WSA Browser

Glossary of WSA NonSurvey attributes (UKIDSSDR4)

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

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

H

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

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

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

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

h2AperMag4Err [nspid]Source WSA NonSurvey Error in extended source H2 mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

h2AperMag6 [nspid]Source WSA NonSurvey Extended source H2 aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

h2AperMag6Err [nspid]Source WSA NonSurvey Error in extended source H2 mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

h2aStrat [nspid]VarFrameSetInfo WSA NonSurvey Strateva parameter a in H2 band, see Sesar et al. 2007. real 4 -0.9999995e9

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

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

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

h2bStrat [nspid]VarFrameSetInfo WSA NonSurvey Strateva parameter b in H2 band, see Sesar et al. 2007. real 4 -0.9999995e9

The best fit solution to the expected RMS 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.

h2chiSq [nspid]VarFrameSetInfo WSA NonSurvey Fit of Strateva function to data in H2 band real 4 -0.9999995e9

The best fit solution to the expected RMS 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.

h2chiSqpd [nspid]Variability WSA NonSurvey Chi square (per degree of freedom) fit to data (mean and expected rms) real 4 0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median and median absolute deviation are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. 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.

h2Class [nspid]Source WSA NonSurvey discrete image classification flag in H2 smallint 2 -9999 CLASS_MISC

h2ClassStat [nspid]Source WSA NonSurvey N(0,1) stellarness-of-profile statistic in H2 real 4 -0.9999995e9 STAT_PROP

h2cStrat [nspid]VarFrameSetInfo WSA NonSurvey Strateva parameter a in H2 band, see Sesar et al. 2007. real 4 -0.9999995e9

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

h2Deblend [nspid]Source WSA NonSurvey placeholder flag indicating parent/child relation in H2 int 4 -99999999 CODE_MISC

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

h2Ell [nspid]Source WSA NonSurvey 1-b/a, where a/b=semi-major/minor axes in H2 real 4 -0.9999995e9 PHYS_ELLIPTICITY

h2eNum [nspid]MergeLog WSA NonSurvey the extension number of this H2 detector tinyint 1 NUMBER

h2ErrBits [nspid]Source WSA NonSurvey processing warning/error bitwise flags in H2 int 4 -99999999 CODE_MISC

h2Eta [nspid]Source WSA NonSurvey Offset of H2 detection from master position (+north/-south) real 4 arcsec -0.9999995e9 POS_EQ_DEC_OFF

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

h2expML [nspid]VarFrameSetInfo WSA NonSurvey Expected magnitude limit of frameSet in this in H2 band. real 4 -0.9999995e9

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

h2ExpRms [nspid]Variability WSA NonSurvey Rms calculated from polynomial fit to minimum 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 and median absolute deviation are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3.

h2Gausig [nspid]Source WSA NonSurvey RMS of axes of ellipse fit in H2 real 4 pixels -0.9999995e9 MORPH_PARAM

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

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

h2IntRms [nspid]Variability WSA NonSurvey Intrinsic rms in H2-band real 4 mag -0.9999995e9

The photometry is calculated for good observations in the best aperture. The mean, rms, median and median absolute deviation are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. 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.

h2MagMAD [nspid]Variability WSA NonSurvey Median Absolute Deviation of H2 magnitude real 4 mag -0.9999995e9

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

h2MagRms [nspid]Variability WSA NonSurvey rms of H2 magnitude real 4 mag -0.9999995e9

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

h2maxCadence [nspid]Variability WSA NonSurvey maximum gap between observations real 4 days -0.9999995e9

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

h2meanMag [nspid]Variability WSA NonSurvey Mean H2 magnitude real 4 mag -0.9999995e9

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

h2medCadence [nspid]Variability WSA NonSurvey median gap between observations real 4 days -0.9999995e9

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

h2medianMag [nspid]Variability WSA NonSurvey Median H2 magnitude real 4 mag -0.9999995e9

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

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

h2minCadence [nspid]Variability WSA NonSurvey minimum gap between observations real 4 days -0.9999995e9

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

h2nDof [nspid]VarFrameSetInfo WSA NonSurvey Number of degrees of freedom of fit in H2 band. smallint 2 -9999

The best fit solution to the expected RMS 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.

h2ndof [nspid]Variability WSA NonSurvey Number of degrees of freedom for chisquare int 4 -9999

The photometry is calculated for good observations in the best aperture. The mean, rms, median and median absolute deviation are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. 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.

h2nFlaggedObs [nspid]Variability WSA NonSurvey Number of detections in H2 band flagged as potentially spurious by userv1707Detection.ppErrBits int 4 0

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

h2nGoodObs [nspid]Variability WSA NonSurvey Number of good detections in H2 band int 4 0

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

h2nMissingObs [nspid]Variability WSA NonSurvey Number of H2 band frames that this object should have been detected on and was not int 4 0

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

h2ObjID [nspid]Source WSA NonSurvey the UID of the H2 detection bigint 8 -99999999 ID_NUMBER

h2PA [nspid]Source WSA NonSurvey ellipse fit celestial orientation in H2 real 4 Degrees -0.9999995e9 POS_POS-ANG

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

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

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

h2probVar [nspid]Variability WSA NonSurvey Probability of variable from chi-square (and other data) real 4 0.9999995e9

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

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

h2PsfMagErr [nspid]Source WSA NonSurvey Error in point source profile-fitted H2 mag real 4 mag -0.9999995e9 ERROR

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

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

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

h2skewness [nspid]Variability WSA NonSurvey Skewness in H2 band (see Sesar et al. 2007) real 4 -0.9999995e9

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

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

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

h2VarClass [nspid]Variability WSA NonSurvey Classification of variability in this band smallint 2 -9999

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

h2Xi [nspid]Source WSA NonSurvey Offset of H2 detection from master position (+east/-west) real 4 arcsec -0.9999995e9 POS_EQ_RA_OFF

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

h_1AperMag3 [nspid]Source WSA NonSurvey Default point/extended source H_1 aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

h_1AperMag3Err [nspid]Source WSA NonSurvey Error in default point/extended source H_1 mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

h_1AperMag4 [nspid]Source WSA NonSurvey Extended source H_1 aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

h_1AperMag4Err [nspid]Source WSA NonSurvey Error in extended source H_1 mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

h_1AperMag6 [nspid]Source WSA NonSurvey Extended source H_1 aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

h_1AperMag6Err [nspid]Source WSA NonSurvey Error in extended source H_1 mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

h_1Class [nspid]Source WSA NonSurvey discrete image classification flag in H_1 smallint 2 -9999 CLASS_MISC

h_1ClassStat [nspid]Source WSA NonSurvey N(0,1) stellarness-of-profile statistic in H_1 real 4 -0.9999995e9 STAT_PROP

h_1Deblend [nspid]Source WSA NonSurvey placeholder flag indicating parent/child relation in H_1 int 4 -99999999 CODE_MISC

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

h_1Ell [nspid]Source WSA NonSurvey 1-b/a, where a/b=semi-major/minor axes in H_1 real 4 -0.9999995e9 PHYS_ELLIPTICITY

h_1eNum [nspid]MergeLog WSA NonSurvey the extension number of this H_1 detector tinyint 1 NUMBER

h_1ErrBits [nspid]Source WSA NonSurvey processing warning/error bitwise flags in H_1 int 4 -99999999 CODE_MISC

h_1Eta [nspid]Source WSA NonSurvey Offset of H_1 detection from master position (+north/-south) real 4 arcsec -0.9999995e9 POS_EQ_DEC_OFF

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

h_1Gausig [nspid]Source WSA NonSurvey RMS of axes of ellipse fit in H_1 real 4 pixels -0.9999995e9 MORPH_PARAM

h_1HallMag [nspid]Source WSA NonSurvey Total point source H_1 mag real 4 mag -0.9999995e9 PHOT_MAG

h_1HallMagErr [nspid]Source WSA NonSurvey Error in total point source H_1 mag real 4 mag -0.9999995e9 ERROR

h_1mfID [nspid]MergeLog WSA NonSurvey the UID of the relevant H_1 multiframe bigint 8 ID_FRAME

h_1mk_1Ext [nspid]Source WSA NonSurvey Extended source colour H_1-K_1 (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

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

h_1mk_1ExtErr [nspid]Source WSA NonSurvey Error on extended source colour H_1-K_1 real 4 mag -0.9999995e9 ERROR

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

h_1mk_1Pnt [nspid]Source WSA NonSurvey Point source colour H_1-K_1 (using aperMag3) real 4 mag -0.9999995e9 PHOT_COLOR

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

h_1mk_1PntErr [nspid]Source WSA NonSurvey Error on point source colour H_1-K_1 real 4 mag -0.9999995e9 ERROR

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

h_1ObjID [nspid]Source WSA NonSurvey the UID of the H_1 detection bigint 8 -99999999 ID_NUMBER

h_1PA [nspid]Source WSA NonSurvey ellipse fit celestial orientation in H_1 real 4 Degrees -0.9999995e9 POS_POS-ANG

h_1PetroMag [nspid]Source WSA NonSurvey Extended source H_1 mag (Petrosian) real 4 mag -0.9999995e9 PHOT_MAG

h_1PetroMagErr [nspid]Source WSA NonSurvey Error in extended source H_1 mag (Petrosian) real 4 mag -0.9999995e9 ERROR

h_1ppErrBits [nspid]Source WSA NonSurvey additional WFAU post-processing error bits in H_1 int 4 0 CODE_MISC

h_1PsfMag [nspid]Source WSA NonSurvey Point source profile-fitted H_1 mag real 4 mag -0.9999995e9 PHOT_MAG

h_1PsfMagErr [nspid]Source WSA NonSurvey Error in point source profile-fitted H_1 mag real 4 mag -0.9999995e9 ERROR

h_1SeqNum [nspid]Source WSA NonSurvey the running number of the H_1 detection int 4 -99999999 ID_NUMBER

h_1SerMag2D [nspid]Source WSA NonSurvey Extended source H_1 mag (profile-fitted) real 4 mag -0.9999995e9 PHOT_MAG

h_1SerMag2DErr [nspid]Source WSA NonSurvey Error in extended source H_1 mag (profile-fitted) real 4 mag -0.9999995e9 ERROR

h_1Xi [nspid]Source WSA NonSurvey Offset of H_1 detection from master position (+east/-west) real 4 arcsec -0.9999995e9 POS_EQ_RA_OFF

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

h_2AperMag3 [nspid]Source WSA NonSurvey Default point/extended source H_2 aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

h_2AperMag3Err [nspid]Source WSA NonSurvey Error in default point/extended source H_2 mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

h_2AperMag4 [nspid]Source WSA NonSurvey Extended source H_2 aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

h_2AperMag4Err [nspid]Source WSA NonSurvey Error in extended source H_2 mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

h_2AperMag6 [nspid]Source WSA NonSurvey Extended source H_2 aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

h_2AperMag6Err [nspid]Source WSA NonSurvey Error in extended source H_2 mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

h_2Class [nspid]Source WSA NonSurvey discrete image classification flag in H_2 smallint 2 -9999 CLASS_MISC

h_2ClassStat [nspid]Source WSA NonSurvey N(0,1) stellarness-of-profile statistic in H_2 real 4 -0.9999995e9 STAT_PROP

h_2Deblend [nspid]Source WSA NonSurvey placeholder flag indicating parent/child relation in H_2 int 4 -99999999 CODE_MISC

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

h_2Ell [nspid]Source WSA NonSurvey 1-b/a, where a/b=semi-major/minor axes in H_2 real 4 -0.9999995e9 PHYS_ELLIPTICITY

h_2eNum [nspid]MergeLog WSA NonSurvey the extension number of this H_2 detector tinyint 1 NUMBER

h_2ErrBits [nspid]Source WSA NonSurvey processing warning/error bitwise flags in H_2 int 4 -99999999 CODE_MISC

h_2Eta [nspid]Source WSA NonSurvey Offset of H_2 detection from master position (+north/-south) real 4 arcsec -0.9999995e9 POS_EQ_DEC_OFF

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

h_2Gausig [nspid]Source WSA NonSurvey RMS of axes of ellipse fit in H_2 real 4 pixels -0.9999995e9 MORPH_PARAM

h_2HallMag [nspid]Source WSA NonSurvey Total point source H_2 mag real 4 mag -0.9999995e9 PHOT_MAG

h_2HallMagErr [nspid]Source WSA NonSurvey Error in total point source H_2 mag real 4 mag -0.9999995e9 ERROR

h_2mfID [nspid]MergeLog WSA NonSurvey the UID of the relevant H_2 multiframe bigint 8 ID_FRAME

h_2ObjID [nspid]Source WSA NonSurvey the UID of the H_2 detection bigint 8 -99999999 ID_NUMBER

h_2PA [nspid]Source WSA NonSurvey ellipse fit celestial orientation in H_2 real 4 Degrees -0.9999995e9 POS_POS-ANG

h_2PetroMag [nspid]Source WSA NonSurvey Extended source H_2 mag (Petrosian) real 4 mag -0.9999995e9 PHOT_MAG

h_2PetroMagErr [nspid]Source WSA NonSurvey Error in extended source H_2 mag (Petrosian) real 4 mag -0.9999995e9 ERROR

h_2ppErrBits [nspid]Source WSA NonSurvey additional WFAU post-processing error bits in H_2 int 4 0 CODE_MISC

h_2PsfMag [nspid]Source WSA NonSurvey Point source profile-fitted H_2 mag real 4 mag -0.9999995e9 PHOT_MAG

h_2PsfMagErr [nspid]Source WSA NonSurvey Error in point source profile-fitted H_2 mag real 4 mag -0.9999995e9 ERROR

h_2SeqNum [nspid]Source WSA NonSurvey the running number of the H_2 detection int 4 -99999999 ID_NUMBER

h_2SerMag2D [nspid]Source WSA NonSurvey Extended source H_2 mag (profile-fitted) real 4 mag -0.9999995e9 PHOT_MAG

h_2SerMag2DErr [nspid]Source WSA NonSurvey Error in extended source H_2 mag (profile-fitted) real 4 mag -0.9999995e9 ERROR

h_2Xi [nspid]Source WSA NonSurvey Offset of H_2 detection from master position (+east/-west) real 4 arcsec -0.9999995e9 POS_EQ_RA_OFF

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

h_3AperMag3 [nspid]Source WSA NonSurvey Default point/extended source H_3 aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

h_3AperMag3Err [nspid]Source WSA NonSurvey Error in default point/extended source H_3 mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

h_3AperMag4 [nspid]Source WSA NonSurvey Extended source H_3 aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

h_3AperMag4Err [nspid]Source WSA NonSurvey Error in extended source H_3 mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

h_3AperMag6 [nspid]Source WSA NonSurvey Extended source H_3 aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

h_3AperMag6Err [nspid]Source WSA NonSurvey Error in extended source H_3 mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

h_3Class [nspid]Source WSA NonSurvey discrete image classification flag in H_3 smallint 2 -9999 CLASS_MISC

h_3ClassStat [nspid]Source WSA NonSurvey N(0,1) stellarness-of-profile statistic in H_3 real 4 -0.9999995e9 STAT_PROP

h_3Deblend [nspid]Source WSA NonSurvey placeholder flag indicating parent/child relation in H_3 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.

h_3Ell [nspid]Source WSA NonSurvey 1-b/a, where a/b=semi-major/minor axes in H_3 real 4 -0.9999995e9 PHYS_ELLIPTICITY

h_3eNum [nspid]MergeLog WSA NonSurvey the extension number of this H_3 detector tinyint 1 NUMBER

h_3ErrBits [nspid]Source WSA NonSurvey processing warning/error bitwise flags in H_3 int 4 -99999999 CODE_MISC

h_3Eta [nspid]Source WSA NonSurvey Offset of H_3 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.

h_3Gausig [nspid]Source WSA NonSurvey RMS of axes of ellipse fit in H_3 real 4 pixels -0.9999995e9 MORPH_PARAM

h_3HallMag [nspid]Source WSA NonSurvey Total point source H_3 mag real 4 mag -0.9999995e9 PHOT_MAG

h_3HallMagErr [nspid]Source WSA NonSurvey Error in total point source H_3 mag real 4 mag -0.9999995e9 ERROR

h_3mfID [nspid]MergeLog WSA NonSurvey the UID of the relevant H_3 multiframe bigint 8 ID_FRAME

h_3ObjID [nspid]Source WSA NonSurvey the UID of the H_3 detection bigint 8 -99999999 ID_NUMBER

h_3PA [nspid]Source WSA NonSurvey ellipse fit celestial orientation in H_3 real 4 Degrees -0.9999995e9 POS_POS-ANG

h_3PetroMag [nspid]Source WSA NonSurvey Extended source H_3 mag (Petrosian) real 4 mag -0.9999995e9 PHOT_MAG

h_3PetroMagErr [nspid]Source WSA NonSurvey Error in extended source H_3 mag (Petrosian) real 4 mag -0.9999995e9 ERROR

h_3ppErrBits [nspid]Source WSA NonSurvey additional WFAU post-processing error bits in H_3 int 4 0 CODE_MISC

h_3PsfMag [nspid]Source WSA NonSurvey Point source profile-fitted H_3 mag real 4 mag -0.9999995e9 PHOT_MAG

h_3PsfMagErr [nspid]Source WSA NonSurvey Error in point source profile-fitted H_3 mag real 4 mag -0.9999995e9 ERROR

h_3SeqNum [nspid]Source WSA NonSurvey the running number of the H_3 detection int 4 -99999999 ID_NUMBER

h_3SerMag2D [nspid]Source WSA NonSurvey Extended source H_3 mag (profile-fitted) real 4 mag -0.9999995e9 PHOT_MAG

h_3SerMag2DErr [nspid]Source WSA NonSurvey Error in extended source H_3 mag (profile-fitted) real 4 mag -0.9999995e9 ERROR

h_3Xi [nspid]Source WSA NonSurvey Offset of H_3 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.

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

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

hallMag [nspid]Detection WSA NonSurvey Calibrated magnitude within circular aperture r_hall real 4 mag PHOT_INT-MAG

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

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

hAperMag3 [nspid]Source WSA NonSurvey Default point/extended source H aperture corrected mag (2.0 arcsec aperture diameter)
If in doubt use this flux estimator real 4 mag -0.9999995e9 PHOT_MAG

hAperMag3Err [nspid]Source WSA NonSurvey Error in default point/extended source H mag (2.0 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

hAperMag4 [nspid]Source WSA NonSurvey Extended source H aperture corrected mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

hAperMag4Err [nspid]Source WSA NonSurvey Error in extended source H mag (2.8 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

hAperMag6 [nspid]Source WSA NonSurvey Extended source H aperture corrected mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 PHOT_MAG

hAperMag6Err [nspid]Source WSA NonSurvey Error in extended source H mag (5.7 arcsec aperture diameter) real 4 mag -0.9999995e9 ERROR

hClass [nspid]Source WSA NonSurvey discrete image classification flag in H smallint 2 -9999 CLASS_MISC

hClassStat [nspid]Source WSA NonSurvey N(0,1) stellarness-of-profile statistic in H real 4 -0.9999995e9 STAT_PROP

hDeblend [nspid]Source WSA NonSurvey placeholder flag indicating parent/child relation in H int 4 -99999999 CODE_MISC

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

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

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

hEll [nspid]Source WSA NonSurvey 1-b/a, where a/b=semi-major/minor axes in H real 4 -0.9999995e9 PHYS_ELLIPTICITY

heNum [nspid]MergeLog WSA NonSurvey the extension number of this H detector tinyint 1 NUMBER

hErrBits [nspid]Source WSA NonSurvey processing warning/error bitwise flags in H int 4 -99999999 CODE_MISC

hEta [nspid]Source WSA NonSurvey Offset of H detection from master position (+north/-south) real 4 arcsec -0.9999995e9 POS_EQ_DEC_OFF

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

hGausig [nspid]Source WSA NonSurvey RMS of axes of ellipse fit in H real 4 pixels -0.9999995e9 MORPH_PARAM

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

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

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

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

hmfID [nspid]MergeLog WSA NonSurvey the UID of the relevant H multiframe bigint 8 ID_FRAME

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

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

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

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

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

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

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

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

hObjID [nspid]Source WSA NonSurvey the UID of the H detection bigint 8 -99999999 ID_NUMBER

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

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

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

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

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

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

hPsfMagErr [nspid]Source WSA NonSurvey Error in point source profile-fitted H mag real 4 mag -0.9999995e9 ERROR

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

hSerMag2D [nspid]Source WSA NonSurvey Extended source H mag (profile-fitted) real 4 mag -0.9999995e9 PHOT_MAG

hSerMag2DErr [nspid]Source WSA NonSurvey Error in extended source H mag (profile-fitted) real 4 mag -0.9999995e9 ERROR

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

htmID [nspid]Detection, [nspid]Source WSA NonSurvey Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates bigint 8 POS_GENERAL

htmID [nspid]MergeLog WSA NonSurvey HTM index, 20 digits, for co-ordinates bigint 8 POS_GENERAL

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

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

hXi [nspid]Source WSA NonSurvey Offset of H detection from master position (+east/-west) real 4 arcsec -0.9999995e9 POS_EQ_RA_OFF

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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03/04/2009