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Glossary of WSA attributes

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

P

NameSchema TableDatabaseDescriptionTypeLengthUnitDefault ValueUnified Content Descriptor
pa Detection SSA Celestial position angle (E of N) smallint 2 degrees   POS_POS-ANG
pa dxsDetection, dxsListRemeasurement, gcsDetection, gcsListRemeasurement, gpsDetection, gpsListRemeasurement, lasDetection, lasListRemeasurement, udsDetection, udsListRemeasurement WSA ellipse fit orientation to x axis {catalogue TType keyword: Position_angle}
Angle of ellipse major axis wrt x axis.		 real 4 degrees   POS_POS-ANG
pa firstSource FIRST position angle (east of north) derived from the elliptical Gaussian model for the source real 4 degrees   POS_POS-ANG
pairingCriterion Programme WSA The pairing criterion for associating detections into merged sources real 4 Degrees   ??
parentID Detection SSA objID of parent object, = objID for parent/undeblended (ie. not child) object bigint 8     ID_PARENT
pcSysID MultiframeDetector WSA PC system identifier {image extension keyword: PCSYSID} varchar 32   NONE ??
pCut Plate SSA Threshold "percentage cut" for pixel analysis real 4 percent   STAT_%REJECT
petroFlux dxsDetection, dxsListRemeasurement, gcsDetection, gcsListRemeasurement, gpsDetection, gpsListRemeasurement, lasDetection, lasListRemeasurement, udsDetection, udsListRemeasurement WSA flux within circular aperture to k × r_p ; k = 2 {catalogue TType keyword: Petr_flux} real 4 ADU   PHOT_INTENSITY_ADU
petroFluxErr dxsDetection, dxsListRemeasurement, gcsDetection, gcsListRemeasurement, gpsDetection, gpsListRemeasurement, lasDetection, lasListRemeasurement, udsDetection, udsListRemeasurement WSA error on Petrosian flux {catalogue TType keyword: Petr_flux_err} real 4 ADU   ERROR
petroMag dxsDetection, dxsListRemeasurement, gcsDetection, gcsListRemeasurement, gpsDetection, gpsListRemeasurement, lasDetection, lasListRemeasurement, udsDetection, udsListRemeasurement WSA Calibrated Petrosian magnitude within circular aperture r_p real 4 mag   PHOT_INT-MAG
petroMagErr dxsDetection, dxsListRemeasurement, gcsDetection, gcsListRemeasurement, gpsDetection, gpsListRemeasurement, lasDetection, lasListRemeasurement, udsDetection, udsListRemeasurement WSA error on calibrated Petrosian magnitude real 4 mag   ERROR
petroRad dxsDetection, dxsListRemeasurement, gcsDetection, gcsListRemeasurement, gpsDetection, gpsListRemeasurement, lasDetection, lasListRemeasurement, udsDetection, udsListRemeasurement WSA r_p as defined in Yasuda et al. 2001 AJ 112 1104 {catalogue TType keyword: Petr_radius} real 4 pixels   EXTENSION_RAD
pFlag rosat_bsc, rosat_fsc ROSAT possible problem with position determination varchar 1     CODE_MISC
pGalaxy dxsSource, gcsSource, gpsSource, lasSource, udsSource WSA Probability that the source is a galaxy real 4     STAT_PROP
Individual detection classifications are combined in the source merging process to produce a set of attributes for each merged source as follows. Presently, a basic classification table is defined that assigns reasonably accurate, self-consistent probability values for a given classification code:
FlagMeaning
Probability (%)
StarGalaxyNoiseSaturated
-9Saturated 0.0 0.0 5.095.0
-3Probable galaxy25.070.0 5.0 0.0
-2Probable star70.025.0 5.0 0.0
-1Star90.0 5.0 5.0 0.0
0Noise 5.0 5.090.0 0.0
+1Galaxy 5.090.0 5.0 0.0

Then, each separately available classification is combined for a merged source using Bayesian classification rules, assuming each datum is independent:

P(classk)=ΠiP(classk)i / ΣkΠiP(classk)i
where classk is one of star|galaxy|noise|saturated, and i denotes the ith single detection passband measurement available (the non-zero entries are necessary for the independent measures method to work, since some cases might otherwise be mutually exclusive). For example, if an object is classed in J|H|K as -1|-2|+1 it would have merged classification probabilities of pStar=73.5%, pGalaxy=26.2%, pNoise=0.3% and pSaturated=0.0%. Decision thresholds for the resulting discrete classification flag mergedClass are 90% for definitive and 70% for probable; hence the above example would be classified (not unreasonably) as probably a star (mergedClass=-2). An additional decision rule enforces mergedClass=-9 (saturated) when any individual classification flag indicates saturation.

ph_qual twomass_psc 2MASS Photometric quality flag. varchar 3     CODE_QUALITY
phaRange rosat_bsc, rosat_fsc ROSAT PHA range with highest detection likelihood varchar 1     CODE_MISC
pHeight dxsDetection, dxsListRemeasurement, gcsDetection, gcsListRemeasurement, gpsDetection, gpsListRemeasurement, lasDetection, lasListRemeasurement, udsDetection, udsListRemeasurement WSA Highest pixel value above sky {catalogue TType keyword: Peak_height}
In counts relative to local value of sky - also zeroth order aperture flux.		 real 4 ADU   PHOT_COUNTS_MISC
pHeightErr dxsDetection, dxsListRemeasurement, gcsDetection, gcsListRemeasurement, gpsDetection, gpsListRemeasurement, lasDetection, lasListRemeasurement, udsDetection, udsListRemeasurement WSA Error in peak height {catalogue TType keyword: Peak_height_err} real 4 ADU   ERROR
phi_opt twomass_psc 2MASS Position angle on the sky of the vector from the the associated optical source to the TWOMASS source position, in degrees East of North. smallint 2 degrees   POS_POS-ANG
photZP Multiframe WSA Photometric zeropoint for default extinction {image primary HDU keyword: MAGZPT} real 4 mag -0.9999995e9  
photZPCat MultiframeDetector WSA Photometric zero point for default extinction for the catalogue data {catalogue extension keyword:  MAGZPT} real 4 mags -0.9999995e9 ??
Derived detector zero-point in the sense of what magnitude object gives a total (corrected) flux of 1 count/s. These ZPs are appropriate for generating magnitudes in the natural detector+filter system based on Vega, see CASU reports for more details on colour equations etc. The ZPs have been derived from a robust average of all photometric standards observed on any particular set of frames, corrected for airmass but assuming the default extinction values listed later. For other airmass or other values of the extinction use
ZP → ZP - [sec(z)-1]×extinct + extinct default - extinct
You can then make use of any of the assorted flux estimators to produce magnitudes via
Mag = ZP - 2.5*log10(flux/exptime) - aperCor - skyCorr
Note that for the so-called total and isophotal flux options it is not possible to have a single-valued aperture correction.
photZPErr Multiframe WSA Photometric zeropoint error {image primary HDU keyword: MAGZRR} real 4 mag -0.9999995e9  
photZPErrCat MultiframeDetector WSA Photometric zero point error for the catalogue data {catalogue extension keyword:  MAGZRR}
[Currently set to -1 for WFCAM data.]		 real 4 mags -0.9999995e9 ??
Error in the zero point. If good photometric night this error will be at the level of a few percent. Values of 0.05 and above indicate correspondingly non-photometric night and worse.
photZPErrExt MultiframeDetector WSA Photometric zero point error of the detector {image extension keyword: MAGZRR}
[Currently set to -1 for WFCAM data.]		 real 4 mags -0.9999995e9 ??
Error in the zero point. If good photometric night this error will be at the level of a few percent. Values of 0.05 and above indicate correspondingly non-photometric night and worse.
photZPExt MultiframeDetector WSA Photometric zero point for default extinction of the detector {image extension keyword: MAGZPT} real 4 mags -0.9999995e9 ??
Derived detector zero-point in the sense of what magnitude object gives a total (corrected) flux of 1 count/s. These ZPs are appropriate for generating magnitudes in the natural detector+filter system based on Vega, see CASU reports for more details on colour equations etc. The ZPs have been derived from a robust average of all photometric standards observed on any particular set of frames, corrected for airmass but assuming the default extinction values listed later. For other airmass or other values of the extinction use
ZP → ZP - [sec(z)-1]×extinct + extinct default - extinct
You can then make use of any of the assorted flux estimators to produce magnitudes via
Mag = ZP - 2.5*log10(flux/exptime) - aperCor - skyCorr
Note that for the so-called total and isophotal flux options it is not possible to have a single-valued aperture correction.
pixelScale MultiframeDetector WSA Warning - Original detector pixel size, the actual angular pixel size is written to xPixSize and yPixSize in the CurrentAstrometry table {image extension keyword: PIXLSIZE} real 4 arcsec per pixel -0.9999995e9 INST_PIXSIZE
plateID Detection SSA Plate ID of the plate that this detection came from int 4     ID_PLATE
plateID Plate SSA Unique identifier of the plate: surveyID plus field number combo int 4     ID_PLATE
plateNum Plate SSA Plate number assigned by observatory smallint 2     ID_PLATE
plateScale Survey SSA Nominal plate scale real 4 arcsec/mm   INST_SCALE
plxCol Plate SSA Name of parallax column in reference catalogue varchar 16     REMARKS
pNearH iras_psc IRAS Number of nearby hours-confirmed point sources tinyint 1     NUMBER
pNearW iras_psc IRAS Number of nearby weeks-confirmed point sources tinyint 1     NUMBER
pNoise dxsSource, gcsSource, gpsSource, lasSource, udsSource WSA Probability that the source is noise real 4     STAT_PROP
Individual detection classifications are combined in the source merging process to produce a set of attributes for each merged source as follows. Presently, a basic classification table is defined that assigns reasonably accurate, self-consistent probability values for a given classification code:
FlagMeaning
Probability (%)
StarGalaxyNoiseSaturated
-9Saturated 0.0 0.0 5.095.0
-3Probable galaxy25.070.0 5.0 0.0
-2Probable star70.025.0 5.0 0.0
-1Star90.0 5.0 5.0 0.0
0Noise 5.0 5.090.0 0.0
+1Galaxy 5.090.0 5.0 0.0

Then, each separately available classification is combined for a merged source using Bayesian classification rules, assuming each datum is independent:

P(classk)=ΠiP(classk)i / ΣkΠiP(classk)i
where classk is one of star|galaxy|noise|saturated, and i denotes the ith single detection passband measurement available (the non-zero entries are necessary for the independent measures method to work, since some cases might otherwise be mutually exclusive). For example, if an object is classed in J|H|K as -1|-2|+1 it would have merged classification probabilities of pStar=73.5%, pGalaxy=26.2%, pNoise=0.3% and pSaturated=0.0%. Decision thresholds for the resulting discrete classification flag mergedClass are 90% for definitive and 70% for probable; hence the above example would be classified (not unreasonably) as probably a star (mergedClass=-2). An additional decision rule enforces mergedClass=-9 (saturated) when any individual classification flag indicates saturation.

pointingID Multiframe WSA Pointing ID within survey {image primary HDU keyword: SURVEY_I} varchar 64   NONE ??
pos iras_asc IRAS Position Angle from IRAS Source to Association (E of N) smallint 2 degrees   POS_POS-ANG
posAng iras_psc IRAS Uncertainty ellipse position angle (East of North) smallint 2 degrees   POS_POS-ANG
posAngle CurrentAstrometry, PreviousAstrometry WSA orientation of image x-axis to N-S float 8 Degrees -0.9999995e9 POS_POS-ANG
postProb JunkDetection SSA Posterior probability of detection being junk real 4     STAT_PROBABILITY
ppErrBits dxsDetection, dxsListRemeasurement, gcsDetection, gcsListRemeasurement, gpsDetection, gpsListRemeasurement, lasDetection, lasListRemeasurement, udsDetection, udsListRemeasurement WSA additional WFAU post-processing error bits (place holder for now) int 4   0 CODE_MISC
prfMag Detection SSA Profile magnitude real 4 instrumental units   PHOT_PHG_MAG
prfStat Detection SSA Profile statistic real 4 N(0,1)   CLASS_STAR/GALAXY
prfStatB Source SSA Profile statistic from B band detection real 4 N(0,1) -0.99999995e9 CLASS_STAR/GALAXY
prfStatI Source SSA Profile statistic from I band detection real 4 N(0,1) -0.99999995e9 CLASS_STAR/GALAXY
prfStatR1 Source SSA Profile statistic from R1 band detection real 4 N(0,1) -0.99999995e9 CLASS_STAR/GALAXY
prfStatR2 Source SSA Profile statistic from R2 band detection real 4 N(0,1) -0.99999995e9 CLASS_STAR/GALAXY
priFlgLb rosat_bsc, rosat_fsc ROSAT priority flag L-broad tinyint 1     CODE_MISC
priFlgLh rosat_bsc, rosat_fsc ROSAT priority flag L-hard tinyint 1     CODE_MISC
priFlgLs rosat_bsc, rosat_fsc ROSAT priority flag L-soft tinyint 1     CODE_MISC
priFlgMb rosat_bsc, rosat_fsc ROSAT priority flag M-broad tinyint 1     CODE_MISC
priFlgMh rosat_bsc, rosat_fsc ROSAT priority flag M-hard tinyint 1     CODE_MISC
priFlgMs rosat_bsc, rosat_fsc ROSAT priority flag M-soft tinyint 1     CODE_MISC
priOrSec dxsSource, gcsSource, gpsSource, lasSource, udsSource WSA Seam code for a unique (=0) or duplicated (!=0) source (eg. flags overlap duplicates). bigint 8   -99999999 CODE_MISC
Because of the spacing of the detectors in WFCAM, and the restrictions on guide star brightness, there will always be overlap regions between adjacent frame sets. Source merging is done on a set-by-set basis; hence after source merging there are usually a small number of duplicate sources in the table. A process known as seaming takes place after source merging is complete, whereby duplicates are identified and flagged. The flagging attribute is priOrSec, and the meaning of the flag is quite simple: if a source is not found to be duplicated in overlap regions, then priOrSec=0; if a source is duplicated, then priOrSec will be set to the frameSetID of the source that should be considered the best one to use out of the set of duplicates. Presently, the choice of which is best is made on the basis of proximity to the optical axis of the camera, the assumption being that this will give the best quality image in general. So, if a particular source has a non-zero priOrSec that is set to it's own value of frameSetID, then this indicates that there is a duplicate elsewhere in the table, but this is the one that should be selected as the best (i.e. this is the primary source). On the other hand, if a source has a non-zero value of priOrSec that is set a different frameSetID than that of the source in question, then this indicates that this source should be considered as a secondary duplicate of a source who's primary is actually to be found in the frame set pointed to by that value of frameSetID. Hence, the WHERE clause for selecting out a seamless, best catalogue is of the form WHERE ... AND (priOrSec=0 OR priOrSec=frameSetID).
priOrSec dxsSourceRemeasurement, gcsSourceRemeasurement, gpsSourceRemeasurement, lasSourceRemeasurement, udsSourceRemeasurement WSA Seam code for a unique (=0) or duplicated (!=0) source (eg. flags overlap duplicates) bigint 8     CODE_MISC
Because of the spacing of the detectors in WFCAM, and the restrictions on guide star brightness, there will always be overlap regions between adjacent frame sets. Source merging is done on a set-by-set basis; hence after source merging there are usually a small number of duplicate sources in the table. A process known as seaming takes place after source merging is complete, whereby duplicates are identified and flagged. The flagging attribute is priOrSec, and the meaning of the flag is quite simple: if a source is not found to be duplicated in overlap regions, then priOrSec=0; if a source is duplicated, then priOrSec will be set to the frameSetID of the source that should be considered the best one to use out of the set of duplicates. Presently, the choice of which is best is made on the basis of proximity to the optical axis of the camera, the assumption being that this will give the best quality image in general. So, if a particular source has a non-zero priOrSec that is set to it's own value of frameSetID, then this indicates that there is a duplicate elsewhere in the table, but this is the one that should be selected as the best (i.e. this is the primary source). On the other hand, if a source has a non-zero value of priOrSec that is set a different frameSetID than that of the source in question, then this indicates that this source should be considered as a secondary duplicate of a source who's primary is actually to be found in the frame set pointed to by that value of frameSetID. Hence, the WHERE clause for selecting out a seamless, best catalogue is of the form WHERE ... AND (priOrSec=0 OR priOrSec=frameSetID).
productID RequiredDiffImage WSA A unique identifier assigned to each required difference image product entry int 4     ??
productID RequiredMosaic WSA A unique identifier assigned to each required mosaic product entry int 4     ??
productID RequiredStack WSA A unique identifier assigned to each required stack product entry int 4     ??
programmeID Programme WSA UID of the archived programme coded as above int 4     ID_SURVEY
programmeID ProgrammeCurationHistory, ProgrammeTable, RequiredCurationTask, RequiredDiffImage, RequiredFilters, RequiredListDrivenProduct, RequiredMosaic, RequiredNeighbours, RequiredStack WSA the unique programme ID int 4     ID_SURVEY
programmeID ProgrammeFrame, SurveyProgrammes WSA WSA assigned programme UID {image primary HDU keyword: PROJECT} int 4   -99999999 ID_SURVEY
project Multiframe WSA Time-allocation code {image primary HDU keyword: PROJECT} varchar 64   NONE REFER_CODE
projection RequiredMosaic WSA CASU mosaic tool option to specify output WCS projection type (TAN for gnomonic, ZPN for zenithal polynomial) varchar 3     ??
propPeriod Programme WSA the proprietory period for any data taken for this programme in months, e.g. 12 for open time. int 4 months   TIME_PERIOD
proprietary Survey WSA Logical flag indicating whether a survey is proprietary or not (1=yes; 0=no) tinyint 1     ??
prox twomass_psc, twomass_xsc 2MASS Proximity. real 4 arcsec   POS_ANG_DIST_GENERAL
pSaturated dxsSource, gcsSource, gpsSource, lasSource, udsSource WSA Probability that the source is saturated real 4     STAT_PROP
Individual detection classifications are combined in the source merging process to produce a set of attributes for each merged source as follows. Presently, a basic classification table is defined that assigns reasonably accurate, self-consistent probability values for a given classification code:
FlagMeaning
Probability (%)
StarGalaxyNoiseSaturated
-9Saturated 0.0 0.0 5.095.0
-3Probable galaxy25.070.0 5.0 0.0
-2Probable star70.025.0 5.0 0.0
-1Star90.0 5.0 5.0 0.0
0Noise 5.0 5.090.0 0.0
+1Galaxy 5.090.0 5.0 0.0

Then, each separately available classification is combined for a merged source using Bayesian classification rules, assuming each datum is independent:

P(classk)=ΠiP(classk)i / ΣkΠiP(classk)i
where classk is one of star|galaxy|noise|saturated, and i denotes the ith single detection passband measurement available (the non-zero entries are necessary for the independent measures method to work, since some cases might otherwise be mutually exclusive). For example, if an object is classed in J|H|K as -1|-2|+1 it would have merged classification probabilities of pStar=73.5%, pGalaxy=26.2%, pNoise=0.3% and pSaturated=0.0%. Decision thresholds for the resulting discrete classification flag mergedClass are 90% for definitive and 70% for probable; hence the above example would be classified (not unreasonably) as probably a star (mergedClass=-2). An additional decision rule enforces mergedClass=-9 (saturated) when any individual classification flag indicates saturation.

psfFitChi2 dxsDetection, dxsListRemeasurement, gcsDetection, gcsListRemeasurement, gpsDetection, gpsListRemeasurement, lasDetection, lasListRemeasurement, udsDetection, udsListRemeasurement WSA standard normalised variance of PSF fit {catalogue TType keyword: PSF_fit_chi2} real 4   -0.9999995e9 FIT_STDEV
psfFitDof dxsDetection, dxsListRemeasurement, gcsDetection, gcsListRemeasurement, gpsDetection, gpsListRemeasurement, lasDetection, lasListRemeasurement, udsDetection, udsListRemeasurement WSA no. of degrees of freedom of PSF fit {catalogue TType keyword: PSF_fit_dof} smallint 2   -9999 STAT_N-DOF
psfFitX dxsDetection, dxsListRemeasurement, gcsDetection, gcsListRemeasurement, gpsDetection, gpsListRemeasurement, lasDetection, lasListRemeasurement, udsDetection, udsListRemeasurement WSA PSF-fitted X coordinate {catalogue TType keyword: PSF_fit_X} real 4 pixels -0.9999995e9 POS_PLATE_X
psfFitXerr dxsDetection, dxsListRemeasurement, gcsDetection, gcsListRemeasurement, gpsDetection, gpsListRemeasurement, lasDetection, lasListRemeasurement, udsDetection, udsListRemeasurement WSA Error on PSF-fitted X coordinate {catalogue TType keyword: PSF_fit_X_err} real 4 pixels -0.9999995e9 ERROR
psfFitY dxsDetection, dxsListRemeasurement, gcsDetection, gcsListRemeasurement, gpsDetection, gpsListRemeasurement, lasDetection, lasListRemeasurement, udsDetection, udsListRemeasurement WSA PSF-fitted Y coordinate {catalogue TType keyword: PSF_fit_Y} real 4 pixels -0.9999995e9 POS_PLATE_Y
psfFitYerr dxsDetection, dxsListRemeasurement, gcsDetection, gcsListRemeasurement, gpsDetection, gpsListRemeasurement, lasDetection, lasListRemeasurement, udsDetection, udsListRemeasurement WSA Error on PSF-fitted Y coordinate {catalogue TType keyword: PSF_fit_y_err} real 4 pixels -0.9999995e9 ERROR
psfFlux dxsDetection, dxsListRemeasurement, gcsDetection, gcsListRemeasurement, gpsDetection, gpsListRemeasurement, lasDetection, lasListRemeasurement, udsDetection, udsListRemeasurement WSA PSF-fitted flux {catalogue TType keyword: PSF_flux} real 4 ADU -0.9999995e9 PHOT_INTENSITY_ADU
psfFluxErr dxsDetection, dxsListRemeasurement, gcsDetection, gcsListRemeasurement, gpsDetection, gpsListRemeasurement, lasDetection, lasListRemeasurement, udsDetection, udsListRemeasurement WSA Error on PSF-fitted flux {catalogue TType keyword: PSF_flux_err} real 4 ADU -0.9999995e9 ERROR
psfMag dxsDetection, dxsListRemeasurement, gcsDetection, gcsListRemeasurement, gpsDetection, gpsListRemeasurement, lasDetection, lasListRemeasurement, udsDetection, udsListRemeasurement WSA PSF-fitted calibrated magnitude real 4 mag -0.9999995e9 PHOT_PROFILE
psfMagErr dxsDetection, dxsListRemeasurement, gcsDetection, gcsListRemeasurement, gpsDetection, gpsListRemeasurement, lasDetection, lasListRemeasurement, udsDetection, udsListRemeasurement WSA Error on PSF-fitted calibrated magnitude real 4 mag -0.9999995e9 ERROR
pStar dxsSource, gcsSource, gpsSource, lasSource, udsSource WSA Probability that the source is a star real 4     STAT_PROP
Individual detection classifications are combined in the source merging process to produce a set of attributes for each merged source as follows. Presently, a basic classification table is defined that assigns reasonably accurate, self-consistent probability values for a given classification code:
FlagMeaning
Probability (%)
StarGalaxyNoiseSaturated
-9Saturated 0.0 0.0 5.095.0
-3Probable galaxy25.070.0 5.0 0.0
-2Probable star70.025.0 5.0 0.0
-1Star90.0 5.0 5.0 0.0
0Noise 5.0 5.090.0 0.0
+1Galaxy 5.090.0 5.0 0.0

Then, each separately available classification is combined for a merged source using Bayesian classification rules, assuming each datum is independent:

P(classk)=ΠiP(classk)i / ΣkΠiP(classk)i
where classk is one of star|galaxy|noise|saturated, and i denotes the ith single detection passband measurement available (the non-zero entries are necessary for the independent measures method to work, since some cases might otherwise be mutually exclusive). For example, if an object is classed in J|H|K as -1|-2|+1 it would have merged classification probabilities of pStar=73.5%, pGalaxy=26.2%, pNoise=0.3% and pSaturated=0.0%. Decision thresholds for the resulting discrete classification flag mergedClass are 90% for definitive and 70% for probable; hence the above example would be classified (not unreasonably) as probably a star (mergedClass=-2). An additional decision rule enforces mergedClass=-9 (saturated) when any individual classification flag indicates saturation.

pts_key twomass_psc 2MASS A unique identification number for the PSC source. int 4     ID_NUMBER
pts_key twomass_xsc 2MASS key to point source data DB record. int 4     ID_NUMBER
pv21 CurrentAstrometry, PreviousAstrometry WSA Coefficient for r term (use only with ZPN projection) {image extension keyword: PV2_1}
transformation from pixel to celestial co-ordinates		 float 8   -0.9999995e9 POS_TRANSF_PARAM
pv22 CurrentAstrometry, PreviousAstrometry WSA Coefficient for r**2 term (use only with ZPN projection) {image extension keyword: PV2_2}
transformation from pixel to celestial co-ordinates		 float 8   -0.9999995e9 POS_TRANSF_PARAM
pv23 CurrentAstrometry, PreviousAstrometry WSA Coefficient for r**3 term (use only with ZPN projection) {image extension keyword: PV2_3}
transformation from pixel to celestial co-ordinates		 float 8   -0.9999995e9 POS_TRANSF_PARAM
pxcntr twomass_psc 2MASS The pts_key value of the nearest source in the PSC. int 4     NUMBER
pxcntr twomass_xsc 2MASS ext_key value of nearest XSC source. int 4     NUMBER
pxpa twomass_psc, twomass_xsc 2MASS The position angle on the sky of the vector from the source to the nearest neighbor in the PSC, in degrees East of North. smallint 2 degrees   POS_POS-ANG


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