H 
Name  Schema Table  Database  Description  Type  Length  Unit  Default Value  Unified Content Descriptor 
h2AperMag1 
calSynopticSource 
WSACalib 
Extended source H2 aperture corrected mag (0.7 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 (0.7 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 medianabsolute 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 chisquared and number of degrees of freedom are also calculated. 
h2aStratPht 
calVarFrameSetInfo 
WSACalib 
Strateva parameter, a, in fit to photometric rms vs magnitude in H2 band, see Sesar et al. 2007. 
real 
4 

0.9999995e9 

The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the medianabsolute 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 chisquared 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 (16) for photometric statistics in the H2 band 
int 
4 

9999 

Aperture magnitude (16) 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 medianabsolute 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 chisquared 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 medianabsolute 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 chisquared 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 medianabsolute 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 chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 medianabsolute 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 chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
h2Class 
calSource, 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, calSynopticSource 
WSACalib 
N(0,1) stellarnessofprofile statistic in H2 
real 
4 

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

0.9999995e9 
STAT_PROP 
h2ClassStat 
gpsSourceRemeasurement 
WSA 
N(0,1) stellarnessofprofile 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 medianabsolute 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 chisquared 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 medianabsolute 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 chisquared 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 postprocessing software based on testing the areal profiles aprof28 (these are set by CASU to 1 for deblended components, or positive values for nondeblended detections). We encode this in an information bit of ppErrBits for convenience when querying the merged source tables. 
h2Deblend 
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, calSynopticSource 
WSACalib 
1b/a, where a/b=semimajor/minor axes in H2 
real 
4 

0.9999995e9 
PHYS_ELLIPTICITY 
h2Ell 
gpsJHKsource, gpsPointSource, gpsSource, gpsSourceRemeasurement, reliableGpsPointSource 
WSA 
1b/a, where a/b=semimajor/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 
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; UHS; also nonsurvey 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; UHS; also nonsurvey 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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, 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 H2band 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
h2isDefAst 
calVarFrameSetInfo 
WSACalib 
Use a default model for the astrometric noise in H2 band. 
tinyint 
1 

0 

h2isDefPht 
calVarFrameSetInfo 
WSACalib 
Use a default model for the photometric noise in H2 band. 
tinyint 
1 

0 

h2Mag 
gpsSourceRemeasurement 
WSA 
H2 mag (as appropriate for this merged source) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 
Minimum magnitude in H2 band, of good detections 
real 
4 

0.9999995e9 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 H2K (using appropriate mags) 
real 
4 
mag 

PHOT_COLOR 
h2mk_1Err 
gpsSourceRemeasurement 
WSA 
Error on colour H2K 
real 
4 
mag 

ERROR 
h2mk_1Pnt 
gpsJHKsource, gpsPointSource, reliableGpsPointSource 
WSA 
Point source colour H2K (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
h2mk_1Pnt 
gpsSource 
WSA 
Point source colour H2K (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource 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 signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
h2mk_1PntErr 
gpsJHKsource, gpsPointSource, reliableGpsPointSource 
WSA 
Error on point source colour H2K 
real 
4 
mag 
0.9999995e9 
ERROR 
h2mk_1PntErr 
gpsSource 
WSA 
Error on point source colour H2K 
real 
4 
mag 
0.9999995e9 
ERROR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource 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 signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
h2mkExt 
calSource 
WSACalib 
Extended source colour H2K (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource 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 signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
h2mkExtErr 
calSource 
WSACalib 
Error on extended source colour H2K 
real 
4 
mag 
0.9999995e9 
ERROR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource 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 signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
h2mkPnt 
calSource, calSynopticSource 
WSACalib 
Point source colour H2K (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource 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 signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
h2mkPntErr 
calSource, calSynopticSource 
WSACalib 
Error on point source colour H2K 
real 
4 
mag 
0.9999995e9 
ERROR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource 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 signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
h2ndof 
calVariability 
WSACalib 
Number of degrees of freedom for chisquare 
smallint 
2 

9999 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 medianabsolute 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 chisquared 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 medianabsolute 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 chisquared 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 H2band 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 
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, calSynopticSource 
WSACalib 
ellipse fit celestial orientation in H2 
real 
4 
Degrees 
0.9999995e9 
POS_POSANG 
h2PA 
gpsJHKsource, gpsPointSource, gpsSource, gpsSourceRemeasurement, reliableGpsPointSource 
WSA 
ellipse fit celestial orientation in H2 
real 
4 
Degrees 
0.9999995e9 
POS_POSANG 
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 postprocessing error bits in H2 
int 
4 

0 
CODE_MISC 
Postprocessing 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 4byte 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 
gpsJHKsource, gpsPointSource, gpsSource, gpsSourceRemeasurement, reliableGpsPointSource 
WSA 
additional WFAU postprocessing error bits in H2 
int 
4 

0 
CODE_MISC 
h2probVar 
calVariability 
WSACalib 
Probability of variable from chisquare (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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 profilefitted H2 mag 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
h2PsfMagErr 
calSource 
WSACalib 
Error in point source profilefitted 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 
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 (profilefitted) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
h2SerMag2DErr 
calSource 
WSACalib 
Error in extended source H2 mag (profilefitted) 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 obsfirst 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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; UHS; also nonsurvey 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; UHS; also nonsurvey 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 
Hband 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 5sigma isophote. 
real 
4 


PHYS_AXISRATIO 
h_5sig_phi 
twomass_xsc 
2MASS 
H angle to 5sigma 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 3sigma isophote. 
real 
4 


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


CODE_MISC 
h_bisym_chi 
twomass_xsc 
2MASS 
H bisymmetric crosscorrelation chi. 
real 
4 


FIT_PARAM_VALUE 
h_bisym_rat 
twomass_xsc 
2MASS 
H bisymmetric 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 Hband 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 5sigma to 3sigma 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 HKs color, computed from the Hband and Ksband 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 Hband 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 
allwise_sc 
WISE 
2MASS Hband magnitude or magnitude upper limit of the associated 2MASS PSC source. This column is "null" if there is no associated 2MASS PSC source or if the 2MASS PSC Hband magnitude entry is "null". 
float 
8 
mag 


h_m_2mass 
wise_allskysc 
WISE 
2MASS Hband 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 Hband magnitude entry is default. 
real 
4 
mag 
0.9999995e9 

h_m_2mass 
wise_prelimsc 
WISE 
2MASS Hband 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 Hband 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 
Hband "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 halflight 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 1sigma uncertainty in 10 arcsec circular ap. mag. 
real 
4 
mag 

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

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

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

ERROR 
h_msig_2mass 
allwise_sc 
WISE 
2MASS Hband corrected photometric uncertainty of the associated 2MASS PSC source. This column is "null" if there is no associated 2MASS PSC source or if the 2MASS PSC Hband uncertainty entry is "null". 
float 
8 
mag 


h_msig_2mass 
wise_allskysc 
WISE 
2MASS Hband 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 Hband uncertainty entry is default. 
real 
4 
mag 
0.9999995e9 

h_msig_2mass 
wise_prelimsc 
WISE 
2MASS Hband 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 Hband uncertainty entry is default 
real 
4 
mag 
0.9999995e9 

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

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

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

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

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

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


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

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

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

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

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


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

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

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

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

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

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

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

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

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

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

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


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

ERROR 
h_msig_stdap 
twomass_psc 
2MASS 
Uncertainty in the Hband standard aperture magnitude. 
real 
4 
mag 

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

ERROR 
h_msigcom 
twomass_psc 
2MASS 
Combined, or total photometric uncertainty for the default Hband 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 Hband 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 Hband 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 5sigma to 3sigma percent area change. 
smallint 
2 


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

POS_POSANG 
h_psfchi 
twomass_psc 
2MASS 
Reduced chisquared goodnessoffit value for the Hband profilefit photometry made on the 1.3 s "Read_2" exposures. 
real 
4 


FIT_PARAM_VALUE 
h_psp 
twomass_scn 
2MASS 
Hband 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 
Base10 logarithm of the mode of the noise distribution for all point source detections in the scan, where the noise is estimated from the measured Hband 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 semimajor axis. 
real 
4 
arcsec 

EXTENSION_RAD 
h_r_eff 
twomass_xsc 
2MASS 
H halflight (integrated halfflux 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. semimajor 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. semimajor 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 
Hband 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 
RMSerror of Hband 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 
Hband "scan" signaltonoise ratio. 
real 
4 
mag 

INST_NOISE 
h_snr 
twomass_sixx2_psc 
2MASS 
H band "scan" signaltonoise ratio 
real 
4 



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


CODE_MISC 
h_zp_ap 
twomass_scn 
2MASS 
Photometric zeropoint for Hband aperture photometry. 
real 
4 
mag 

PHOT_ZP 
h_zp_ap 
twomass_sixx2_scn 
2MASS 
H band ap. calibration photometric zeropoint for scan 
real 
4 
mag 


h_zperr_ap 
twomass_scn 
2MASS 
RMSerror of zeropoint for Hband aperture photometry 
real 
4 
mag 

FIT_ERROR 
h_zperr_ap 
twomass_sixx2_scn 
2MASS 
H band ap. calibration rms error of zeropoint for scan 
real 
4 
mag 


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

POS_POSANG 
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 
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 
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 



hallFlux 
uhsDetection, uhsDetectionAll 
WSAUHS 
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 
UKIDSSDetection 
WSA 
error on Hall flux 
real 
4 
ADU 

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

ERROR 
hallFluxErr 
dxsDetection, gcsDetection, gcsListRemeasurement, gpsDetection, gpsListRemeasurement, lasDetection, lasListRemeasurement 
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 



hallFluxErr 
uhsDetection, uhsDetectionAll 
WSAUHS 
error on Hall flux {catalogue TType keyword: Hall_flux_err} 
real 
4 
ADU 

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

PHOT_INTMAG 
hallMag 
calDetection 
WSACalib 
Calibrated magnitude within circular aperture r_hall 
real 
4 
mag 

PHOT_INTMAG 
hallMag 
ptsDetection 
WSATransit 
Calibrated magnitude within circular aperture r_hall 
real 
4 
mag 

PHOT_INTMAG 
hallMag 
udsDetection 
WSA 
Not available in SE output 
real 
4 



hallMag 
uhsDetection, uhsDetectionAll 
WSAUHS 
Calibrated magnitude within circular aperture r_hall 
real 
4 
mag 

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

ERROR 
hallMagErr 
calDetection 
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 



hallMagErr 
uhsDetection, uhsDetectionAll 
WSAUHS 
Calibrated error on Hall magnitude 
real 
4 
mag 

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

EXTENSION_RAD 
hallRad 
calDetection 
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 
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 
pixels 

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

EXTENSION_RAD 
hAperMag1 
calSynopticSource 
WSACalib 
Extended source H aperture corrected mag (0.7 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 (0.7 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 medianabsolute 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 chisquared 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 medianabsolute 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 chisquared and number of degrees of freedom are also calculated. 
haStratPht 
calVarFrameSetInfo 
WSACalib 
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 medianabsolute 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 chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
haStratPht 
dxsVarFrameSetInfo, udsVarFrameSetInfo 
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 medianabsolute 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 chisquared 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 (16) for photometric statistics in the H band 
int 
4 

9999 

Aperture magnitude (16) 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 (16) for photometric statistics in the H band 
int 
4 

9999 

Aperture magnitude (16) 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 medianabsolute 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 chisquared 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 medianabsolute 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 chisquared 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 medianabsolute 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 chisquared 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 medianabsolute 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 chisquared 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 medianabsolute 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 chisquared 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 medianabsolute 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 chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 medianabsolute 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 chisquared 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 medianabsolute 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 chisquared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. 
hClass 
calSource, 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 
WSA 
discrete image classification flag in H 
smallint 
2 

9999 
CLASS_MISC 
hClassStat 
calSource, calSynopticSource 
WSACalib 
N(0,1) stellarnessofprofile 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 
WSA 
N(0,1) stellarnessofprofile statistic in H 
real 
4 

0.9999995e9 
STAT_PROP 
hClassStat 
gpsJHKsource, gpsPointSource, gpsSource, reliableGpsPointSource, reliableUdsSource, udsSource 
WSA 
SExtractor 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 medianabsolute 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 chisquared 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 medianabsolute 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 chisquared 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 medianabsolute 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 chisquared 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 medianabsolute 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 chisquared 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 postprocessing software based on testing the areal profiles aprof28 (these are set by CASU to 1 for deblended components, or positive values for nondeblended detections). We encode this in an information bit of ppErrBits for convenience when querying the merged source tables. 
hDeblend 
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 
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 postprocessing software based on testing the areal profiles aprof28 (these are set by CASU to 1 for deblended components, or positive values for nondeblended 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 

hdtFile 
Multiframe 
WSAUHS 
Name of global hdt file {image primary HDU keyword: HDTFILE} 
varchar 
32 

NONE 

hdtFileExt 
MultiframeDetector 
WSA 
Name of cameraspecific hdt file {image extension keyword: HDTFILE2} 
varchar 
32 

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

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

NONE 
?? 
hdtFileExt 
MultiframeDetector 
WSAUHS 
Name of cameraspecific hdt file {image extension keyword: HDTFILE2} 
varchar 
32 

NONE 
?? 
hEll 
calSource, calSynopticSource 
WSACalib 
1b/a, where a/b=semimajor/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 
WSA 
1b/a, where a/b=semimajor/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 
dxsJKsource, gcsPointSource, gcsSourceRemeasurement, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSourceRemeasurement, lasExtendedSource, lasPointSource, lasSourceRemeasurement, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource 
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; UHS; also nonsurvey 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; UHS; also nonsurvey 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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, 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 
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 singleframe Hband electronic glitch. 
smallint 
2 


CODE_MISC 
hgl 
twomass_sixx2_scn 
2MASS 
singleframe Hband glitch flag (0:not found1: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 
HIGH_BACKGROUND 
xmm3dr4 
XMM 
The flag is set to 1 (= True) if this detection comes from a field which, during manual screening, was considered to have a high background level which notably impacted on source detection. 
bit 
1 



hIntRms 
calVariability 
WSACalib 
Intrinsic rms in Hband 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 Hband 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hip 
hipparcos_new_reduction 
GAIADR1 
Hipparcos identifier 
int 
4 


meta.main;meta.id 
hip 
tgas_source 
GAIADR1 
Hipparcos identifier 
int 
4 


id.cross 
hip 
tycho2 
GAIADR1 
Hipparcos number 
varchar 
16 


meta.id.cross 
hip_tyc_oid 
gaia_hip_tycho2_match 
GAIADR1 
Initial Gaia Source List identifier for Hipparcos/Tycho2 
bigint 
8 


id.cross 
hisDefAst 
calVarFrameSetInfo 
WSACalib 
Use a default model for the astrometric noise in H band. 
tinyint 
1 

0 

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

0 

hisDefPht 
calVarFrameSetInfo 
WSACalib 
Use a default model for the photometric noise in H band. 
tinyint 
1 

0 

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

0 

hkiWS 
calVariability 
WSACalib 
WelchStetson 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 WelchStetson 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 
Semimajor axis of halflight ellipse 
real 
4 
pixel 


hMag 
gcsSourceRemeasurement, gpsSourceRemeasurement, lasSourceRemeasurement 
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_INTMAG 
hMag 
ukirtFSstars 
WSACalib 
H band total magnitude on the MKO(UFTI) system 
real 
4 
mag 

PHOT_INTMAG 
hMag 
ukirtFSstars 
WSAUHS 
H band total magnitude on the MKO(UFTI) system 
real 
4 
mag 

PHOT_INTMAG 
hMagErr 
gcsSourceRemeasurement, gpsSourceRemeasurement, lasSourceRemeasurement 
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 
hMagErr 
ukirtFSstars 
WSAUHS 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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, udsVariability 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
hmk 
lasSourceRemeasurement 
WSA 
Default colour HK (using appropriate mags) 
real 
4 
mag 

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

PHOT_COLOR 
hmk_1Err 
gcsSourceRemeasurement, gpsSourceRemeasurement 
WSA 
Error on colour HK 
real 
4 
mag 

ERROR 
hmk_1Ext 
gcsPointSource, gcsZYJHKsource, reliableGcsPointSource 
WSA 
Extended source colour HK (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
hmk_1Ext 
gcsSource 
WSA 
Extended source colour HK (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource 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 signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmk_1ExtErr 
gcsPointSource, gcsZYJHKsource, reliableGcsPointSource 
WSA 
Error on extended source colour HK 
real 
4 
mag 
0.9999995e9 
ERROR 
hmk_1ExtErr 
gcsSource 
WSA 
Error on extended source colour HK 
real 
4 
mag 
0.9999995e9 
ERROR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource 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 signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmk_1Pnt 
gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, reliableGcsPointSource, reliableGpsPointSource 
WSA 
Point source colour HK (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
hmk_1Pnt 
gcsSource, gpsSource 
WSA 
Point source colour HK (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource 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 signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmk_1PntErr 
gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, reliableGcsPointSource, reliableGpsPointSource 
WSA 
Error on point source colour HK 
real 
4 
mag 
0.9999995e9 
ERROR 
hmk_1PntErr 
gcsSource, gpsSource 
WSA 
Error on point source colour HK 
real 
4 
mag 
0.9999995e9 
ERROR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource 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 signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmkErr 
lasSourceRemeasurement 
WSA 
Error on colour HK 
real 
4 
mag 

ERROR 
hmkExt 
calSource 
WSACalib 
Extended source colour HK (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource 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 signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmkExt 
dxsJKsource, lasExtendedSource, lasPointSource, lasYJHKsource, reliableDxsSource, reliableLasPointSource, reliableUdsSource 
WSA 
Extended source colour HK (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
hmkExt 
dxsSource, lasSource, udsSource 
WSA 
Extended source colour HK (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource 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 signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmkExtErr 
calSource 
WSACalib 
Error on extended source colour HK 
real 
4 
mag 
0.9999995e9 
ERROR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource 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 signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmkExtErr 
dxsJKsource, lasExtendedSource, lasPointSource, lasYJHKsource, reliableDxsSource, reliableLasPointSource, reliableUdsSource 
WSA 
Error on extended source colour HK 
real 
4 
mag 
0.9999995e9 
ERROR 
hmkExtErr 
dxsSource, lasSource, udsSource 
WSA 
Error on extended source colour HK 
real 
4 
mag 
0.9999995e9 
ERROR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource 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 signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmkPnt 
calSource, calSynopticSource 
WSACalib 
Point source colour HK (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource 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 signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmkPnt 
dxsJKsource, lasExtendedSource, lasPointSource, lasYJHKsource, reliableDxsSource, reliableLasPointSource, reliableUdsSource 
WSA 
Point source colour HK (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
hmkPnt 
dxsSource, lasSource, udsSource 
WSA 
Point source colour HK (using aperMag3) 
real 
4 
mag 
0.9999995e9 
PHOT_COLOR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource 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 signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmkPntErr 
calSource, calSynopticSource 
WSACalib 
Error on point source colour HK 
real 
4 
mag 
0.9999995e9 
ERROR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource 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 signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hmkPntErr 
dxsJKsource, lasExtendedSource, lasPointSource, lasYJHKsource, reliableDxsSource, reliableLasPointSource, reliableUdsSource 
WSA 
Error on point source colour HK 
real 
4 
mag 
0.9999995e9 
ERROR 
hmkPntErr 
dxsSource, lasSource, udsSource 
WSA 
Error on point source colour HK 
real 
4 
mag 
0.9999995e9 
ERROR 
Default colours from pairs of adjacent passbands within a given set (e.g. YJ, JH and HK for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the pointsource 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 signaltonoise. At some point in the future, this may be changed such that pointsource colours will be computed from the PSFfitted measures and extended source colours computed from the 2d Sersic model profile fits. 
hndof 
calVariability 
WSACalib 
Number of degrees of freedom for chisquare 
smallint 
2 

9999 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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, udsVariability 
WSA 
Number of degrees of freedom for chisquare 
smallint 
2 

9999 

The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 medianabsolute 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 chisquared 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 medianabsolute 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 chisquared 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 medianabsolute 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 chisquared 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 medianabsolute 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 chisquared 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 Hband 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 Hband 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 
gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, lasExtendedSource, lasPointSource, lasYJHKsource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource 
WSA 
DEPRECATED (do not use) 
bigint 
8 

99999999 
ID_NUMBER 
hObjID 
gcsSource, gcsSourceRemeasurement, gpsSource, gpsSourceRemeasurement, lasSource, lasSourceRemeasurement 
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 

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

hp_mag 
hipparcos_new_reduction 
GAIADR1 
Hipparcos magnitude 
float 
8 
mag 

em.opt;phot.mag 
hPA 
calSource, calSynopticSource 
WSACalib 
ellipse fit celestial orientation in H 
real 
4 
Degrees 
0.9999995e9 
POS_POSANG 
hPA 
dxsJKsource, dxsSource, gcsPointSource, gcsSource, gcsSourceRemeasurement, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, gpsSourceRemeasurement, lasExtendedSource, lasPointSource, lasSource, lasSourceRemeasurement, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource, udsSource 
WSA 
ellipse fit celestial orientation in H 
real 
4 
Degrees 
0.9999995e9 
POS_POSANG 
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 postprocessing error bits in H 
int 
4 

0 
CODE_MISC 
Postprocessing 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 4byte 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 
dxsJKsource, gcsPointSource, gcsSourceRemeasurement, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, gpsSourceRemeasurement, lasExtendedSource, lasPointSource, lasSourceRemeasurement, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource, udsSource 
WSA 
additional WFAU postprocessing error bits in H 
int 
4 

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

0 
CODE_MISC 
Postprocessing 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 4byte 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 chisquare (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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquare (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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 profilefitted 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 profilefitted 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 profilefitted 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 profilefitted 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_HARDNESSRATIO 
hr2 
rosat_bsc, rosat_fsc 
ROSAT 
hardness ratio 2 
float 
8 


SPECT_HARDNESSRATIO 
hry 
twomass_scn 
2MASS 
Flag indicating the Hband array configuration for the camera. 
smallint 
2 


CODE_MISC 
hry 
twomass_sixx2_scn 
2MASS 
Hband 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 
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 
WSA 
the running number of the H remeasurement 
int 
4 

99999999 
ID_NUMBER 
hSerMag2D 
calSource 
WSACalib 
Extended source H mag (profilefitted) 
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 (profilefitted) 
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 (profilefitted) 
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 (profilefitted) 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. 
htm20 
allwise_sc 
WISE 
Level 20 HTM spatial index key 
bigint 
8 



HTMID 
twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0, xmm3dr4 
XMM 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


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

99999999 
pos.eq 
htmID 
CurrentAstrometry 
WSATransit 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates of device centre 
bigint 
8 

99999999 
pos.eq 
htmID 
CurrentAstrometry 
WSAUHS 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates of device centre 
bigint 
8 

99999999 
pos.eq 
htmID 
CurrentAstrometry, PreviousAstrometry 
WSA 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates of device centre 
bigint 
8 

99999999 
pos.eq 
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, udsMergeLog, udsSource 
WSA 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


POS_GENERAL 
htmID 
calDetection, calMergeLog, calSource, calSynopticMergeLog, calSynopticSource 
WSACalib 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


POS_GENERAL 
htmID 
first08Jul16Source, firstSource, firstSource12Feb16 
FIRST 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


POS_GENERAL 
htmID 
gaia_source, hipparcos_new_reduction, igsl_source, tgas_source, tycho2 
GAIADR1 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


pos.eq 
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 coordinates 
bigint 
8 


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


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


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


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


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


POS_GENERAL 
htmID 
uhsDetection, uhsDetectionAll, uhsMergeLog, uhsSource, uhsSourceAll 
WSAUHS 
Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial coordinates 
bigint 
8 


POS_GENERAL 
htmID 
wise_allskysc, wise_prelimsc 
WISE 
Hierarchical Triangular Mesh (HTM) index for equatorial coordinates (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 obsfirst 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 obsfirst 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 
meta.note;obs 
humidity 
Multiframe 
WSACalib 
Relative Humidity {image primary HDU keyword: HUMIDITY} 
real 
4 

0.9999995e9 
meta.note;obs 
humidity 
Multiframe 
WSATransit 
Relative Humidity {image primary HDU keyword: HUMIDITY} 
real 
4 

0.9999995e9 
meta.note;obs 
humidity 
Multiframe 
WSAUHS 
Relative Humidity {image primary HDU keyword: HUMIDITY} 
real 
4 

0.9999995e9 
meta.note;obs 
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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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 chisquared is calculated, assuming a nonvariable object which has the noise from the expectedrms and mean calculated as above. The probVar statistic assumes a chisquared 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; UHS; also nonsurvey 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; UHS; also nonsurvey 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 

hz10cd 
Multiframe 
WSAUHS 
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 

hz10ch 
Multiframe 
WSAUHS 
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 

hz10sd 
Multiframe 
WSAUHS 
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 

hz10sh 
Multiframe 
WSAUHS 
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 

hz5cd 
Multiframe 
WSAUHS 
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 

hz5ch 
Multiframe 
WSAUHS 
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 

hz5sd 
Multiframe 
WSAUHS 
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 

hz5sh 
Multiframe 
WSAUHS 
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 

hz6cd 
Multiframe 
WSAUHS 
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 

hz6ch 
Multiframe 
WSAUHS 
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 

hz6sd 
Multiframe 
WSAUHS 
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 

hz6sh 
Multiframe 
WSAUHS 
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 

hz9cd 
Multiframe 
WSAUHS 
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 

hz9ch 
Multiframe 
WSAUHS 
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 

hz9sd 
Multiframe 
WSAUHS 
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 

hz9sh 
Multiframe 
WSAUHS 
Trefoil: HZ9SH {image primary HDU keyword: HZ9SH} 
real 
4 

0.9999995e9 
