N 
Name  Schema Table  Database  Description  Type  Length  Unit  Default Value  Unified Content Descriptor 
N1 
glimpse_hrc_inter, glimpse_mca_inter 
GLIMPSE 
Possible number of detections for band 1 
int 
4 

9 

N2 
glimpse_hrc_inter, glimpse_mca_inter 
GLIMPSE 
Possible number of detections for band 2 
int 
4 

9 

N3 
glimpse_hrc_inter, glimpse_mca_inter 
GLIMPSE 
Possible number of detections for band 3 
int 
4 

9 

N3_6 
glimpse1_hrc, glimpse1_mca, glimpse2_hrc, glimpse2_mca 
GLIMPSE 
Number of possible detections for 3.6um IRAC (Band 1) 
int 
4 

9 

N4 
glimpse_hrc_inter, glimpse_mca_inter 
GLIMPSE 
Possible number of detections for band 4 
int 
4 

9 

N4_5 
glimpse1_hrc, glimpse1_mca, glimpse2_hrc, glimpse2_mca 
GLIMPSE 
Number of possible detections for 4.5um IRAC (Band 2) 
int 
4 

9 

N5_8 
glimpse1_hrc, glimpse1_mca, glimpse2_hrc, glimpse2_mca 
GLIMPSE 
Number of possible detections for 5.8um IRAC (Band 3) 
int 
4 

9 

N8_0 
glimpse1_hrc, glimpse1_mca, glimpse2_hrc, glimpse2_mca 
GLIMPSE 
Number of possible detections for 8.0um IRAC (Band 4) 
int 
4 

9 

n_2mass 
allwise_sc 
WISE 
The number of 2MASS PSC entries found within a 3" radius of the WISE source position. If more than one 2MASS PSC falls within 3" of the WISE position, the closest 2MASS PSC entry is listed. This column is zero if there is no associated 2MASS PSC source. 
int 
4 



n_2mass 
wise_allskysc 
WISE 
The number of 2MASS PSC entries found within a 3" radius of the WISE source position. If more than one 2MASS PSC falls within 3" of the WISE position, the closest 2MASS PSC entry is listed. This column is default if there is no associated 2MASS PSC source 
smallint 
2 

9999 

n_2mass 
wise_prelimsc 
WISE 
The number of 2MASS PSC entries found within a 3" radius of the WISE source position If more than one 2MASS PSC falls within 3" of the WISE position, the closest 2MASS PSC entry is listed. This column is default if there is no associated 2MASS PSC source 
smallint 
2 

9999 

n_aw 
catwise_2020, catwise_prelim 
WISE 
number of AllWISE matches within 2.75 asec 
int 
4 



n_blank 
twomass_xsc 
2MASS 
number of blanked source records. 
smallint 
2 


NUMBER 
N_DETECTIONS 
twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 
XMM 
The number of detections of the unique source SRCID used to derive the averaged values. 
int 
4 



N_DETECTIONS 
xmm3dr4 
XMM 
The number of detections of the unique source SRCID used to derive the averaged values. 
smallint 
2 



n_ext 
twomass_scn 
2MASS 
Number of regular extended sources detected in scan. 
int 
4 


NUMBER 
n_ext 
twomass_sixx2_scn 
2MASS 
number of regular extended sources detected in scan 
int 
4 



N_SPEC 
mgcBrightSpec 
MGC 
Total number of spectra for this object 
smallint 
2 



n_sub 
twomass_xsc 
2MASS 
number of subtracted source records. 
smallint 
2 


NUMBER 
na 
allwise_sc 
WISE 
Active deblending flag. Indicates if a single detection was split into multiple sources in the process of profilefitting: 0  the source is not actively deblended; 1  the source is actively deblended. 
int 
4 



na 
catwise_2020, catwise_prelim 
WISE 
number of actively deblended components 
int 
4 



na 
wise_allskysc 
WISE 
Active deblending flag. Indicates if a single detection was split into multiple sources in the process of profilefitting: 0  the source is not actively deblended; 1  the source is actively deblended. 
smallint 
2 

9999 

na 
wise_prelimsc 
WISE 
Active deblending flag Indicates if a single detection was split into multiple sources in the process of profilefitting: 0  the source is not actively deblended; 1  the source is actively deblended. 
smallint 
2 

9999 

name 
Filter 
WSA 
The name of the filter, eg. "MKO J", "WFCAM Y" etc. 
varchar 
16 


meta.note 
name 
Filter 
WSACalib 
The name of the filter, eg. "MKO J", "WFCAM Y" etc. 
varchar 
16 


meta.note 
name 
Filter 
WSATransit 
The name of the filter, eg. "MKO J", "WFCAM Y" etc. 
varchar 
16 


meta.note 
name 
Filter 
WSAUHS 
The name of the filter, eg. "MKO J", "WFCAM Y" etc. 
varchar 
16 


meta.note 
name 
RequiredMatchedApertureProduct 
WSA 
the name of the matched aperture product 
varchar 
16 


?? 
name 
RequiredMatchedApertureProduct 
WSAUHS 
the name of the matched aperture product 
varchar 
16 


?? 
name 
RequiredMergeLogMultiEpoch 
WSAUHS 
Name of the stacked product 
varchar 
64 


?? 
name 
RequiredMergeLogMultiEpoch, RequiredStack 
WSA 
Name of the stacked product 
varchar 
64 


?? 
name 
RequiredMosaic 
WSA 
Name of the mosaiced product 
varchar 
64 


?? 
name 
RequiredMosaic 
WSACalib 
Name of the mosaiced product 
varchar 
64 


?? 
name 
RequiredMosaic 
WSATransit 
Name of the mosaiced product 
varchar 
64 


?? 
name 
RequiredMosaic 
WSAUHS 
Name of the mosaiced product 
varchar 
64 


?? 
name 
RequiredMosaicTopLevel 
WSAUHS 
Name of the mosaiced product set up 
varchar 
64 


?? 
name 
RequiredRegion 
WSA 
Name of the region 
varchar 
64 


?? 
name 
RequiredRegion 
WSAUHS 
Name of the region 
varchar 
64 


?? 
name 
Survey 
WSA 
The short name for the survey 
varchar 
128 


?? 
name 
Survey 
WSACalib 
The short name for the survey 
varchar 
128 


?? 
name 
Survey 
WSATransit 
The short name for the survey 
varchar 
128 


?? 
name 
Survey 
WSAUHS 
The short name for the survey 
varchar 
128 


?? 
name 
iras_asc, iras_psc 
IRAS 
Source Name 
varchar 
11 


ID_MAIN 
name 
ukirtFSstars 
WSA 
reference name of field 
varchar 
16 

NONE 
???? 
name 
ukirtFSstars 
WSACalib 
reference name of field 
varchar 
16 

NONE 
???? 
name 
ukirtFSstars 
WSAUHS 
reference name of field 
varchar 
16 

NONE 
???? 
nb 
allwise_sc 
WISE 
Number of PSF components used simultaneously in the profilefitting for this source. This number includes the source itself, so the minimum value of nb is "1". Nb is greater than "1" when the source is fit concurrently with other nearby detections (passive deblending), or when a single source is split into two components during the fitting process (active deblending). 
int 
4 



nb 
catwise_2020, catwise_prelim 
WISE 
number of blend components used in each fit 
int 
4 



nb 
wise_allskysc 
WISE 
Number of PSF components used simultaneously in the profilefitting for this source. This number includes the source itself, so the minimum value of nb is "1". Nb is greater than "1" when the source is fit concurrently with other nearby detections (passive deblending), or when a single source is split into two components during the fitting process (active deblending). 
smallint 
2 

9999 

nb 
wise_prelimsc 
WISE 
Number of PSF components used simultaneously in the profilefitting for this source This number includes the source itself, so the minimum value of nb is "1". Nb is greater than "1" when the source is fit concurrently with other nearby detections (passive deblending), or when a single source is split into two components during the fitting process (active deblending). 
smallint 
2 

9999 

nbjAperMag1 
calSynopticSource 
WSACalib 
Extended source Nbj aperture corrected mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
nbjAperMag1Err 
calSynopticSource 
WSACalib 
Error in extended source Nbj mag (1.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
nbjAperMag2 
calSynopticSource 
WSACalib 
Extended source Nbj aperture corrected mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
nbjAperMag2Err 
calSynopticSource 
WSACalib 
Error in extended source Nbj mag (1.4 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
nbjAperMag3 
calSource 
WSACalib 
Default point/extended source Nbj aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
nbjAperMag3 
calSynopticSource 
WSACalib 
Default point/extended source Nbj aperture corrected mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
nbjAperMag3Err 
calSource, calSynopticSource 
WSACalib 
Error in default point/extended source Nbj mag (2.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
nbjAperMag4 
calSource, calSynopticSource 
WSACalib 
Extended source Nbj aperture corrected mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
nbjAperMag4Err 
calSource, calSynopticSource 
WSACalib 
Error in extended source Nbj mag (2.8 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
nbjAperMag5 
calSynopticSource 
WSACalib 
Extended source Nbj aperture corrected mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
nbjAperMag5Err 
calSynopticSource 
WSACalib 
Error in extended source Nbj mag (4.0 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
nbjAperMag6 
calSource 
WSACalib 
Extended source Nbj aperture corrected mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
nbjAperMag6Err 
calSource 
WSACalib 
Error in extended source Nbj mag (5.7 arcsec aperture diameter) 
real 
4 
mag 
0.9999995e9 
ERROR 
nbjaStratAst 
calVarFrameSetInfo 
WSACalib 
Strateva parameter, a, in fit to astrometric rms vs magnitude in Nbj 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. 
nbjaStratPht 
calVarFrameSetInfo 
WSACalib 
Strateva parameter, a, in fit to photometric rms vs magnitude in Nbj 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. 
nbjbestAper 
calVariability 
WSACalib 
Best aperture (16) for photometric statistics in the Nbj 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) 
nbjbStratAst 
calVarFrameSetInfo 
WSACalib 
Strateva parameter, b, in fit to astrometric rms vs magnitude in Nbj 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. 
nbjbStratPht 
calVarFrameSetInfo 
WSACalib 
Strateva parameter, b, in fit to photometric rms vs magnitude in Nbj 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. 
nbjchiSqAst 
calVarFrameSetInfo 
WSACalib 
Goodness of fit of Strateva function to astrometric data in Nbj 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. 
nbjchiSqpd 
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. 
nbjchiSqPht 
calVarFrameSetInfo 
WSACalib 
Goodness of fit of Strateva function to photometric data in Nbj 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. 
nbjClass 
calSource, calSynopticSource 
WSACalib 
discrete image classification flag in Nbj 
smallint 
2 

9999 
CLASS_MISC 
nbjClassStat 
calSource, calSynopticSource 
WSACalib 
N(0,1) stellarnessofprofile statistic in Nbj 
real 
4 

0.9999995e9 
STAT_PROP 
nbjcStratAst 
calVarFrameSetInfo 
WSACalib 
Strateva parameter, c, in fit to astrometric rms vs magnitude in Nbj 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. 
nbjcStratPht 
calVarFrameSetInfo 
WSACalib 
Strateva parameter, c, in fit to photometric rms vs magnitude in Nbj 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. 
nbjDeblend 
calSource 
WSACalib 
placeholder flag indicating parent/child relation in Nbj 
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. 
nbjDeblend 
calSynopticSource 
WSACalib 
placeholder flag indicating parent/child relation in Nbj 
int 
4 

99999999 
CODE_MISC 
nbjEll 
calSource, calSynopticSource 
WSACalib 
1b/a, where a/b=semimajor/minor axes in Nbj 
real 
4 

0.9999995e9 
PHYS_ELLIPTICITY 
nbjeNum 
calMergeLog, calSynopticMergeLog 
WSACalib 
the extension number of this Nbj frame 
tinyint 
1 


NUMBER 
nbjErrBits 
calSource, calSynopticSource 
WSACalib 
processing warning/error bitwise flags in Nbj 
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. 
nbjEta 
calSource, calSynopticSource 
WSACalib 
Offset of Nbj 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. 
nbjexpML 
calVarFrameSetInfo 
WSACalib 
Expected magnitude limit of frameSet in this in Nbj 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. 
nbjExpRms 
calVariability 
WSACalib 
Rms calculated from polynomial fit to modal RMS as a function of magnitude in Nbj 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. 
nbjGausig 
calSource, calSynopticSource 
WSACalib 
RMS of axes of ellipse fit in Nbj 
real 
4 
pixels 
0.9999995e9 
MORPH_PARAM 
nbjHallMag 
calSource 
WSACalib 
Total point source Nbj mag 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
nbjHallMagErr 
calSource 
WSACalib 
Error in total point source Nbj mag 
real 
4 
mag 
0.9999995e9 
ERROR 
nbjIntRms 
calVariability 
WSACalib 
Intrinsic rms in Nbjband 
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. 
nbjisDefAst 
calVarFrameSetInfo 
WSACalib 
Use a default model for the astrometric noise in Nbj band. 
tinyint 
1 

0 

nbjisDefPht 
calVarFrameSetInfo 
WSACalib 
Use a default model for the photometric noise in Nbj band. 
tinyint 
1 

0 

nbjMagMAD 
calVariability 
WSACalib 
Median Absolute Deviation of Nbj 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. 
nbjMagRms 
calVariability 
WSACalib 
rms of Nbj 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. 
nbjmaxCadence 
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. 
nbjMaxMag 
calVariability 
WSACalib 
Maximum magnitude in Nbj 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. 
nbjmeanMag 
calVariability 
WSACalib 
Mean Nbj 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. 
nbjmedCadence 
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. 
nbjmedianMag 
calVariability 
WSACalib 
Median Nbj 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. 
nbjmfID 
calMergeLog, calSynopticMergeLog 
WSACalib 
the UID of the relevant Nbj multiframe 
bigint 
8 


ID_FRAME 
nbjminCadence 
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. 
nbjMinMag 
calVariability 
WSACalib 
Minimum magnitude in Nbj 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. 
nbjmjExt 
calSource 
WSACalib 
Extended source colour NbjJ (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. 
nbjmjExtErr 
calSource 
WSACalib 
Error on extended source colour NbjJ 
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. 
nbjmjPnt 
calSource, calSynopticSource 
WSACalib 
Point source colour NbjJ (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. 
nbjmjPntErr 
calSource, calSynopticSource 
WSACalib 
Error on point source colour NbjJ 
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. 
nbjndof 
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. 
nbjnDofAst 
calVarFrameSetInfo 
WSACalib 
Number of degrees of freedom of astrometric fit in Nbj 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. 
nbjnDofPht 
calVarFrameSetInfo 
WSACalib 
Number of degrees of freedom of photometric fit in Nbj 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. 
nbjnFlaggedObs 
calVariability 
WSACalib 
Number of detections in Nbj 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. 
nbjnGoodObs 
calVariability 
WSACalib 
Number of good detections in Nbj 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. 
nbjNgt3sig 
calVariability 
WSACalib 
Number of good detections in Nbjband 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. 
nbjnMissingObs 
calVariability 
WSACalib 
Number of Nbj 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. 
nbjPA 
calSource, calSynopticSource 
WSACalib 
ellipse fit celestial orientation in Nbj 
real 
4 
Degrees 
0.9999995e9 
POS_POSANG 
nbjPetroMag 
calSource 
WSACalib 
Extended source Nbj mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
nbjPetroMagErr 
calSource 
WSACalib 
Error in extended source Nbj mag (Petrosian) 
real 
4 
mag 
0.9999995e9 
ERROR 
nbjppErrBits 
calSource, calSynopticSource 
WSACalib 
additional WFAU postprocessing error bits in Nbj 
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. 
nbjprobVar 
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. 
nbjPsfMag 
calSource 
WSACalib 
Point source profilefitted Nbj mag 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
nbjPsfMagErr 
calSource 
WSACalib 
Error in point source profilefitted Nbj mag 
real 
4 
mag 
0.9999995e9 
ERROR 
nbjSeqNum 
calSource, calSynopticSource 
WSACalib 
the running number of the Nbj detection 
int 
4 

99999999 
ID_NUMBER 
nbjSerMag2D 
calSource 
WSACalib 
Extended source Nbj mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
PHOT_MAG 
nbjSerMag2DErr 
calSource 
WSACalib 
Error in extended source Nbj mag (profilefitted) 
real 
4 
mag 
0.9999995e9 
ERROR 
nbjskewness 
calVariability 
WSACalib 
Skewness in Nbj 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. 
nbjtotalPeriod 
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. 
nbjVarClass 
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. 
nbjXi 
calSource, calSynopticSource 
WSACalib 
Offset of Nbj 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. 
nc 
hipparcos_new_reduction 
GAIADR1 
Number of components 
int 
4 


meta.number 
ndet 
twomass_psc 
2MASS 
Frame detection statistics. 
varchar 
6 


NUMBER 
ndet 
twomass_sixx2_psc 
2MASS 
number of >3sig. ap. mag measurements, # possible (jjhhkk) 
varchar 
6 



nDetections 
ObjectThin 
PS1DR2 
Number of single epoch detections in all filters. 
smallint 
2 

999 

NED_CLASS 
mgcBrightSpec 
MGC 
MGC translation of NED_IDENT 
smallint 
2 



NED_DEC 
mgcBrightSpec 
MGC 
NED object declination in deg (J2000) 
float 
8 



NED_IDENT 
mgcBrightSpec 
MGC 
NED identification 
varchar 
4 



NED_N 
mgcBrightSpec 
MGC 
Number of NED objects matched to this MGC object 
smallint 
2 



NED_NAME 
mgcBrightSpec 
MGC 
NED object name 
varchar 
32 



NED_RA 
mgcBrightSpec 
MGC 
NED object right ascension in deg (J2000) 
float 
8 



NED_ZHELIO 
mgcBrightSpec 
MGC 
NED heliocentric redshift 
real 
4 



NED_ZQUAL 
mgcBrightSpec 
MGC 
NED redshift quality 
tinyint 
1 



neighboursSchema 
Programme 
WSA 
Script file that describes the neighbour tables schema for this programme 
varchar 
64 


?? 
neighboursSchema 
Programme 
WSACalib 
Script file that describes the neighbour tables schema for this programme 
varchar 
64 


?? 
neighboursSchema 
Programme 
WSATransit 
Script file that describes the neighbour tables schema for this programme 
varchar 
64 


?? 
neighboursSchema 
Programme 
WSAUHS 
Script file that describes the neighbour tables schema for this programme 
varchar 
64 


?? 
neighbourTable 
RequiredNeighbours 
WSA 
the name of the neighbour join table 
varchar 
256 


meta.id;meta.dataset 
neighbourTable 
RequiredNeighbours 
WSACalib 
the name of the neighbour join table 
varchar 
256 


meta.id;meta.dataset 
neighbourTable 
RequiredNeighbours 
WSATransit 
the name of the neighbour join table 
varchar 
256 


meta.id;meta.dataset 
neighbourTable 
RequiredNeighbours 
WSAUHS 
the name of the neighbour join table 
varchar 
256 


meta.id;meta.dataset 
nEpochs 
RequiredMapAverages 
WSA 
Number of frames to average over 
int 
4 

99999999 

nEpochs 
RequiredMapAverages 
WSAUHS 
Number of frames to average over 
int 
4 

99999999 

new_matched_transits 
gaia_source 
GAIAEDR3 
The number of transits newly incorporated into an existing source in the current cycle 
smallint 
2 


meta.number 
newBrframe 
calMergeLog, calSynopticMergeLog 
WSACalib 
new/old flag (1/0) of this detector image 
tinyint 
1 


CODE_MISC 
newFrameSet 
calMergeLog, calSynopticMergeLog 
WSACalib 
Flag used internally by curation applications 
tinyint 
1 


CODE_MISC 
newFrameSet 
dxsJKmergeLog, dxsMergeLog, gcsMergeLog, gcsZYJHKmergeLog, gpsJHKmergeLog, gpsMergeLog, lasMergeLog, lasYJHKmergeLog, udsMergeLog 
WSA 
Flag used internally by curation applications 
tinyint 
1 


CODE_MISC 
newFrameSet 
lasYselJRemeasMergeLog 
WSA 
Flag used internally by curation applications 
tinyint 
1 


meta.code 
newFrameSet 
uhsMergeLog 
WSAUHS 
Flag used internally by curation applications 
tinyint 
1 


CODE_MISC 
newH2frame 
calMergeLog, calSynopticMergeLog 
WSACalib 
new/old flag (1/0) of this detector image 
tinyint 
1 


CODE_MISC 
newH2frame 
gpsJHKmergeLog, gpsMergeLog 
WSA 
new/old flag (1/0) of this detector image 
tinyint 
1 


CODE_MISC 
newHframe 
calMergeLog, calSynopticMergeLog 
WSACalib 
new/old flag (1/0) of this detector image 
tinyint 
1 


CODE_MISC 
newHframe 
dxsJKmergeLog, dxsMergeLog, gcsMergeLog, gcsZYJHKmergeLog, gpsJHKmergeLog, gpsMergeLog, lasMergeLog, lasYJHKmergeLog, udsMergeLog 
WSA 
new/old flag (1/0) of this detector image 
tinyint 
1 


CODE_MISC 
newHframe 
lasYselJRemeasMergeLog 
WSA 
new/old flag (1/0) of this detector image 
tinyint 
1 


meta.code;em.IR.H 
newJ_1frame 
lasMergeLog, lasYJHKmergeLog 
WSA 
new/old flag (1/0) of this detector image 
tinyint 
1 


CODE_MISC 
newJ_2frame 
lasMergeLog, lasYJHKmergeLog 
WSA 
new/old flag (1/0) of this detector image 
tinyint 
1 


CODE_MISC 
newJframe 
calMergeLog, calSynopticMergeLog 
WSACalib 
new/old flag (1/0) of this detector image 
tinyint 
1 


CODE_MISC 
newJframe 
dxsJKmergeLog, dxsMergeLog, gcsMergeLog, gcsZYJHKmergeLog, gpsJHKmergeLog, gpsMergeLog, lasMergeLog, lasYJHKmergeLog, udsMergeLog 
WSA 
new/old flag (1/0) of this detector image 
tinyint 
1 


CODE_MISC 
newJframe 
lasYselJRemeasMergeLog 
WSA 
new/old flag (1/0) of this detector image 
tinyint 
1 


meta.code;em.IR.J 
newJframe 
uhsMergeLog 
WSAUHS 
new/old flag (1/0) of this detector image 
tinyint 
1 


CODE_MISC 
newK_1frame 
gcsMergeLog, gcsZYJHKmergeLog, gpsJHKmergeLog, gpsMergeLog 
WSA 
new/old flag (1/0) of this detector image 
tinyint 
1 


CODE_MISC 
newK_2frame 
gcsMergeLog, gcsZYJHKmergeLog, gpsJHKmergeLog, gpsMergeLog 
WSA 
new/old flag (1/0) of this detector image 
tinyint 
1 


CODE_MISC 
newKframe 
calMergeLog, calSynopticMergeLog 
WSACalib 
new/old flag (1/0) of this detector image 
tinyint 
1 


CODE_MISC 
newKframe 
dxsJKmergeLog, dxsMergeLog, gcsMergeLog, gcsZYJHKmergeLog, gpsJHKmergeLog, gpsMergeLog, lasMergeLog, lasYJHKmergeLog, udsMergeLog 
WSA 
new/old flag (1/0) of this detector image 
tinyint 
1 


CODE_MISC 
newKframe 
lasYselJRemeasMergeLog 
WSA 
new/old flag (1/0) of this detector image 
tinyint 
1 


meta.code;em.IR.K 
newKframe 
uhsMergeLog 
WSAUHS 
new/old flag (1/0) of this detector image 
tinyint 
1 


CODE_MISC 
newlyIngested 
Multiframe 
WSA 
Curation flag for internal use only (0=no, 1=yes) 
tinyint 
1 

1 
?? 
newlyIngested 
Multiframe 
WSACalib 
Curation flag for internal use only (0=no, 1=yes) 
tinyint 
1 

1 
?? 
newlyIngested 
Multiframe 
WSATransit 
Curation flag for internal use only (0=no, 1=yes) 
tinyint 
1 

1 
?? 
newlyIngested 
Multiframe 
WSAUHS 
Curation flag for internal use only (0=no, 1=yes) 
tinyint 
1 

1 
?? 
newNbjframe 
calMergeLog, calSynopticMergeLog 
WSACalib 
new/old flag (1/0) of this detector image 
tinyint 
1 


CODE_MISC 
newYframe 
calMergeLog, calSynopticMergeLog 
WSACalib 
new/old flag (1/0) of this detector image 
tinyint 
1 


CODE_MISC 
newYframe 
gcsMergeLog, gcsZYJHKmergeLog, lasMergeLog, lasYJHKmergeLog 
WSA 
new/old flag (1/0) of this detector image 
tinyint 
1 


CODE_MISC 
newYframe 
lasYselJRemeasMergeLog 
WSA 
new/old flag (1/0) of this detector image 
tinyint 
1 


meta.code;em.IR.NIR 
newZframe 
calMergeLog, calSynopticMergeLog 
WSACalib 
new/old flag (1/0) of this detector image 
tinyint 
1 


CODE_MISC 
newZframe 
gcsMergeLog, gcsZYJHKmergeLog 
WSA 
new/old flag (1/0) of this detector image 
tinyint 
1 


CODE_MISC 
nFlag 
rosat_bsc, rosat_fsc 
ROSAT 
nearby sources affecting SASS flux determination 
varchar 
1 


CODE_MISC 
nFoc 
Multiframe 
WSA 
Number of positions in focus scan {image primary HDU keyword: NFOC} 
smallint 
2 

9999 
meta.number 
nFoc 
Multiframe 
WSACalib 
Number of positions in focus scan {image primary HDU keyword: NFOC} 
smallint 
2 

9999 
meta.number 
nFoc 
Multiframe 
WSATransit 
Number of positions in focus scan {image primary HDU keyword: NFOC} 
smallint 
2 

9999 
meta.number 
nFoc 
Multiframe 
WSAUHS 
Number of positions in focus scan {image primary HDU keyword: NFOC} 
smallint 
2 

9999 
meta.number 
nFocScan 
Multiframe 
WSA 
Number of focus scans in focus test {image primary HDU keyword: NFOCSCAN} 
smallint 
2 

9999 
meta.number 
nFocScan 
Multiframe 
WSACalib 
Number of focus scans in focus test {image primary HDU keyword: NFOCSCAN} 
smallint 
2 

9999 
meta.number 
nFocScan 
Multiframe 
WSATransit 
Number of focus scans in focus test {image primary HDU keyword: NFOCSCAN} 
smallint 
2 

9999 
meta.number 
nFocScan 
Multiframe 
WSAUHS 
Number of focus scans in focus test {image primary HDU keyword: NFOCSCAN} 
smallint 
2 

9999 
meta.number 
nFrames 
calVariability 
WSACalib 
Number of frames with good detections used to calculate astrometric fits 
int 
4 

0 
NUMBER 
The Variability table contains statistics from the set of observations of each source. At present, the mean ra and dec and the error in two tangential directions are calculated. The "ra" direction is defined as tangential to both the radial direction and the cartesian zaxis and the "dec" direction is defined as both the radial direction and the "ra" direction. Since the current model is just the mean and standard deviation of the data, then the chisquared of the fit=1. Data from good frames across all bands go into the astrometric model determination. This will include bands in nonsynoptic filters: the one observation in these bands can help. In future releases a fit will be made to the rms data as a function of magnitude in each band, as has already happened for photometric data and a motion model that incorporates proper motion (and possibly parallax) will be used. The motion model is a parameter in the VarFrameSetInfo table. 
nFrames 
dxsVariability, gcsVariability, gpsVariability, lasVariability, udsVariability 
WSA 
Number of frames with good detections used to calculate astrometric fits 
int 
4 

0 
NUMBER 
The Variability table contains statistics from the set of observations of each source. At present, the mean ra and dec and the error in two tangential directions are calculated. The "ra" direction is defined as tangential to both the radial direction and the cartesian zaxis and the "dec" direction is defined as both the radial direction and the "ra" direction. Since the current model is just the mean and standard deviation of the data, then the chisquared of the fit=1. Data from good frames across all bands go into the astrometric model determination. This will include bands in nonsynoptic filters: the one observation in these bands can help. In future releases a fit will be made to the rms data as a function of magnitude in each band, as has already happened for photometric data and a motion model that incorporates proper motion (and possibly parallax) will be used. The motion model is a parameter in the VarFrameSetInfo table. 
nFrames 
gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource 
WSA 
No. of frames used for this proper motion measurement 
tinyint 
1 

0 
NUMBER 
nFrames 
uhsVariability 
WSAUHS 
Number of frames with good detections used to calculate astrometric fits 
int 
4 

0 
NUMBER 
The Variability table contains statistics from the set of observations of each source. At present, the mean ra and dec and the error in two tangential directions are calculated. The "ra" direction is defined as tangential to both the radial direction and the cartesian zaxis and the "dec" direction is defined as both the radial direction and the "ra" direction. Since the current model is just the mean and standard deviation of the data, then the chisquared of the fit=1. Data from good frames across all bands go into the astrometric model determination. This will include bands in nonsynoptic filters: the one observation in these bands can help. In future releases a fit will be made to the rms data as a function of magnitude in each band, as has already happened for photometric data and a motion model that incorporates proper motion (and possibly parallax) will be used. The motion model is a parameter in the VarFrameSetInfo table. 
ng 
ObjectThin 
PS1DR2 
Number of single epoch detections in g filter. 
smallint 
2 

999 

ngrp 
allwise_sc 
WISE 
Excess number of positionally associated duplicate resolution groups in which this extractions was included. Values of ngrp>0 indicate that the source was associated with more than one possible group. CAUTION: In the AllSky Release Catalog and 3Band Cryo Source Working Database, this column indicated the total number of groups with which a source was associated. In the AllWISE Catalog and Reject Table, ngrp is the total number of groups minus one. 
smallint 
2 



ngrp 
wise_allskysc 
WISE 
Number of positionally associated duplicate resolution groups in which this extractions was included. 
smallint 
2 

9999 

nhcon 
iras_psc 
IRAS 
Number of times observed (<25) 
tinyint 
1 


NUMBER 
ni 
ObjectThin 
PS1DR2 
Number of single epoch detections in i filter. 
smallint 
2 

999 

nId 
iras_psc 
IRAS 
Number of positional associations (<25). 
tinyint 
1 


NUMBER 
night_key 
twomass_xsc 
2MASS 
key to night data record in "scan DB". 
smallint 
2 


ID_NUMBER 
nightZPCat 
MultiframeDetector 
WSA 
Average photometric zero point for night {catalogue extension keyword: NIGHTZPT} 
real 
4 
mags 
0.9999995e9 
?? 
nightZPCat 
MultiframeDetector 
WSACalib 
Average photometric zero point for night {catalogue extension keyword: NIGHTZPT} 
real 
4 
mags 
0.9999995e9 
?? 
nightZPCat 
MultiframeDetector 
WSATransit 
Average photometric zero point for night {catalogue extension keyword: NIGHTZPT} 
real 
4 
mags 
0.9999995e9 
?? 
nightZPCat 
MultiframeDetector 
WSAUHS 
Average photometric zero point for night {catalogue extension keyword: NIGHTZPT} 
real 
4 
mags 
0.9999995e9 
?? 
nightZPCat 
PreviousMFDZP 
WSA 
Average photometric zero point for night 
real 
4 
mags 
0.9999995e9 
?? 
nightZPCat 
PreviousMFDZP 
WSACalib 
Average photometric zero point for night 
real 
4 
mags 
0.9999995e9 
?? 
nightZPCat 
PreviousMFDZP 
WSAUHS 
Average photometric zero point for night 
real 
4 
mags 
0.9999995e9 
?? 
nightZPErrCat 
MultiframeDetector 
WSA 
Photometric zero point sigma for night {catalogue extension keyword: NIGHTZRR} <0.05 mags for a good night 
real 
4 
mags 
0.9999995e9 
?? 
nightZPErrCat 
MultiframeDetector 
WSACalib 
Photometric zero point sigma for night {catalogue extension keyword: NIGHTZRR} <0.05 mags for a good night 
real 
4 
mags 
0.9999995e9 
?? 
nightZPErrCat 
MultiframeDetector 
WSATransit 
Photometric zero point sigma for night {catalogue extension keyword: NIGHTZRR} <0.05 mags for a good night 
real 
4 
mags 
0.9999995e9 
?? 
nightZPErrCat 
MultiframeDetector 
WSAUHS 
Photometric zero point sigma for night {catalogue extension keyword: NIGHTZRR} <0.05 mags for a good night 
real 
4 
mags 
0.9999995e9 
?? 
nightZPErrCat 
PreviousMFDZP 
WSA 
Photometric zero point sigma for night <0.05 mags for a good night 
real 
4 
mags 
0.9999995e9 
?? 
nightZPErrCat 
PreviousMFDZP 
WSACalib 
Photometric zero point sigma for night <0.05 mags for a good night 
real 
4 
mags 
0.9999995e9 
?? 
nightZPErrCat 
PreviousMFDZP 
WSAUHS 
Photometric zero point sigma for night <0.05 mags for a good night 
real 
4 
mags 
0.9999995e9 
?? 
nightZPNum 
MultiframeDetector 
WSA 
Number of ZP in band used to calculate nightZPCat {catalogue extension keyword: NIGHTNUM} 
int 
4 
mags 
99999999 
?? 
nightZPNum 
MultiframeDetector 
WSACalib 
Number of ZP in band used to calculate nightZPCat {catalogue extension keyword: NIGHTNUM} 
int 
4 
mags 
99999999 
?? 
nightZPNum 
MultiframeDetector 
WSATransit 
Number of ZP in band used to calculate nightZPCat {catalogue extension keyword: NIGHTNUM} 
int 
4 
mags 
99999999 
?? 
nightZPNum 
MultiframeDetector 
WSAUHS 
Number of ZP in band used to calculate nightZPCat {catalogue extension keyword: NIGHTNUM} 
int 
4 
mags 
99999999 
?? 
nightZPNum 
PreviousMFDZP 
WSA 
Number of ZP in band used to calculate nightZPCat 
int 
4 
mags 
99999999 
?? 
nightZPNum 
PreviousMFDZP 
WSACalib 
Number of ZP in band used to calculate nightZPCat 
int 
4 
mags 
99999999 
?? 
nightZPNum 
PreviousMFDZP 
WSAUHS 
Number of ZP in band used to calculate nightZPCat 
int 
4 
mags 
99999999 
?? 
nInFrameset 
lasMapRemeasAver 
WSA 
Number of frames in the frameSet linked in MapProvenance 
int 
4 



nIters 
catwise_2020, catwise_prelim 
WISE 
number of chisquareminimization iterations 
int 
4 



nIters_pm 
catwise_2020, catwise_prelim 
WISE 
number of chisquareminimization iterations 
int 
4 



njitter 
Multiframe 
WSA 
Number of positions in telescope pattern {image primary HDU keyword: NJITTER} 
smallint 
2 

9999 
meta.number 
njitter 
Multiframe 
WSACalib 
Number of positions in telescope pattern {image primary HDU keyword: NJITTER} 
smallint 
2 

9999 
meta.number 
njitter 
Multiframe 
WSATransit 
Number of positions in telescope pattern {image primary HDU keyword: NJITTER} 
smallint 
2 

9999 
meta.number 
njitter 
Multiframe 
WSAUHS 
Number of positions in telescope pattern {image primary HDU keyword: NJITTER} 
smallint 
2 

9999 
meta.number 
nLrs 
iras_psc 
IRAS 
Number of significant LRS spectra 
tinyint 
1 


NUMBER 
nMeasurements 
lasMapRemeasAver 
WSA 
Number used in average. 
int 
4 



nonperp 
dxsAstrometricInfo, gcsAstrometricInfo, gpsAstrometricInfo, lasAstrometricInfo, udsAstrometricInfo 
WSA 
Nonperpendicularity of axes 
float 
8 
radians 
0.9999995e9 
?? 
nonperp 
uhsAstrometricInfo 
WSAUHS 
Nonperpendicularity of axes 
float 
8 
radians 
0.9999995e9 
?? 
nopt_mchs 
twomass_psc 
2MASS 
The number of USNOA2.0 or Tycho 2 optical sources found within a 5" radius of the TWOMASS position. 
smallint 
2 


NUMBER 
nPass 
RequiredFilters 
WSA 
the number of passes that will be made 
smallint 
2 


meta.number 
nPass 
RequiredFilters 
WSACalib 
the number of passes that will be made 
smallint 
2 


meta.number 
nPass 
RequiredFilters 
WSATransit 
the number of passes that will be made 
smallint 
2 


meta.number 
nPass 
RequiredFilters 
WSAUHS 
the number of passes that will be made 
smallint 
2 


meta.number 
nr 
ObjectThin 
PS1DR2 
Number of single epoch detections in r filter. 
smallint 
2 

999 

nStackDetections 
ObjectThin 
PS1DR2 
Number of stack detections. 
smallint 
2 

999 

nStackObjectRows 
ObjectThin 
PS1DR2 
Number of independent StackObjectThin rows associated with this object. 
smallint 
2 

999 

nSteps 
catwise_2020, catwise_prelim 
WISE 
number of steps in all iterations 
int 
4 



nSteps_pm 
catwise_2020, catwise_prelim 
WISE 
number of steps in all iterations 
int 
4 



ntr 
hipparcos_new_reduction 
GAIADR1 
Number of field transits used 
int 
4 


meta.id;obs.field 
nu_eff_used_in_astrometry 
gaia_source 
GAIAEDR3 
Effective wavenumber of the source used in the astrometric solution 
real 
4 
micron^1 

em.wavenumber 
num 
tycho2 
GAIADR1 
NUmber of positions used 
smallint 
2 


meta.number 
num_harmonics_for_p1 
cepheid, rrlyrae 
GAIADR1 
Number of harmonics used to model P1 of the light curve 
int 
4 


meta.number 
num_observations_processed 
phot_variable_time_series_g_fov_statistical_parameters 
GAIADR1 
Number of processed Gband observations for variability analysis 
int 
4 


meta.number 
numAxes 
MultiframeDetector 
WSA 
Number of data axes; eg. 2 
tinyint 
1 


meta.number 
numAxes 
MultiframeDetector 
WSACalib 
Number of data axes; eg. 2 
tinyint 
1 


meta.number 
numAxes 
MultiframeDetector 
WSATransit 
Number of data axes; eg. 2 
tinyint 
1 


meta.number 
numAxes 
MultiframeDetector 
WSAUHS 
Number of data axes; eg. 2 
tinyint 
1 


meta.number 
numberStk 
RequiredStack 
WSA 
Number of intermediate stacks. If default, stack all good quality stacks 
int 
4 

99999999 

numberStk 
RequiredStack 
WSACalib 
Number of intermediate stacks. If default, stack all good quality stacks 
int 
4 

99999999 

numberStk 
RequiredStack 
WSATransit 
Number of intermediate stacks. If default, stack all good quality stacks 
int 
4 

99999999 

numberStk 
RequiredStack 
WSAUHS 
Number of intermediate stacks. If default, stack all good quality stacks 
int 
4 

99999999 

numDetectors 
Multiframe 
WSA 
The number of "detectors" (=image extensions in FITS file) 
tinyint 
1 


?? 
numDetectors 
Multiframe 
WSACalib 
The number of "detectors" (=image extensions in FITS file) 
tinyint 
1 


?? 
numDetectors 
Multiframe 
WSATransit 
The number of "detectors" (=image extensions in FITS file) 
tinyint 
1 


?? 
numDetectors 
Multiframe 
WSAUHS 
The number of "detectors" (=image extensions in FITS file) 
tinyint 
1 


?? 
numExp 
Multiframe 
WSA 
Number of exposures in integration {image primary HDU keyword: NEXP} 
smallint 
2 

9999 
meta.number 
numExp 
Multiframe 
WSACalib 
Number of exposures in integration {image primary HDU keyword: NEXP} 
smallint 
2 

9999 
meta.number 
numExp 
Multiframe 
WSATransit 
Number of exposures in integration {image primary HDU keyword: NEXP} 
smallint 
2 

9999 
meta.number 
numExp 
Multiframe 
WSAUHS 
Number of exposures in integration {image primary HDU keyword: NEXP} 
smallint 
2 

9999 
meta.number 
numInts 
Multiframe 
WSA 
Number of integrations in observation {image primary HDU keyword: NINT} 
smallint 
2 


meta.number 
numInts 
Multiframe 
WSACalib 
Number of integrations in observation {image primary HDU keyword: NINT} 
smallint 
2 


meta.number 
numInts 
Multiframe 
WSATransit 
Number of integrations in observation {image primary HDU keyword: NINT} 
smallint 
2 


meta.number 
numInts 
Multiframe 
WSAUHS 
Number of integrations in observation {image primary HDU keyword: NINT} 
smallint 
2 


meta.number 
numReads 
Multiframe 
WSA 
Number of reads per exposure {image primary HDU keyword: NREADS} 
smallint 
2 

9999 
meta.number 
numReads 
Multiframe 
WSACalib 
Number of reads per exposure {image primary HDU keyword: NREADS} 
smallint 
2 

9999 
meta.number 
numReads 
Multiframe 
WSATransit 
Number of reads per exposure {image primary HDU keyword: NREADS} 
smallint 
2 

9999 
meta.number 
numReads 
Multiframe 
WSAUHS 
Number of reads per exposure {image primary HDU keyword: NREADS} 
smallint 
2 

9999 
meta.number 
numRms 
CurrentAstrometry 
WSACalib 
No. of astrometric standards used in fit {image extension keyword: NUMBRMS} 
int 
4 

99999999 
stat.fit.param 
numRms 
CurrentAstrometry 
WSATransit 
No. of astrometric standards used in fit {image extension keyword: NUMBRMS} 
int 
4 

99999999 
stat.fit.param 
numRms 
CurrentAstrometry 
WSAUHS 
No. of astrometric standards used in fit {image extension keyword: NUMBRMS} 
int 
4 

99999999 
stat.fit.param 
numRms 
CurrentAstrometry, PreviousAstrometry 
WSA 
No. of astrometric standards used in fit {image extension keyword: NUMBRMS} 
int 
4 

99999999 
stat.fit.param 
numZPCat 
MultiframeDetector 
WSA 
Number of standards used in determining photZPCat and photZPCatErr {catalogue extension keyword: NUMZPT} 
int 
4 

99999999 

numZPCat 
MultiframeDetector 
WSACalib 
Number of standards used in determining photZPCat and photZPCatErr {catalogue extension keyword: NUMZPT} 
int 
4 

99999999 

numZPCat 
MultiframeDetector 
WSATransit 
Number of standards used in determining photZPCat and photZPCatErr {catalogue extension keyword: NUMZPT} 
int 
4 

99999999 

numZPCat 
MultiframeDetector 
WSAUHS 
Number of standards used in determining photZPCat and photZPCatErr {catalogue extension keyword: NUMZPT} 
int 
4 

99999999 

numZPCat 
PreviousMFDZP 
WSA 
Number of standards used in determining photZP and photZPErr 
int 
4 

99999999 

numZPCat 
PreviousMFDZP 
WSACalib 
Number of standards used in determining photZP and photZPErr 
int 
4 

99999999 

numZPCat 
PreviousMFDZP 
WSAUHS 
Number of standards used in determining photZP and photZPErr 
int 
4 

99999999 

nuStep 
Multiframe 
WSA 
Number of positions in microstep pattern {image primary HDU keyword: NUSTEP} 
smallint 
2 

9999 
meta.number 
nuStep 
Multiframe 
WSACalib 
Number of positions in microstep pattern {image primary HDU keyword: NUSTEP} 
smallint 
2 

9999 
meta.number 
nuStep 
Multiframe 
WSATransit 
Number of positions in microstep pattern {image primary HDU keyword: NUSTEP} 
smallint 
2 

9999 
meta.number 
nuStep 
Multiframe 
WSAUHS 
Number of positions in microstep pattern {image primary HDU keyword: NUSTEP} 
smallint 
2 

9999 
meta.number 
nustep 
RequiredMosaic 
WSACalib 
Amount of microstepping 
tinyint 
1 


?? 
nustep 
RequiredMosaic 
WSATransit 
Amount of microstepping 
tinyint 
1 


?? 
nustep 
RequiredMosaic 
WSAUHS 
Amount of microstepping 
tinyint 
1 


?? 
nustep 
RequiredMosaic, RequiredStack 
WSA 
Amount of microstepping 
tinyint 
1 


?? 
NVSS 
nvssSource 
NVSS 
Source name 
varchar 
14 


ID_MAIN 
ny 
ObjectThin 
PS1DR2 
Number of single epoch detections in y filter. 
smallint 
2 

999 

nz 
ObjectThin 
PS1DR2 
Number of single epoch detections in z filter. 
smallint 
2 

999 
