-sigma uncertainty in 20mag/sq." iso. circ. mag. real 4 mag ERROR

h_msig_i20e twomass_xsc 2MASS H 1-sigma uncertainty in 20mag/sq." iso. ell. mag. real 4 mag ERROR

h_msig_i21c twomass_xsc 2MASS H 1-sigma uncertainty in 21mag/sq." iso. circ. mag. real 4 mag ERROR

h_msig_i21e twomass_xsc 2MASS H 1-sigma uncertainty in 21mag/sq." iso. ell. mag. real 4 mag ERROR

h_msig_j21fc twomass_xsc 2MASS H 1-sigma uncertainty in 21mag/sq." iso.fid.circ.mag. real 4 mag ERROR

h_msig_j21fe twomass_xsc 2MASS H 1-sigma uncertainty in 21mag/sq." iso.fid.ell.mag. real 4 mag ERROR

h_msig_k20fc twomass_xsc 2MASS H 1-sigma uncertainty in 20mag/sq." iso.fid.circ. mag. real 4 mag ERROR

h_msig_k20fe twomass_sixx2_xsc 2MASS H 1-sigma uncertainty in 20mag/sq.″ iso.fid.ell.mag real 4 mag

h_msig_k20fe twomass_xsc 2MASS H 1-sigma uncertainty in 20mag/sq." iso.fid.ell.mag. real 4 mag ERROR

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

h_msig_sys twomass_xsc 2MASS H 1-sigma uncertainty in system photometry mag. real 4 mag ERROR

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

h_msigcom twomass_sixx2_psc 2MASS combined (total) H band photometric uncertainty real 4 mag

h_msnr10 twomass_scn 2MASS The estimated H-band magnitude at which SNR=10 is achieved for this scan. real 4 mag SPECT_FLUX_VALUE

h_msnr10 twomass_sixx2_scn 2MASS H mag at which SNR=10 is achieved, from h_psp and h_zp_ap real 4 mag

h_n_snr10 twomass_scn 2MASS Number of point sources at H-band with SNR>10 (instrumental mag <=15.1) int 4 NUMBER

h_n_snr10 twomass_sixx2_scn 2MASS number of H point sources with SNR>10 (instrumental m<=15.1) int 4

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

h_peak twomass_xsc 2MASS H peak pixel brightness. real 4 mag PHOT_SB_GENERAL

h_perc_darea twomass_xsc 2MASS H 5-sigma to 3-sigma percent area change. smallint 2 FIT_PARAM

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

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

h_psp twomass_scn 2MASS H-band photometric sensitivity paramater (PSP). real 4 INST_SENSITIVITY

h_psp twomass_sixx2_scn 2MASS H photometric sensitivity param: h_shape_avg*(h_fbg_avg^.29) real 4

h_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 H-band photometric errors and is expressed in units of mJy. real 4 INST_NOISE

h_pts_noise twomass_sixx2_scn 2MASS log10 of H band modal point src noise estimate real 4 logmJy

h_r_c twomass_xsc 2MASS H Kron circular aperture radius. real 4 arcsec EXTENSION_RAD

h_r_e twomass_xsc 2MASS H Kron elliptical aperture semi-major axis. real 4 arcsec EXTENSION_RAD

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

h_r_i20c twomass_xsc 2MASS H 20mag/sq." isophotal circular aperture radius. real 4 arcsec EXTENSION_RAD

h_r_i20e twomass_xsc 2MASS H 20mag/sq." isophotal elliptical ap. semi-major axis. real 4 arcsec EXTENSION_RAD

h_r_i21c twomass_xsc 2MASS H 21mag/sq." isophotal circular aperture radius. real 4 arcsec EXTENSION_RAD

h_r_i21e twomass_xsc 2MASS H 21mag/sq." isophotal elliptical ap. semi-major axis. real 4 arcsec EXTENSION_RAD

h_resid_ann twomass_xsc 2MASS H residual annulus background median. real 4 DN CODE_MISC

h_sc_1mm twomass_xsc 2MASS H 1st moment (score) (LCSB: super blk 2,4,8 SNR). real 4 CODE_MISC

h_sc_2mm twomass_xsc 2MASS H 2nd moment (score) (LCSB: SNRMAX - super SNR max). real 4 CODE_MISC

h_sc_msh twomass_xsc 2MASS H median shape score. real 4 CODE_MISC

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

h_sc_r1 twomass_xsc 2MASS H r1 (score). real 4 CODE_MISC

h_sc_r23 twomass_xsc 2MASS H r23 (score) (LCSB: TSNR - integrated SNR for r=15). real 4 CODE_MISC

h_sc_sh twomass_xsc 2MASS H shape (score). real 4 CODE_MISC

h_sc_vint twomass_xsc 2MASS H vint (score). real 4 CODE_MISC

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

h_seetrack twomass_xsc 2MASS H band seetracking score. real 4 CODE_MISC

h_sh0 twomass_xsc 2MASS H ridge shape (LCSB: BSNR limit). real 4 FIT_PARAM

h_shape_avg twomass_scn 2MASS H-band average seeing shape for scan. real 4 INST_SEEING

h_shape_avg twomass_sixx2_scn 2MASS H band average seeing shape for scan real 4

h_shape_rms twomass_scn 2MASS RMS-error of H-band average seeing shape. real 4 INST_SEEING

h_shape_rms twomass_sixx2_scn 2MASS rms of H band avg seeing shape for scan real 4

h_sig_sh0 twomass_xsc 2MASS H ridge shape sigma (LCSB: B2SNR limit). real 4 FIT_PARAM

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

h_snr twomass_sixx2_psc 2MASS H band "scan" signal-to-noise ratio real 4

h_subst2 twomass_xsc 2MASS H residual background #2 (score). real 4 CODE_MISC

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

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

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

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

ha twomass_scn 2MASS Hour angle at beginning of scan. float 8 hr POS_POS-ANG

ha twomass_sixx2_scn 2MASS beginning hour angle of scan data float 8 hr

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

hallFlux calDetection, calListRemeasurement WSACalib flux within circular aperture to k × r_h; k = 5; alternative total flux {catalogue TType keyword: Hall_flux} real 4 ADU PHOT_INTENSITY_ADU

hallFlux dxsDetection, gcsDetection, gcsListRemeasurement, gpsDetection, gpsListRemeasurement, lasDetection, lasListRemeasurement, udsListRemeasurement WSA flux within circular aperture to k × r_h; k = 5; alternative total flux {catalogue TType keyword: Hall_flux} real 4 ADU PHOT_INTENSITY_ADU

hallFlux ptsDetection WSATransit flux within circular aperture to k × r_h; k = 5; alternative total flux {catalogue TType keyword: Hall_flux} real 4 ADU PHOT_INTENSITY_ADU

hallFlux udsDetection WSA Not available in SE output {catalogue TType keyword: Hall_flux} real 4 -0.9999995e9

hallFluxErr UKIDSSDetection WSA error on Hall flux real 4 ADU ERROR

hallFluxErr calDetection, calListRemeasurement WSACalib error on Hall flux {catalogue TType keyword: Hall_flux_err} real 4 ADU ERROR

hallFluxErr dxsDetection, gcsDetection, gcsListRemeasurement, gpsDetection, gpsListRemeasurement, lasDetection, lasListRemeasurement, udsListRemeasurement WSA error on Hall flux {catalogue TType keyword: Hall_flux_err} real 4 ADU ERROR

hallFluxErr ptsDetection WSATransit error on Hall flux {catalogue TType keyword: Hall_flux_err} real 4 ADU ERROR

hallFluxErr udsDetection WSA Not available in SE output {catalogue TType keyword: Hall_flux_err} real 4 -0.9999995e9

hallMag dxsDetection, gcsDetection, gcsListRemeasurement, gpsDetection, gpsListRemeasurement, lasDetection, lasListRemeasurement, UKIDSSDetection, udsListRemeasurement WSA Calibrated magnitude within circular aperture r_hall real 4 mag PHOT_INT-MAG

hallMag calDetection, calListRemeasurement WSACalib Calibrated magnitude within circular aperture r_hall real 4 mag PHOT_INT-MAG

hallMag ptsDetection WSATransit Calibrated magnitude within circular aperture r_hall real 4 mag PHOT_INT-MAG

hallMag udsDetection WSA Not available in SE output real 4 -0.9999995e9

hallMagErr dxsDetection, gcsDetection, gcsListRemeasurement, gpsDetection, gpsListRemeasurement, lasDetection, lasListRemeasurement, UKIDSSDetection, udsListRemeasurement WSA Calibrated error on Hall magnitude real 4 mag ERROR

hallMagErr calDetection, calListRemeasurement WSACalib Calibrated error on Hall magnitude real 4 mag ERROR

hallMagErr ptsDetection WSATransit Calibrated error on Hall magnitude real 4 mag ERROR

hallMagErr udsDetection WSA Not available in SE output real 4 -0.9999995e9

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

hallRad calDetection, calListRemeasurement WSACalib r_h image scale radius eg. Hall & Mackay 1984 MNRAS 210 979 {catalogue TType keyword: Hall_radius} real 4 pixels EXTENSION_RAD

hallRad dxsDetection, gcsDetection, gcsListRemeasurement, gpsDetection, gpsListRemeasurement, lasDetection, lasListRemeasurement, udsListRemeasurement WSA r_h image scale radius eg. Hall & Mackay 1984 MNRAS 210 979 {catalogue TType keyword: Hall_radius} real 4 pixels EXTENSION_RAD

hallRad ptsDetection WSATransit r_h image scale radius eg. Hall & Mackay 1984 MNRAS 210 979 {catalogue TType keyword: Hall_radius} real 4 pixels EXTENSION_RAD

hallRad udsDetection WSA Not available in SE output {catalogue TType keyword: Hall_radius} real 4 -0.9999995e9

hAperMag1 calSynopticSource WSACalib Extended source H aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

hAperMag1 gpsJHKsource, gpsPointSource, gpsSource, reliableGpsPointSource WSA Extended source H aperture corrected mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

hAperMag1Err calSynopticSource WSACalib Error in extended source H mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

hAperMag1Err gpsJHKsource, gpsPointSource, gpsSource, reliableGpsPointSource WSA Error in extended source H mag (1.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

hAperMag2 calSynopticSource WSACalib Extended source H aperture corrected mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

hAperMag2Err calSynopticSource WSACalib Error in extended source H mag (1.4 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

hAperMag3 calSource WSACalib Default point/extended source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

hAperMag3 calSynopticSource WSACalib Default point/extended source H aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

hAperMag3 dxsJKsource, gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, lasExtendedSource, lasPointSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource WSA Default point/extended source H aperture corrected mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

hAperMag3 dxsSource, gcsSource, gpsSource, lasSource WSA Default point/extended source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

hAperMag3 reliableUdsSource WSA Default point/extended source H mag, no aperture correction applied real 4 mag -0.9999995e9 PHOT_MAG

hAperMag3 udsSource WSA Default point/extended source H mag, no aperture correction applied
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

hAperMag3Err calSource, calSynopticSource WSACalib Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

hAperMag3Err dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource, udsSource WSA Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

hAperMag4 calSource, calSynopticSource WSACalib Extended source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

hAperMag4 dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource WSA Extended source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

hAperMag4 reliableUdsSource, udsSource WSA Extended source H mag, no aperture correction applied real 4 mag -0.9999995e9 PHOT_MAG

hAperMag4Err calSource, calSynopticSource WSACalib Error in extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

hAperMag4Err dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource, udsSource WSA Error in extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

hAperMag5 calSynopticSource WSACalib Extended source H aperture corrected mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

hAperMag5Err calSynopticSource WSACalib Error in extended source H mag (4.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

hAperMag6 calSource WSACalib Extended source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

hAperMag6 dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableLasPointSource WSA Extended source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

hAperMag6 reliableUdsSource, udsSource WSA Extended source H mag, no aperture correction applied real 4 mag -0.9999995e9 PHOT_MAG

hAperMag6Err calSource WSACalib Error in extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

hAperMag6Err dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableLasPointSource, reliableUdsSource, udsSource WSA Error in extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

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

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

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

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

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

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

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

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

haStratPht udsVarFrameSetInfo WSA Strateva parameter, a, in fit to photmetric rms vs magnitude in H band, see Sesar et al. 2007. real 4 -0.9999995e9

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

hchiSqAst dxsVarFrameSetInfo, udsVarFrameSetInfo WSA Goodness of fit of Strateva function to astrometric data in H band real 4 -0.9999995e9

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

hchiSqpd 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.

hchiSqpd dxsVariability, 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.

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

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

hchiSqPht dxsVarFrameSetInfo, udsVarFrameSetInfo WSA Goodness of fit of Strateva function to photometric data in H band real 4 -0.9999995e9

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

hClass calSource, calSourceRemeasurement, calSynopticSource WSACalib discrete image classification flag in H smallint 2 -9999 CLASS_MISC

hClass dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsSourceRemeasurement, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, gpsSourceRemeasurement, lasExtendedSource, lasPointSource, lasSource, lasSourceRemeasurement, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource, udsSource, udsSourceRemeasurement WSA discrete image classification flag in H smallint 2 -9999 CLASS_MISC

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

hClassStat dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsSourceRemeasurement, gcsZYJHKsource, gpsSourceRemeasurement, lasExtendedSource, lasPointSource, lasSource, lasSourceRemeasurement, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableLasPointSource, udsSourceRemeasurement WSA N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 STAT_PROP

hClassStat gpsJHKsource, gpsPointSource, gpsSource, reliableGpsPointSource, reliableUdsSource, udsSource WSA S-Extractor classification statistic in H real 4 -0.9999995e9 STAT_PROP

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

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

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

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

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

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

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

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

hDeblend calSource WSACalib placeholder flag indicating parent/child relation in H int 4 -99999999 CODE_MISC

This CASU pipeline processing source extraction flag is a placeholder only, and is always set to zero in all passbands in the merged source lists. If you need to know when a particular image detection is a component of a deblend or not, test bit 4 of attribute ppErrBits (see corresponding glossary entry) which is set by WFAU's post-processing software based on testing the areal profiles aprof2-8 (these are set by CASU to -1 for deblended components, or positive values for non-deblended detections). We encode this in an information bit of ppErrBits for convenience when querying the merged source tables.

hDeblend calSourceRemeasurement, calSynopticSource WSACalib placeholder flag indicating parent/child relation in H int 4 -99999999 CODE_MISC

hDeblend dxsJKsource, gcsPointSource, gcsSourceRemeasurement, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, gpsSourceRemeasurement, lasExtendedSource, lasPointSource, lasSourceRemeasurement, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource, udsSource, udsSourceRemeasurement WSA placeholder flag indicating parent/child relation in H int 4 -99999999 CODE_MISC

hDeblend dxsSource, gcsSource, lasSource WSA placeholder flag indicating parent/child relation in H int 4 -99999999 CODE_MISC

This CASU pipeline processing source extraction flag is a placeholder only, and is always set to zero in all passbands in the merged source lists. If you need to know when a particular image detection is a component of a deblend or not, test bit 4 of attribute ppErrBits (see corresponding glossary entry) which is set by WFAU's post-processing software based on testing the areal profiles aprof2-8 (these are set by CASU to -1 for deblended components, or positive values for non-deblended detections). We encode this in an information bit of ppErrBits for convenience when querying the merged source tables.

hdtFile Multiframe WSA Name of global hdt file {image primary HDU keyword: HDTFILE} varchar 32 NONE

hdtFile Multiframe WSACalib Name of global hdt file {image primary HDU keyword: HDTFILE} varchar 32 NONE

hdtFile Multiframe WSATransit Name of global hdt file {image primary HDU keyword: HDTFILE} varchar 32 NONE

hdtFileExt MultiframeDetector WSA Name of camera-specific hdt file {image extension keyword: HDTFILE2} varchar 32 NONE ??

hdtFileExt MultiframeDetector WSACalib Name of camera-specific hdt file {image extension keyword: HDTFILE2} varchar 32 NONE ??

hdtFileExt MultiframeDetector WSATransit Name of camera-specific hdt file {image extension keyword: HDTFILE2} varchar 32 NONE ??

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

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

hemis twomass_psc 2MASS Hemisphere code for the TWOMASS Observatory from which this source was observed. varchar 1 OBS_CODE

hemis twomass_scn 2MASS Observatory from which data were obtained: "n" = north = Mt. Hopkins, "s" = south = Cerro Tololo. varchar 1 OBS_CODE

hemis twomass_sixx2_scn 2MASS hemisphere (N/S) of observation varchar 1

hemis twomass_xsc 2MASS hemisphere (N/S) of observation. "n" = North/Mt. Hopkins; "s" = South/CTIO. varchar 1 OBS_CODE

heNum calMergeLog, calSynopticMergeLog WSACalib the extension number of this H frame tinyint 1 NUMBER

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

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

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

hErrBits calSourceRemeasurement WSACalib processing warning/error bitwise flags in H int 4 -99999999 CODE_MISC

hErrBits dxsJKsource, gcsPointSource, gcsSourceRemeasurement, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSourceRemeasurement, lasExtendedSource, lasPointSource, lasSourceRemeasurement, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource, udsSourceRemeasurement WSA processing warning/error bitwise flags in H int 4 -99999999 CODE_MISC

hErrBits dxsSource, gcsSource, lasSource WSA processing warning/error bitwise flags in H int 4 -99999999 CODE_MISC

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

hErrBits gpsSource, udsSource WSA processing warning/error bitwise flags in H int 4 -99999999 CODE_MISC

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

Bit Flag Meaning

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

2 The object was originally blended with another

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

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

16 Object's aperture data are incomplete or corrupted

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

64 Memory overflow occurred during deblending

128 Memory overflow occurred during extraction

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

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

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

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

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 2.0 (UKIDSS LAS and GPS; also non-survey programmes) or 1.0 (UKIDSS GPS, DXS and UDS) arcseconds is used, the higher value enabling pairing of moving sources when epoch separations may be several years. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the LAS, you might wish to insist that the offsets in the selected sample are all below 1 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

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

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

hexpML dxsVarFrameSetInfo, udsVarFrameSetInfo WSA Expected magnitude limit of frameSet in this in H band. real 4 -0.9999995e9

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

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

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

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

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

hGausig calSource, calSourceRemeasurement, calSynopticSource WSACalib RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 MORPH_PARAM

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

hgl twomass_scn 2MASS Special flag indicating whether or not this scan has a single-frame H-band electronic glitch. smallint 2 CODE_MISC

hgl twomass_sixx2_scn 2MASS single-frame H-band glitch flag (0:not found|1:found) smallint 2

hHallMag calSource WSACalib Total point source H mag real 4 mag -0.9999995e9 PHOT_MAG

hHallMag dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableLasPointSource WSA Total point source H mag real 4 mag -0.9999995e9 PHOT_MAG

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

hHallMagErr calSource WSACalib Error in total point source H mag real 4 mag -0.9999995e9 ERROR

hHallMagErr dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableLasPointSource WSA Error in total point source H mag real 4 mag -0.9999995e9 ERROR

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

hIntRms calVariability WSACalib Intrinsic rms in H-band real 4 mag -0.9999995e9

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

hIntRms dxsVariability, udsVariability WSA Intrinsic rms in H-band real 4 mag -0.9999995e9

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

hisDefAst dxsVarFrameSetInfo WSA Use a default model for the astrometric noise in H band. tinyint 1 0

hisDefPht dxsVarFrameSetInfo WSA Use a default model for the photometric noise in H band. tinyint 1 0

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

The Welch-Stetson statistic is a measure of the correlation of the variability between two bands. We use the calculation in Welch D.L. and Stetson P.B. 1993, AJ, 105, 5, which is also used in Sesar et al. 2007, AJ, 134, 2236. We use the aperMag3 magnitude when comparing between bands.

HLRADIUS mgcBrightSpec MGC Semi-major axis of half-light ellipse real 4 pixel

hMag calSourceRemeasurement WSACalib H mag (as appropriate for this merged source) real 4 mag -0.9999995e9 PHOT_MAG

hMag gcsSourceRemeasurement, gpsSourceRemeasurement, lasSourceRemeasurement, udsSourceRemeasurement WSA H mag (as appropriate for this merged source) real 4 mag -0.9999995e9 PHOT_MAG

hMag ukirtFSstars WSA H band total magnitude on the MKO(UFTI) system real 4 mag PHOT_INT-MAG

hMag ukirtFSstars WSACalib H band total magnitude on the MKO(UFTI) system real 4 mag PHOT_INT-MAG

hMagErr calSourceRemeasurement WSACalib Error in H mag real 4 mag -0.9999995e9 ERROR

hMagErr gcsSourceRemeasurement, gpsSourceRemeasurement, lasSourceRemeasurement, udsSourceRemeasurement WSA Error in H mag real 4 mag -0.9999995e9 ERROR

hMagErr ukirtFSstars WSA H band magnitude error real 4 mag ERROR

hMagErr ukirtFSstars WSACalib H band magnitude error real 4 mag ERROR

hMagMAD calVariability WSACalib Median Absolute Deviation of H magnitude real 4 mag -0.9999995e9

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

hMagMAD dxsVariability, udsVariability WSA Median Absolute Deviation of H magnitude real 4 mag -0.9999995e9

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

hMagRms calVariability WSACalib rms of H magnitude real 4 mag -0.9999995e9

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

hMagRms dxsVariability, udsVariability WSA rms of H magnitude real 4 mag -0.9999995e9

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

hmaxCadence 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.

hmaxCadence dxsVariability, 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.

hMaxMag calVariability WSACalib Maximum magnitude in H band, of good detections real 4 -0.9999995e9

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

hMaxMag dxsVariability, udsVariability WSA Maximum magnitude in H band, of good detections real 4 -0.9999995e9

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

hmeanMag calVariability WSACalib Mean H magnitude real 4 mag -0.9999995e9

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

hmeanMag dxsVariability, udsVariability WSA Mean H magnitude real 4 mag -0.9999995e9

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

hmedCadence 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.

hmedCadence dxsVariability, 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.

hmedianMag calVariability WSACalib Median H magnitude real 4 mag -0.9999995e9

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

hmedianMag dxsVariability, udsVariability WSA Median H magnitude real 4 mag -0.9999995e9

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

hmfID calMergeLog, calSynopticMergeLog WSACalib the UID of the relevant H multiframe bigint 8 ID_FRAME

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

hminCadence 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.

hminCadence dxsVariability, 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.

hMinMag calVariability WSACalib 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.

hMinMag dxsVariability WSA Minimum magnitude in H band, of good detections real 4 -0.9999995e9

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

hMinMag udsVariability WSA real 4 -0.9999995e9

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

hmk calSourceRemeasurement WSACalib Default colour H-K (using appropriate mags) real 4 mag PHOT_COLOR

hmk lasSourceRemeasurement, udsSourceRemeasurement WSA Default colour H-K (using appropriate mags) real 4 mag PHOT_COLOR

hmk_1 gcsSourceRemeasurement, gpsSourceRemeasurement WSA Default colour H-K (using appropriate mags) real 4 mag PHOT_COLOR

hmk_1Err gcsSourceRemeasurement, gpsSourceRemeasurement WSA Error on colour H-K real 4 mag ERROR

hmk_1Ext gcsPointSource, gcsZYJHKsource, reliableGcsPointSource WSA Extended source colour H-K (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

hmk_1Ext gcsSource WSA Extended source colour H-K (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

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

hmk_1ExtErr gcsPointSource, gcsZYJHKsource, reliableGcsPointSource WSA Error on extended source colour H-K real 4 mag -0.9999995e9 ERROR

hmk_1ExtErr gcsSource WSA Error on extended source colour H-K real 4 mag -0.9999995e9 ERROR

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

hmk_1Pnt gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, reliableGcsPointSource, reliableGpsPointSource WSA Point source colour H-K (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

hmk_1Pnt gcsSource, gpsSource WSA Point source colour H-K (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

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

hmk_1PntErr gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, reliableGcsPointSource, reliableGpsPointSource WSA Error on point source colour H-K real 4 mag -0.9999995e9 ERROR

hmk_1PntErr gcsSource, gpsSource WSA Error on point source colour H-K real 4 mag -0.9999995e9 ERROR

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

hmkErr calSourceRemeasurement WSACalib Error on colour H-K real 4 mag ERROR

hmkErr lasSourceRemeasurement, udsSourceRemeasurement WSA Error on colour H-K real 4 mag ERROR

hmkExt calSource WSACalib Extended source colour H-K (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

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

hmkExt dxsJKsource, lasExtendedSource, lasPointSource, lasYJHKsource, reliableDxsSource, reliableLasPointSource, reliableUdsSource WSA Extended source colour H-K (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

hmkExt dxsSource, lasSource, udsSource WSA Extended source colour H-K (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

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

hmkExtErr calSource WSACalib Error on extended source colour H-K real 4 mag -0.9999995e9 ERROR

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

hmkExtErr dxsJKsource, lasExtendedSource, lasPointSource, lasYJHKsource, reliableDxsSource, reliableLasPointSource, reliableUdsSource WSA Error on extended source colour H-K real 4 mag -0.9999995e9 ERROR

hmkExtErr dxsSource, lasSource, udsSource WSA Error on extended source colour H-K real 4 mag -0.9999995e9 ERROR

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

hmkPnt calSource, calSynopticSource WSACalib Point source colour H-K (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

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

hmkPnt dxsJKsource, lasExtendedSource, lasPointSource, lasYJHKsource, reliableDxsSource, reliableLasPointSource, reliableUdsSource WSA Point source colour H-K (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

hmkPnt dxsSource, lasSource, udsSource WSA Point source colour H-K (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

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

hmkPntErr calSource, calSynopticSource WSACalib Error on point source colour H-K real 4 mag -0.9999995e9 ERROR

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

hmkPntErr dxsJKsource, lasExtendedSource, lasPointSource, lasYJHKsource, reliableDxsSource, reliableLasPointSource, reliableUdsSource WSA Error on point source colour H-K real 4 mag -0.9999995e9 ERROR

hmkPntErr dxsSource, lasSource, udsSource WSA Error on point source colour H-K real 4 mag -0.9999995e9 ERROR

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

hndof calVariability WSACalib Number of degrees of freedom for chisquare int 4 -99999999

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.

hndof dxsVariability 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.

hndof udsVariability WSA Number of degrees of freedom for chisquare int 4 -99999999

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

hnDofAst calVarFrameSetInfo WSACalib Number of degrees of freedom of astrometric fit in H band. smallint 2 -9999

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

hnDofAst dxsVarFrameSetInfo, udsVarFrameSetInfo WSA Number of degrees of freedom of astrometric fit in H band. smallint 2 -9999

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

hnDofPht calVarFrameSetInfo WSACalib Number of degrees of freedom of photometric fit in H band. smallint 2 -9999

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

hnDofPht dxsVarFrameSetInfo, udsVarFrameSetInfo WSA Number of degrees of freedom of photometric fit in H band. smallint 2 -9999

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

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

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

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

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

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

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

hnGoodObs calVariability WSACalib Number of good detections in H band int 4 0

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

hnGoodObs dxsVariability, udsVariability WSA Number of good detections in H band int 4 0

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

hNgt3sig calVariability WSACalib Number of good detections in H-band that are more than 3 sigma deviations smallint 2 -9999

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

hNgt3sig dxsVariability, udsVariability WSA Number of good detections in H-band that are more than 3 sigma deviations smallint 2 -9999

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

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

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

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

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

hObjID calSource, calSourceRemeasurement, calSynopticSource WSACalib DEPRECATED (do not use) bigint 8 -99999999 ID_NUMBER

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

hObjID gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, lasExtendedSource, lasPointSource, lasYJHKsource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource WSA DEPRECATED (do not use) bigint 8 -99999999 ID_NUMBER

hObjID gcsSource, gcsSourceRemeasurement, gpsSource, gpsSourceRemeasurement, lasSource, lasSourceRemeasurement, udsSource, udsSourceRemeasurement WSA DEPRECATED (do not use) bigint 8 -99999999 ID_NUMBER

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

hourAngle Multiframe WSA Hour angle {image primary HDU keyword: HABASE} real 4 degrees -0.9999995e9

hourAngle Multiframe WSACalib Hour angle {image primary HDU keyword: HABASE} real 4 degrees -0.9999995e9

hourAngle Multiframe WSATransit Hour angle {image primary HDU keyword: HABASE} real 4 degrees -0.9999995e9

hPA calSource, calSourceRemeasurement, calSynopticSource WSACalib ellipse fit celestial orientation in H real 4 Degrees -0.9999995e9 POS_POS-ANG

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

hPetroMag calSource WSACalib Extended source H mag (Petrosian) real 4 mag -0.9999995e9 PHOT_MAG

hPetroMag dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableLasPointSource, reliableUdsSource, udsSource WSA Extended source H mag (Petrosian) real 4 mag -0.9999995e9 PHOT_MAG

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

hPetroMagErr dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableLasPointSource, reliableUdsSource, udsSource WSA Error in extended source H mag (Petrosian) real 4 mag -0.9999995e9 ERROR

hppErrBits calSource, calSynopticSource WSACalib additional WFAU post-processing error bits in H int 4 0 CODE_MISC

Post-processing error quality bit flags assigned (NB: from UKIDSS DR2 release onwards) in the WSA curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

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

1 15 Source in poor flat field region 32768 0x00008000 All but mosaics

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues (though deeps excluded prior to DR8)

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 GPS only

2 19 Possible crosstalk artefact/contamination 524288 0x00080000 All but GPS

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All but mosaics

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all K band sources in the LAS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hppErrBits calSourceRemeasurement WSACalib additional WFAU post-processing error bits in H int 4 0 CODE_MISC

hppErrBits dxsJKsource, gcsPointSource, gcsSourceRemeasurement, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, gpsSourceRemeasurement, lasExtendedSource, lasPointSource, lasSourceRemeasurement, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource, udsSource, udsSourceRemeasurement WSA additional WFAU post-processing error bits in H int 4 0 CODE_MISC

hppErrBits dxsSource, gcsSource, lasSource WSA additional WFAU post-processing error bits in H int 4 0 CODE_MISC

Post-processing error quality bit flags assigned (NB: from UKIDSS DR2 release onwards) in the WSA curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

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

1 15 Source in poor flat field region 32768 0x00008000 All but mosaics

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues (though deeps excluded prior to DR8)

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 GPS only

2 19 Possible crosstalk artefact/contamination 524288 0x00080000 All but GPS

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All but mosaics

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all K band sources in the LAS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

hprobVar 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.

hprobVar dxsVariability, 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.

hPsfMag calSource WSACalib Point source profile-fitted H mag real 4 mag -0.9999995e9 PHOT_MAG

hPsfMag dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableLasPointSource WSA Point source profile-fitted H mag real 4 mag -0.9999995e9 PHOT_MAG

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

hPsfMagErr calSource WSACalib Error in point source profile-fitted H mag real 4 mag -0.9999995e9 ERROR

hPsfMagErr dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableLasPointSource WSA Error in point source profile-fitted H mag real 4 mag -0.9999995e9 ERROR

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

hr1 rosat_bsc, rosat_fsc ROSAT hardness ratio 1 float 8 SPECT_HARDNESS-RATIO

hr2 rosat_bsc, rosat_fsc ROSAT hardness ratio 2 float 8 SPECT_HARDNESS-RATIO

hry twomass_scn 2MASS Flag indicating the H-band array configuration for the camera. smallint 2 CODE_MISC

hry twomass_sixx2_scn 2MASS H-band detector array switched, north only (0=old, 1=new) smallint 2

hsdFlag_100 iras_psc IRAS Source is located in high source density bin (100 micron). tinyint 1 REMARKS

hsdFlag_12 iras_psc IRAS Source is located in high source density bin (12 micron). tinyint 1 REMARKS

hsdFlag_25 iras_psc IRAS Source is located in high source density bin (25 micron). tinyint 1 REMARKS

hsdFlag_60 iras_psc IRAS Source is located in high source density bin (60 micron). tinyint 1 REMARKS

hSeqNum calSource, calSynopticSource WSACalib the running number of the H detection int 4 -99999999 ID_NUMBER

hSeqNum calSourceRemeasurement WSACalib the running number of the H remeasurement int 4 -99999999 ID_NUMBER

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

hSeqNum gcsSourceRemeasurement, gpsSourceRemeasurement, lasSourceRemeasurement, udsSourceRemeasurement WSA the running number of the H remeasurement int 4 -99999999 ID_NUMBER

hSerMag2D calSource WSACalib Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 PHOT_MAG

hSerMag2D dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableLasPointSource WSA Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 PHOT_MAG

hSerMag2D reliableUdsSource, udsSource WSA Not available in SE output real 4 mag -0.9999995e9 PHOT_MAG

hSerMag2DErr calSource WSACalib Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 ERROR

hSerMag2DErr dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsZYJHKsource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableLasPointSource WSA Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 ERROR

hSerMag2DErr reliableUdsSource, udsSource WSA Not available in SE output real 4 mag -0.9999995e9 ERROR

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

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

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

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

HTMID twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 POS_GENERAL

htmID CurrentAstrometry WSACalib Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 POS_GENERAL

htmID CurrentAstrometry WSATransit Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 POS_GENERAL

htmID CurrentAstrometry, PreviousAstrometry WSA Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre bigint 8 -99999999 POS_GENERAL

htmID dxsDetection, dxsJKmergeLog, dxsJKsource, dxsMergeLog, dxsSource, gcsDetection, gcsListRemeasurement, gcsMergeLog, gcsPointSource, gcsSource, gcsSourceRemeasurement, gcsZYJHKmergeLog, gcsZYJHKsource, gpsDetection, gpsJHKmergeLog, gpsJHKsource, gpsListRemeasurement, gpsMergeLog, gpsPointSource, gpsSource, gpsSourceRemeasurement, lasDetection, lasExtendedSource, lasListRemeasurement, lasMergeLog, lasPointSource, lasSource, lasSourceRemeasurement, lasYJHKmergeLog, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource, UKIDSSDetection, udsDetection, udsListRemeasurement, udsMergeLog, udsSource, udsSourceRemeasurement WSA Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 POS_GENERAL

htmID calDetection, calListRemeasurement, calMergeLog, calSource, calSourceRemeasurement, calSynopticMergeLog, calSynopticSource WSACalib Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 POS_GENERAL

htmID first08Jul16Source, firstSource FIRST Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 POS_GENERAL

htmID glimpse1_hrc, glimpse1_mca, glimpse2_hrc, glimpse2_mca, glimpse_hrc_inter, glimpse_mca_inter GLIMPSE Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 POS_GENERAL

htmID iras_psc IRAS Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 POS_GENERAL

htmID mgcDetection MGC Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 POS_GENERAL

htmID nvssSource NVSS Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 POS_GENERAL

htmID ptsDetection WSATransit Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 POS_GENERAL

htmID rosat_bsc, rosat_fsc ROSAT Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 POS_GENERAL

htmID twomass_psc, twomass_scn, twomass_sixx2_psc, twomass_sixx2_scn, twomass_sixx2_xsc, twomass_xsc 2MASS Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 POS_GENERAL

htmID wise_prelimsc WISE Hierarchical Triangular Mesh (HTM) index for equatorial co-ordinates (similar to spt_ind in IPAC IRSA schema, but recomputed to level 20) bigint 8 POS_GENERAL

htotalPeriod 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.

htotalPeriod dxsVariability, 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.

humidity Multiframe WSA Relative Humidity {image primary HDU keyword: HUMIDITY} real 4 -0.9999995e9 OBS_CONDITIONS

humidity Multiframe WSACalib Relative Humidity {image primary HDU keyword: HUMIDITY} real 4 -0.9999995e9 OBS_CONDITIONS

humidity Multiframe WSATransit Relative Humidity {image primary HDU keyword: HUMIDITY} real 4 -0.9999995e9 OBS_CONDITIONS

hVarClass 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.

hVarClass dxsVariability, 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.

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

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

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

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

When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 2.0 (UKIDSS LAS and GPS; also non-survey programmes) or 1.0 (UKIDSS GPS, DXS and UDS) arcseconds is used, the higher value enabling pairing of moving sources when epoch separations may be several years. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the LAS, you might wish to insist that the offsets in the selected sample are all below 1 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands.

hz10cd Multiframe WSA Trefoil: HZ10CD {image primary HDU keyword: HZ10CD} real 4 -0.9999995e9

hz10cd Multiframe WSACalib Trefoil: HZ10CD {image primary HDU keyword: HZ10CD} real 4 -0.9999995e9

hz10cd Multiframe WSATransit Trefoil: HZ10CD {image primary HDU keyword: HZ10CD} real 4 -0.9999995e9

hz10ch Multiframe WSA Trefoil: HZ10CH {image primary HDU keyword: HZ10CH} real 4 -0.9999995e9

hz10ch Multiframe WSACalib Trefoil: HZ10CH {image primary HDU keyword: HZ10CH} real 4 -0.9999995e9

hz10ch Multiframe WSATransit Trefoil: HZ10CH {image primary HDU keyword: HZ10CH} real 4 -0.9999995e9

hz10sd Multiframe WSA Trefoil: HZ10SD {image primary HDU keyword: HZ10SD} real 4 -0.9999995e9

hz10sd Multiframe WSACalib Trefoil: HZ10SD {image primary HDU keyword: HZ10SD} real 4 -0.9999995e9

hz10sd Multiframe WSATransit Trefoil: HZ10SD {image primary HDU keyword: HZ10SD} real 4 -0.9999995e9

hz10sh Multiframe WSA Trefoil: HZ10SH {image primary HDU keyword: HZ10SH} real 4 -0.9999995e9

hz10sh Multiframe WSACalib Trefoil: HZ10SH {image primary HDU keyword: HZ10SH} real 4 -0.9999995e9

hz10sh Multiframe WSATransit Trefoil: HZ10SH {image primary HDU keyword: HZ10SH} real 4 -0.9999995e9

hz5cd Multiframe WSA Astigmatism: HZ5CD {image primary HDU keyword: HZ5CD} real 4 -0.9999995e9

hz5cd Multiframe WSACalib Astigmatism: HZ5CD {image primary HDU keyword: HZ5CD} real 4 -0.9999995e9

hz5cd Multiframe WSATransit Astigmatism: HZ5CD {image primary HDU keyword: HZ5CD} real 4 -0.9999995e9

hz5ch Multiframe WSA Astigmatism: HZ5CH {image primary HDU keyword: HZ5CH} real 4 -0.9999995e9

hz5ch Multiframe WSACalib Astigmatism: HZ5CH {image primary HDU keyword: HZ5CH} real 4 -0.9999995e9

hz5ch Multiframe WSATransit Astigmatism: HZ5CH {image primary HDU keyword: HZ5CH} real 4 -0.9999995e9

hz5sd Multiframe WSA Astigmatism: HZ5SD {image primary HDU keyword: HZ5SD} real 4 -0.9999995e9

hz5sd Multiframe WSACalib Astigmatism: HZ5SD {image primary HDU keyword: HZ5SD} real 4 -0.9999995e9

hz5sd Multiframe WSATransit Astigmatism: HZ5SD {image primary HDU keyword: HZ5SD} real 4 -0.9999995e9

hz5sh Multiframe WSA Astigmatism: HZ5SH {image primary HDU keyword: HZ5SH} real 4 -0.9999995e9

hz5sh Multiframe WSACalib Astigmatism: HZ5SH {image primary HDU keyword: HZ5SH} real 4 -0.9999995e9

hz5sh Multiframe WSATransit Astigmatism: HZ5SH {image primary HDU keyword: HZ5SH} real 4 -0.9999995e9

hz6cd Multiframe WSA Astigmatism: HZ6CD {image primary HDU keyword: HZ6CD} real 4 -0.9999995e9

hz6cd Multiframe WSACalib Astigmatism: HZ6CD {image primary HDU keyword: HZ6CD} real 4 -0.9999995e9

hz6cd Multiframe WSATransit Astigmatism: HZ6CD {image primary HDU keyword: HZ6CD} real 4 -0.9999995e9

hz6ch Multiframe WSA Astigmatism: HZ6CH {image primary HDU keyword: HZ6CH} real 4 -0.9999995e9

hz6ch Multiframe WSACalib Astigmatism: HZ6CH {image primary HDU keyword: HZ6CH} real 4 -0.9999995e9

hz6ch Multiframe WSATransit Astigmatism: HZ6CH {image primary HDU keyword: HZ6CH} real 4 -0.9999995e9

hz6sd Multiframe WSA Astigmatism: HZ6SD {image primary HDU keyword: HZ6SD} real 4 -0.9999995e9

hz6sd Multiframe WSACalib Astigmatism: HZ6SD {image primary HDU keyword: HZ6SD} real 4 -0.9999995e9

hz6sd Multiframe WSATransit Astigmatism: HZ6SD {image primary HDU keyword: HZ6SD} real 4 -0.9999995e9

hz6sh Multiframe WSA Astigmatism: HZ6SH {image primary HDU keyword: HZ6SH} real 4 -0.9999995e9

hz6sh Multiframe WSACalib Astigmatism: HZ6SH {image primary HDU keyword: HZ6SH} real 4 -0.9999995e9

hz6sh Multiframe WSATransit Astigmatism: HZ6SH {image primary HDU keyword: HZ6SH} real 4 -0.9999995e9

hz9cd Multiframe WSA Trefoil: HZ9CD {image primary HDU keyword: HZ9CD} real 4 -0.9999995e9

hz9cd Multiframe WSACalib Trefoil: HZ9CD {image primary HDU keyword: HZ9CD} real 4 -0.9999995e9

hz9cd Multiframe WSATransit Trefoil: HZ9CD {image primary HDU keyword: HZ9CD} real 4 -0.9999995e9

hz9ch Multiframe WSA Trefoil: HZ9CH {image primary HDU keyword: HZ9CH} real 4 -0.9999995e9

hz9ch Multiframe WSACalib Trefoil: HZ9CH {image primary HDU keyword: HZ9CH} real 4 -0.9999995e9

hz9ch Multiframe WSATransit Trefoil: HZ9CH {image primary HDU keyword: HZ9CH} real 4 -0.9999995e9

hz9sd Multiframe WSA Trefoil: HZ9SD {image primary HDU keyword: HZ9SD} real 4 -0.9999995e9

hz9sd Multiframe WSACalib Trefoil: HZ9SD {image primary HDU keyword: HZ9SD} real 4 -0.9999995e9

hz9sd Multiframe WSATransit Trefoil: HZ9SD {image primary HDU keyword: HZ9SD} real 4 -0.9999995e9

hz9sh Multiframe WSA Trefoil: HZ9SH {image primary HDU keyword: HZ9SH} real 4 -0.9999995e9

hz9sh Multiframe WSACalib Trefoil: HZ9SH {image primary HDU keyword: HZ9SH} real 4 -0.9999995e9

hz9sh Multiframe WSATransit Trefoil: HZ9SH {image primary HDU keyword: HZ9SH} real 4 -0.9999995e9

WFAU, Institute for Astronomy,
Royal Observatory, Blackford Hill
Edinburgh, EH9 3HJ, UK
Tel +44 131 668 8356 (office)
or +44 131 668 8100 (switchboard)

wsa-support@roe.ac.uk
04/04/2012