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Glossary of WSA NonSurvey attributes (UKIDSSDR5) |
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This Glossary alphabetically lists all attributes used in the WSA NonSurvey database(s) held in the WSA. If you would like to have more information about the schema tables please use the Schema Browser (other Browser versions). |
| A | B | C | D | E | F | G | H | I | J | K | L | M |
| N | O | P | Q | R | S | T | U | V | W | X | Y | Z |
H | ||||||||
|---|---|---|---|---|---|---|---|---|
| Name | Schema Table | Database | Description | Type | Length | Unit | Default Value | Unified Content Descriptor |
| h2AperMag3 | [nspid]Source | WSA NonSurvey | Default point/extended source H2 aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real | 4 | mag | -0.9999995e9 | PHOT_MAG |
| h2AperMag3Err | [nspid]Source | WSA NonSurvey | Error in default point/extended source H2 mag (2.0 arcsec aperture diameter) | real | 4 | mag | -0.9999995e9 | ERROR |
| h2AperMag4 | [nspid]Source | WSA NonSurvey | Extended source H2 aperture corrected mag (2.8 arcsec aperture diameter) | real | 4 | mag | -0.9999995e9 | PHOT_MAG |
| h2AperMag4Err | [nspid]Source | WSA NonSurvey | Error in extended source H2 mag (2.8 arcsec aperture diameter) | real | 4 | mag | -0.9999995e9 | ERROR |
| h2AperMag6 | [nspid]Source | WSA NonSurvey | Extended source H2 aperture corrected mag (5.7 arcsec aperture diameter) | real | 4 | mag | -0.9999995e9 | PHOT_MAG |
| h2AperMag6Err | [nspid]Source | WSA NonSurvey | Error in extended source H2 mag (5.7 arcsec aperture diameter) | real | 4 | mag | -0.9999995e9 | ERROR |
| h2aStrat | [nspid]VarFrameSetInfo | WSA NonSurvey | Strateva parameter a in H2 band, see Sesar et al. 2007. | real | 4 | -0.9999995e9 | ||
| The best fit solution to the expected RMS for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. | ||||||||
| h2bestAper | [nspid]Variability | WSA NonSurvey | Best aperture (1-6) for photometric statistics in the H2 band | int | 4 | -9999 | ||
| Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) | ||||||||
| h2bStrat | [nspid]VarFrameSetInfo | WSA NonSurvey | Strateva parameter b in H2 band, see Sesar et al. 2007. | real | 4 | -0.9999995e9 | ||
| The best fit solution to the expected RMS for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. | ||||||||
| h2chiSq | [nspid]VarFrameSetInfo | WSA NonSurvey | Fit of Strateva function to data in H2 band | real | 4 | -0.9999995e9 | ||
| The best fit solution to the expected RMS for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. | ||||||||
| h2chiSqpd | [nspid]Variability | WSA NonSurvey | Chi square (per degree of freedom) fit to data (mean and expected rms) | real | 4 | 0.9999995e9 | ||
| The photometry is calculated for good observations in the best aperture. The mean, rms, median and median absolute deviation are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. | ||||||||
| h2Class | [nspid]Source | WSA NonSurvey | discrete image classification flag in H2 | smallint | 2 | -9999 | CLASS_MISC | |
| h2ClassStat | [nspid]Source | WSA NonSurvey | N(0,1) stellarness-of-profile statistic in H2 | real | 4 | -0.9999995e9 | STAT_PROP | |
| h2cStrat | [nspid]VarFrameSetInfo | WSA NonSurvey | Strateva parameter a in H2 band, see Sesar et al. 2007. | real | 4 | -0.9999995e9 | ||
| The best fit solution to the expected RMS for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. | ||||||||
| h2Deblend | [nspid]Source | WSA NonSurvey | placeholder flag indicating parent/child relation in H2 | int | 4 | -99999999 | CODE_MISC | |
| This CASU pipeline processing source extraction flag is a placeholder only, and is always set to zero in all passbands in the merged source lists. If you need to know when a particular image detection is a component of a deblend or not, test bit 4 of attribute ppErrBits (see corresponding glossary entry) which is set by WFAU's post-processing software based on testing the areal profiles aprof2-8 (these are set by CASU to -1 for deblended components, or positive values for non-deblended detections). We encode this in an information bit of ppErrBits for convenience when querying the merged source tables. | ||||||||
| h2Ell | [nspid]Source | WSA NonSurvey | 1-b/a, where a/b=semi-major/minor axes in H2 | real | 4 | -0.9999995e9 | PHYS_ELLIPTICITY | |
| h2eNum | [nspid]MergeLog | WSA NonSurvey | the extension number of this H2 detector | tinyint | 1 | NUMBER | ||
| h2ErrBits | [nspid]Source | WSA NonSurvey | processing warning/error bitwise flags in H2 | int | 4 | -99999999 | CODE_MISC | |
| h2Eta | [nspid]Source | WSA NonSurvey | Offset of H2 detection from master position (+north/-south) | real | 4 | arcsec | -0.9999995e9 | POS_EQ_DEC_OFF |
| When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 2.0 (UKIDSS LAS and GPS; also non-survey programmes) or 1.0 (UKIDSS GPS, DXS and UDS) arcseconds is used, the higher value enabling pairing of moving sources when epoch separations may be several years. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the LAS, you might wish to insist that the offsets in the selected sample are all below 1 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. | ||||||||
| h2expML | [nspid]VarFrameSetInfo | WSA NonSurvey | Expected magnitude limit of frameSet in this in H2 band. | real | 4 | -0.9999995e9 | ||
| The expected magnitude limit of an intermediate stack, based on the total exposure time. expML=Filter.oneSecML+1.25*log10(totalExpTime). Since different intermediate stacks can have different exposure times, the totalExpTime is the minimum, as long as the number of stacks with this minimum make up 10% of the total. This is a more conservative treatment than just taking the mean or median total exposure time. | ||||||||
| h2ExpRms | [nspid]Variability | WSA NonSurvey | Rms calculated from polynomial fit to minimum RMS as a function of magnitude in H2 band | real | 4 | mag | -0.9999995e9 | |
| The photometry is calculated for good observations in the best aperture. The mean, rms, median and median absolute deviation are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. | ||||||||
| h2Gausig | [nspid]Source | WSA NonSurvey | RMS of axes of ellipse fit in H2 | real | 4 | pixels | -0.9999995e9 | MORPH_PARAM |
| h2HallMag | [nspid]Source | WSA NonSurvey | Total point source H2 mag | real | 4 | mag | -0.9999995e9 | PHOT_MAG |
| h2HallMagErr | [nspid]Source | WSA NonSurvey | Error in total point source H2 mag | real | 4 | mag | -0.9999995e9 | ERROR |
| h2IntRms | [nspid]Variability | WSA NonSurvey | Intrinsic rms in H2-band | real | 4 | mag | -0.9999995e9 | |
| The photometry is calculated for good observations in the best aperture. The mean, rms, median and median absolute deviation are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. | ||||||||
| h2MagMAD | [nspid]Variability | WSA NonSurvey | Median Absolute Deviation of H2 magnitude | real | 4 | mag | -0.9999995e9 | |
| The photometry is calculated for good observations in the best aperture. The mean, rms, median and median absolute deviation are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. | ||||||||
| h2MagRms | [nspid]Variability | WSA NonSurvey | rms of H2 magnitude | real | 4 | mag | -0.9999995e9 | |
| The photometry is calculated for good observations in the best aperture. The mean, rms, median and median absolute deviation are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. | ||||||||
| h2maxCadence | [nspid]Variability | WSA NonSurvey | maximum gap between observations | real | 4 | days | -0.9999995e9 | |
| The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. | ||||||||
| h2mbrExt | [nspid]Source | WSA NonSurvey | Extended source colour H2-Br (using aperMag3) | real | 4 | mag | -0.9999995e9 | PHOT_COLOR |
| Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits. | ||||||||
| h2mbrExtErr | [nspid]Source | WSA NonSurvey | Error on extended source colour H2-Br | real | 4 | mag | -0.9999995e9 | ERROR |
| Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits. | ||||||||
| h2mbrPnt | [nspid]Source | WSA NonSurvey | Point source colour H2-Br (using aperMag3) | real | 4 | mag | -0.9999995e9 | PHOT_COLOR |
| Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits. | ||||||||
| h2mbrPntErr | [nspid]Source | WSA NonSurvey | Error on point source colour H2-Br | real | 4 | mag | -0.9999995e9 | ERROR |
| Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits. | ||||||||
| h2meanMag | [nspid]Variability | WSA NonSurvey | Mean H2 magnitude | real | 4 | mag | -0.9999995e9 | |
| The photometry is calculated for good observations in the best aperture. The mean, rms, median and median absolute deviation are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. | ||||||||
| h2medCadence | [nspid]Variability | WSA NonSurvey | median gap between observations | real | 4 | days | -0.9999995e9 | |
| The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. | ||||||||
| h2medianMag | [nspid]Variability | WSA NonSurvey | Median H2 magnitude | real | 4 | mag | -0.9999995e9 | |
| The photometry is calculated for good observations in the best aperture. The mean, rms, median and median absolute deviation are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. | ||||||||
| h2mfID | [nspid]MergeLog | WSA NonSurvey | the UID of the relevant H2 multiframe | bigint | 8 | ID_FRAME | ||
| h2minCadence | [nspid]Variability | WSA NonSurvey | minimum gap between observations | real | 4 | days | -0.9999995e9 | |
| The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. | ||||||||
| h2nDof | [nspid]VarFrameSetInfo | WSA NonSurvey | Number of degrees of freedom of fit in H2 band. | smallint | 2 | -9999 | ||
| The best fit solution to the expected RMS for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. | ||||||||
| h2ndof | [nspid]Variability | WSA NonSurvey | Number of degrees of freedom for chisquare | int | 4 | -9999 | ||
| The photometry is calculated for good observations in the best aperture. The mean, rms, median and median absolute deviation are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. | ||||||||
| h2nFlaggedObs | [nspid]Variability | WSA NonSurvey | Number of detections in H2 band flagged as potentially spurious by u05b19Detection.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. | ||||||||
| h2nFlaggedObs | [nspid]Variability | WSA NonSurvey | Number of detections in H2 band flagged as potentially spurious by u05bh53Detection.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. | ||||||||
| h2nFlaggedObs | [nspid]Variability | WSA NonSurvey | Number of detections in H2 band flagged as potentially spurious by u06ad5Detection.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. | ||||||||
| h2nFlaggedObs | [nspid]Variability | WSA NonSurvey | Number of detections in H2 band flagged as potentially spurious by u06ah13Detection.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. | ||||||||
| h2nFlaggedObs | [nspid]Variability | WSA NonSurvey | Number of detections in H2 band flagged as potentially spurious by userv1707Detection.ppErrBits | int | 4 | 0 | ||
| The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. | ||||||||
| h2nFlaggedObs | [nspid]Variability | WSA NonSurvey | Number of detections in H2 band flagged as potentially spurious by userv1721Detection.ppErrBits | int | 4 | 0 | ||
| The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. | ||||||||
| h2nGoodObs | [nspid]Variability | WSA NonSurvey | Number of good detections in H2 band | int | 4 | 0 | ||
| The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. | ||||||||
| h2nMissingObs | [nspid]Variability | WSA NonSurvey | Number of H2 band frames that this object should have been detected on and was not | int | 4 | 0 | ||
| The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. | ||||||||
| h2ObjID | [nspid]Source | WSA NonSurvey | 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 | [nspid]Source | WSA NonSurvey | ellipse fit celestial orientation in H2 | real | 4 | Degrees | -0.9999995e9 | POS_POS-ANG |
| h2PetroMag | [nspid]Source | WSA NonSurvey | Extended source H2 mag (Petrosian) | real | 4 | mag | -0.9999995e9 | PHOT_MAG |
| h2PetroMagErr | [nspid]Source | WSA NonSurvey | Error in extended source H2 mag (Petrosian) | real | 4 | mag | -0.9999995e9 | ERROR |
| h2ppErrBits | [nspid]Source | WSA NonSurvey | additional WFAU post-processing error bits in H2 | int | 4 | 0 | CODE_MISC | |
| h2probVar | [nspid]Variability | WSA NonSurvey | Probability of variable from chi-square (and other data) | real | 4 | 0.9999995e9 | ||
| The photometry is calculated for good observations in the best aperture. The mean, rms, median and median absolute deviation are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. | ||||||||
| h2PsfMag | [nspid]Source | WSA NonSurvey | Point source profile-fitted H2 mag | real | 4 | mag | -0.9999995e9 | PHOT_MAG |
| h2PsfMagErr | [nspid]Source | WSA NonSurvey | Error in point source profile-fitted H2 mag | real | 4 | mag | -0.9999995e9 | ERROR |
| h2SeqNum | [nspid]Source | WSA NonSurvey | the running number of the H2 detection | int | 4 | -99999999 | ID_NUMBER | |
| h2SerMag2D | [nspid]Source | WSA NonSurvey | Extended source H2 mag (profile-fitted) | real | 4 | mag | -0.9999995e9 | PHOT_MAG |
| h2SerMag2DErr | [nspid]Source | WSA NonSurvey | Error in extended source H2 mag (profile-fitted) | real | 4 | mag | -0.9999995e9 | ERROR |
| h2skewness | [nspid]Variability | WSA NonSurvey | Skewness in H2 band (see Sesar et al. 2007) | real | 4 | -0.9999995e9 | ||
| The photometry is calculated for good observations in the best aperture. The mean, rms, median and median absolute deviation are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. | ||||||||
| h2totalPeriod | [nspid]Variability | WSA NonSurvey | total period of observations (last obs-first obs) | real | 4 | days | -0.9999995e9 | |
| The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. | ||||||||
| h2VarClass | [nspid]Variability | WSA NonSurvey | Classification of variability in this band | smallint | 2 | -9999 | ||
| The photometry is calculated for good observations in the best aperture. The mean, rms, median and median absolute deviation are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. | ||||||||
| h2Xi | [nspid]Source | WSA NonSurvey | Offset of H2 detection from master position (+east/-west) | real | 4 | arcsec | -0.9999995e9 | POS_EQ_RA_OFF |
| When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 2.0 (UKIDSS LAS and GPS; also non-survey programmes) or 1.0 (UKIDSS GPS, DXS and UDS) arcseconds is used, the higher value enabling pairing of moving sources when epoch separations may be several years. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the LAS, you might wish to insist that the offsets in the selected sample are all below 1 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. | ||||||||
| hallFlux | [nspid]Detection | WSA NonSurvey | flux within circular aperture to k × r_h; k = 5; alternative total flux {catalogue TType keyword: Hall_flux} | real | 4 | ADU | PHOT_INTENSITY_ADU | |
| hallFluxErr | [nspid]Detection | WSA NonSurvey | error on Hall flux {catalogue TType keyword: Hall_flux_err} | real | 4 | ADU | ERROR | |
| hallMag | [nspid]Detection | WSA NonSurvey | Calibrated magnitude within circular aperture r_hall | real | 4 | mag | PHOT_INT-MAG | |
| hallMagErr | [nspid]Detection | WSA NonSurvey | Calibrated error on Hall magnitude | real | 4 | mag | ERROR | |
| hallRad | [nspid]Detection | WSA NonSurvey | r_h image scale radius eg. Hall & Mackay 1984 MNRAS 210 979 {catalogue TType keyword: Hall_radius} | real | 4 | pixels | EXTENSION_RAD | |
| hAperMag3 | [nspid]Source | WSA NonSurvey | Default point/extended source H aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real | 4 | mag | -0.9999995e9 | PHOT_MAG |
| hAperMag3Err | [nspid]Source | WSA NonSurvey | Error in default point/extended source H mag (2.0 arcsec aperture diameter) | real | 4 | mag | -0.9999995e9 | ERROR |
| hAperMag4 | [nspid]Source | WSA NonSurvey | Extended source H aperture corrected mag (2.8 arcsec aperture diameter) | real | 4 | mag | -0.9999995e9 | PHOT_MAG |
| hAperMag4Err | [nspid]Source | WSA NonSurvey | Error in extended source H mag (2.8 arcsec aperture diameter) | real | 4 | mag | -0.9999995e9 | ERROR |
| hAperMag6 | [nspid]Source | WSA NonSurvey | Extended source H aperture corrected mag (5.7 arcsec aperture diameter) | real | 4 | mag | -0.9999995e9 | PHOT_MAG |
| hAperMag6Err | [nspid]Source | WSA NonSurvey | Error in extended source H mag (5.7 arcsec aperture diameter) | real | 4 | mag | -0.9999995e9 | ERROR |
| haStrat | [nspid]VarFrameSetInfo | WSA NonSurvey | Strateva parameter a in H band, see Sesar et al. 2007. | real | 4 | -0.9999995e9 | ||
| The best fit solution to the expected RMS for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. | ||||||||
| hbestAper | [nspid]Variability | WSA NonSurvey | Best aperture (1-6) for photometric statistics in the H band | int | 4 | -9999 | ||
| Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) | ||||||||
| hbStrat | [nspid]VarFrameSetInfo | WSA NonSurvey | Strateva parameter b in H band, see Sesar et al. 2007. | real | 4 | -0.9999995e9 | ||
| The best fit solution to the expected RMS for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. | ||||||||
| hchiSq | [nspid]VarFrameSetInfo | WSA NonSurvey | Fit of Strateva function to data in H band | real | 4 | -0.9999995e9 | ||
| The best fit solution to the expected RMS for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. | ||||||||
| hchiSqpd | [nspid]Variability | WSA NonSurvey | Chi square (per degree of freedom) fit to data (mean and expected rms) | real | 4 | 0.9999995e9 | ||
| The photometry is calculated for good observations in the best aperture. The mean, rms, median and median absolute deviation are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. | ||||||||
| hClass | [nspid]Source | WSA NonSurvey | discrete image classification flag in H | smallint | 2 | -9999 | CLASS_MISC | |
| hClassStat | [nspid]Source | WSA NonSurvey | N(0,1) stellarness-of-profile statistic in H | real | 4 | -0.9999995e9 | STAT_PROP | |
| hcStrat | [nspid]VarFrameSetInfo | WSA NonSurvey | Strateva parameter a in H band, see Sesar et al. 2007. | real | 4 | -0.9999995e9 | ||
| The best fit solution to the expected RMS for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. | ||||||||
| hDeblend | [nspid]Source | WSA NonSurvey | placeholder flag indicating parent/child relation in H | int | 4 | -99999999 | CODE_MISC | |
| This CASU pipeline processing source extraction flag is a placeholder only, and is always set to zero in all passbands in the merged source lists. If you need to know when a particular image detection is a component of a deblend or not, test bit 4 of attribute ppErrBits (see corresponding glossary entry) which is set by WFAU's post-processing software based on testing the areal profiles aprof2-8 (these are set by CASU to -1 for deblended components, or positive values for non-deblended detections). We encode this in an information bit of ppErrBits for convenience when querying the merged source tables. | ||||||||
| hdtFile | [nspid]Multiframe | WSA NonSurvey | Name of global hdt file {image primary HDU keyword: HDTFILE} | varchar | 32 | NONE | ||
| hdtFileExt | [nspid]MultiframeDetector | WSA NonSurvey | Name of camera-specific hdt file {image extension keyword: HDTFILE2} | varchar | 32 | NONE | ?? | |
| hEll | [nspid]Source | WSA NonSurvey | 1-b/a, where a/b=semi-major/minor axes in H | real | 4 | -0.9999995e9 | PHYS_ELLIPTICITY | |
| heNum | [nspid]MergeLog | WSA NonSurvey | the extension number of this H detector | tinyint | 1 | NUMBER | ||
| hErrBits | [nspid]Source | WSA NonSurvey | processing warning/error bitwise flags in H | int | 4 | -99999999 | CODE_MISC | |
| hEta | [nspid]Source | WSA NonSurvey | Offset of H detection from master position (+north/-south) | real | 4 | arcsec | -0.9999995e9 | POS_EQ_DEC_OFF |
| When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 2.0 (UKIDSS LAS and GPS; also non-survey programmes) or 1.0 (UKIDSS GPS, DXS and UDS) arcseconds is used, the higher value enabling pairing of moving sources when epoch separations may be several years. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the LAS, you might wish to insist that the offsets in the selected sample are all below 1 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. | ||||||||
| hexpML | [nspid]VarFrameSetInfo | WSA NonSurvey | 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 | [nspid]Variability | WSA NonSurvey | Rms calculated from polynomial fit to minimum 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 and median absolute deviation are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. | ||||||||
| hGausig | [nspid]Source | WSA NonSurvey | RMS of axes of ellipse fit in H | real | 4 | pixels | -0.9999995e9 | MORPH_PARAM |
| hHallMag | [nspid]Source | WSA NonSurvey | Total point source H mag | real | 4 | mag | -0.9999995e9 | PHOT_MAG |
| hHallMagErr | [nspid]Source | WSA NonSurvey | Error in total point source H mag | real | 4 | mag | -0.9999995e9 | ERROR |
| hIntRms | [nspid]Variability | WSA NonSurvey | Intrinsic rms in H-band | real | 4 | mag | -0.9999995e9 | |
| The photometry is calculated for good observations in the best aperture. The mean, rms, median and median absolute deviation are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. | ||||||||
| hMag | [nspid]FSstars | WSA NonSurvey | H band total magnitude on the MKO(UFTI) system | real | 4 | mag | PHOT_INT-MAG | |
| hMagErr | [nspid]FSstars | WSA NonSurvey | H band magnitude error | real | 4 | mag | ERROR | |
| hMagMAD | [nspid]Variability | WSA NonSurvey | 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 and median absolute deviation are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. | ||||||||
| hMagRms | [nspid]Variability | WSA NonSurvey | rms of H magnitude | real | 4 | mag | -0.9999995e9 | |
| The photometry is calculated for good observations in the best aperture. The mean, rms, median and median absolute deviation are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. | ||||||||
| hmaxCadence | [nspid]Variability | WSA NonSurvey | maximum gap between observations | real | 4 | days | -0.9999995e9 | |
| The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. | ||||||||
| hmeanMag | [nspid]Variability | WSA NonSurvey | Mean H magnitude | real | 4 | mag | -0.9999995e9 | |
| The photometry is calculated for good observations in the best aperture. The mean, rms, median and median absolute deviation are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. | ||||||||
| hmedCadence | [nspid]Variability | WSA NonSurvey | median gap between observations | real | 4 | days | -0.9999995e9 | |
| The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. | ||||||||
| hmedianMag | [nspid]Variability | WSA NonSurvey | Median H magnitude | real | 4 | mag | -0.9999995e9 | |
| The photometry is calculated for good observations in the best aperture. The mean, rms, median and median absolute deviation are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. | ||||||||
| hmfID | [nspid]MergeLog | WSA NonSurvey | the UID of the relevant H multiframe | bigint | 8 | ID_FRAME | ||
| hminCadence | [nspid]Variability | WSA NonSurvey | minimum gap between observations | real | 4 | days | -0.9999995e9 | |
| The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. | ||||||||
| hmkExt | [nspid]Source | WSA NonSurvey | Extended source colour H-K (using aperMag3) | real | 4 | mag | -0.9999995e9 | PHOT_COLOR |
| Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits. | ||||||||
| hmkExtErr | [nspid]Source | WSA NonSurvey | Error on extended source colour H-K | real | 4 | mag | -0.9999995e9 | ERROR |
| Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits. | ||||||||
| hmkPnt | [nspid]Source | WSA NonSurvey | Point source colour H-K (using aperMag3) | real | 4 | mag | -0.9999995e9 | PHOT_COLOR |
| Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits. | ||||||||
| hmkPntErr | [nspid]Source | WSA NonSurvey | Error on point source colour H-K | real | 4 | mag | -0.9999995e9 | ERROR |
| Default colours from pairs of adjacent passbands within a given set (e.g. Y-J, J-H and H-K for YJHK) are recorded in the merged source table for ease of querying and speedy querying via indexing of these attributes. Presently, the point-source colours and extended source colours are computed from the aperture corrected AperMag3 fixed 2 arcsec aperture diameter measures (for consistent measurement across all passbands) and generally good signal-to-noise. At some point in the future, this may be changed such that point-source colours will be computed from the PSF-fitted measures and extended source colours computed from the 2-d Sersic model profile fits. | ||||||||
| hnDof | [nspid]VarFrameSetInfo | WSA NonSurvey | Number of degrees of freedom of fit in H band. | smallint | 2 | -9999 | ||
| The best fit solution to the expected RMS for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. | ||||||||
| hndof | [nspid]Variability | WSA NonSurvey | Number of degrees of freedom for chisquare | int | 4 | -9999 | ||
| The photometry is calculated for good observations in the best aperture. The mean, rms, median and median absolute deviation are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. | ||||||||
| hnFlaggedObs | [nspid]Variability | WSA NonSurvey | Number of detections in H band flagged as potentially spurious by u05b13Detection.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 | [nspid]Variability | WSA NonSurvey | Number of detections in H band flagged as potentially spurious by u05b17Detection.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 | [nspid]Variability | WSA NonSurvey | Number of detections in H band flagged as potentially spurious by u05bh24Detection.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 | [nspid]Variability | WSA NonSurvey | Number of detections in H band flagged as potentially spurious by u06a3Detection.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 | [nspid]Variability | WSA NonSurvey | Number of detections in H band flagged as potentially spurious by u06ah13Detection.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 | [nspid]Variability | WSA NonSurvey | Number of detections in H band flagged as potentially spurious by u06b30Detection.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 | [nspid]Variability | WSA NonSurvey | Number of detections in H band flagged as potentially spurious by u06b40Detection.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 | [nspid]Variability | WSA NonSurvey | Number of detections in H band flagged as potentially spurious by u06bj5Detection.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 | [nspid]Variability | WSA NonSurvey | Number of detections in H band flagged as potentially spurious by u07a24Detection.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 | [nspid]Variability | WSA NonSurvey | Number of detections in H band flagged as potentially spurious by u07ah16Detection.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 | [nspid]Variability | WSA NonSurvey | Number of detections in H band flagged as potentially spurious by u07ah30Detection.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 | [nspid]Variability | WSA NonSurvey | Number of detections in H band flagged as potentially spurious by u07ah51Detection.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 | [nspid]Variability | WSA NonSurvey | Number of detections in H band flagged as potentially spurious by u07b11Detection.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 | [nspid]Variability | WSA NonSurvey | Number of detections in H band flagged as potentially spurious by u07b13Detection.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 | [nspid]Variability | WSA NonSurvey | Number of detections in H band flagged as potentially spurious by u07b6Detection.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 | [nspid]Variability | WSA NonSurvey | Number of detections in H band flagged as potentially spurious by ucmp4Detection.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 | [nspid]Variability | WSA NonSurvey | Number of detections in H band flagged as potentially spurious by userv1675Detection.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 | [nspid]Variability | WSA NonSurvey | Number of detections in H band flagged as potentially spurious by userv1677Detection.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 | [nspid]Variability | WSA NonSurvey | Number of detections in H band flagged as potentially spurious by userv1736Detection.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 | [nspid]Variability | WSA NonSurvey | Number of detections in H band flagged as potentially spurious by userv1747Detection.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 | [nspid]Variability | WSA NonSurvey | Number of detections in H band flagged as potentially spurious by userv1759Detection.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 | [nspid]Variability | WSA NonSurvey | 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. | ||||||||
| hnMissingObs | [nspid]Variability | WSA NonSurvey | 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 | [nspid]Source | WSA NonSurvey | 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 | [nspid]Multiframe | WSA NonSurvey | Hour angle {image primary HDU keyword: HABASE} | real | 4 | degrees | -0.9999995e9 | |
| hPA | [nspid]Source | WSA NonSurvey | ellipse fit celestial orientation in H | real | 4 | Degrees | -0.9999995e9 | POS_POS-ANG |
| hPetroMag | [nspid]Source | WSA NonSurvey | Extended source H mag (Petrosian) | real | 4 | mag | -0.9999995e9 | PHOT_MAG |
| hPetroMagErr | [nspid]Source | WSA NonSurvey | Error in extended source H mag (Petrosian) | real | 4 | mag | -0.9999995e9 | ERROR |
| hppErrBits | [nspid]Source | WSA NonSurvey | additional WFAU post-processing error bits in H | int | 4 | 0 | CODE_MISC | |
| hprobVar | [nspid]Variability | WSA NonSurvey | Probability of variable from chi-square (and other data) | real | 4 | 0.9999995e9 | ||
| The photometry is calculated for good observations in the best aperture. The mean, rms, median and median absolute deviation are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. | ||||||||
| hPsfMag | [nspid]Source | WSA NonSurvey | Point source profile-fitted H mag | real | 4 | mag | -0.9999995e9 | PHOT_MAG |
| hPsfMagErr | [nspid]Source | WSA NonSurvey | Error in point source profile-fitted H mag | real | 4 | mag | -0.9999995e9 | ERROR |
| hSeqNum | [nspid]Source | WSA NonSurvey | the running number of the H detection | int | 4 | -99999999 | ID_NUMBER | |
| hSerMag2D | [nspid]Source | WSA NonSurvey | Extended source H mag (profile-fitted) | real | 4 | mag | -0.9999995e9 | PHOT_MAG |
| hSerMag2DErr | [nspid]Source | WSA NonSurvey | Error in extended source H mag (profile-fitted) | real | 4 | mag | -0.9999995e9 | ERROR |
| hskewness | [nspid]Variability | WSA NonSurvey | 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 and median absolute deviation are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. | ||||||||
| htmID | [nspid]CurrentAstrometry, [nspid]PreviousAstrometry | WSA NonSurvey | Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates of device centre | bigint | 8 | -99999999 | POS_GENERAL | |
| htmID | [nspid]Detection, [nspid]Source | WSA NonSurvey | Hierarchical Triangular Mesh (HTM) index, 20 deep, for equatorial co-ordinates | bigint | 8 | POS_GENERAL | ||
| htmID | [nspid]MergeLog | WSA NonSurvey | HTM index, 20 digits, for co-ordinates | bigint | 8 | POS_GENERAL | ||
| htotalPeriod | [nspid]Variability | WSA NonSurvey | total period of observations (last obs-first obs) | real | 4 | days | -0.9999995e9 | |
| The observations are classified as good, flagged or missing. Flagged observations are ones where the object has a ppErrBit flag. Missing observations are observations of the part of the sky that include the position of the object, but had no detection. All the statistics are calculated from good observations. The cadence parameters give the minimum, median and maximum time between observations, which is useful to know if the data could be used to find a particular type of variable. | ||||||||
| humidity | [nspid]Multiframe | WSA NonSurvey | Relative Humidity {image primary HDU keyword: HUMIDITY} | real | 4 | -0.9999995e9 | OBS_CONDITIONS | |
| hVarClass | [nspid]Variability | WSA NonSurvey | Classification of variability in this band | smallint | 2 | -9999 | ||
| The photometry is calculated for good observations in the best aperture. The mean, rms, median and median absolute deviation are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. | ||||||||
| hXi | [nspid]Source | WSA NonSurvey | Offset of H detection from master position (+east/-west) | real | 4 | arcsec | -0.9999995e9 | POS_EQ_RA_OFF |
| When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 2.0 (UKIDSS LAS and GPS; also non-survey programmes) or 1.0 (UKIDSS GPS, DXS and UDS) arcseconds is used, the higher value enabling pairing of moving sources when epoch separations may be several years. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the LAS, you might wish to insist that the offsets in the selected sample are all below 1 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. | ||||||||
| hz10cd | [nspid]Multiframe | WSA NonSurvey | Trefoil: HZ10CD {image primary HDU keyword: HZ10CD} | real | 4 | -0.9999995e9 | ||
| hz10ch | [nspid]Multiframe | WSA NonSurvey | Trefoil: HZ10CH {image primary HDU keyword: HZ10CH} | real | 4 | -0.9999995e9 | ||
| hz10sd | [nspid]Multiframe | WSA NonSurvey | Trefoil: HZ10SD {image primary HDU keyword: HZ10SD} | real | 4 | -0.9999995e9 | ||
| hz10sh | [nspid]Multiframe | WSA NonSurvey | Trefoil: HZ10SH {image primary HDU keyword: HZ10SH} | real | 4 | -0.9999995e9 | ||
| hz5cd | [nspid]Multiframe | WSA NonSurvey | Astigmatism: HZ5CD {image primary HDU keyword: HZ5CD} | real | 4 | -0.9999995e9 | ||
| hz5ch | [nspid]Multiframe | WSA NonSurvey | Astigmatism: HZ5CH {image primary HDU keyword: HZ5CH} | real | 4 | -0.9999995e9 | ||
| hz5sd | [nspid]Multiframe | WSA NonSurvey | Astigmatism: HZ5SD {image primary HDU keyword: HZ5SD} | real | 4 | -0.9999995e9 | ||
| hz5sh | [nspid]Multiframe | WSA NonSurvey | Astigmatism: HZ5SH {image primary HDU keyword: HZ5SH} | real | 4 | -0.9999995e9 | ||
| hz6cd | [nspid]Multiframe | WSA NonSurvey | Astigmatism: HZ6CD {image primary HDU keyword: HZ6CD} | real | 4 | -0.9999995e9 | ||
| hz6ch | [nspid]Multiframe | WSA NonSurvey | Astigmatism: HZ6CH {image primary HDU keyword: HZ6CH} | real | 4 | -0.9999995e9 | ||
| hz6sd | [nspid]Multiframe | WSA NonSurvey | Astigmatism: HZ6SD {image primary HDU keyword: HZ6SD} | real | 4 | -0.9999995e9 | ||
| hz6sh | [nspid]Multiframe | WSA NonSurvey | Astigmatism: HZ6SH {image primary HDU keyword: HZ6SH} | real | 4 | -0.9999995e9 | ||
| hz9cd | [nspid]Multiframe | WSA NonSurvey | Trefoil: HZ9CD {image primary HDU keyword: HZ9CD} | real | 4 | -0.9999995e9 | ||
| hz9ch | [nspid]Multiframe | WSA NonSurvey | Trefoil: HZ9CH {image primary HDU keyword: HZ9CH} | real | 4 | -0.9999995e9 | ||
| hz9sd | [nspid]Multiframe | WSA NonSurvey | Trefoil: HZ9SD {image primary HDU keyword: HZ9SD} | real | 4 | -0.9999995e9 | ||
| hz9sh | [nspid]Multiframe | WSA NonSurvey | Trefoil: HZ9SH {image primary HDU keyword: HZ9SH} | real | 4 | -0.9999995e9 | ||
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14/04/2010