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Glossary of WSA NonSurvey attributes (UKIDSSDR4)
This Glossary alphabetically lists all attributes used in the WSA NonSurvey database(s) held in the WSA. If you would like to have more information about the schema tables please use the Schema Browser (other Browser versions).

A

B

C

D

E

F

G

H

I

J

K

L

M

N

O

P

Q

R

S

T

U

V

W

X

Y

Z

M
Name	Schema Table	Database	Description	Type	Length	Unit	Default Value	Unified Content Descriptor
m2u	[nspid]Multiframe	WSA NonSurvey	Raw position of M2 U (N-S tilt) {image primary HDU keyword: M2_U}	real	4	mrad	-0.9999995e9
m2v	[nspid]Multiframe	WSA NonSurvey	Raw position of M2 V (E-W tilt) {image primary HDU keyword: M2_V}	real	4	mrad	-0.9999995e9
m2w	[nspid]Multiframe	WSA NonSurvey	Raw position of M2 W (axial rotation) {image primary HDU keyword: M2_W}	real	4	mrad	-0.9999995e9
m2x	[nspid]Multiframe	WSA NonSurvey	Raw position of M2 X (E-W) {image primary HDU keyword: M2_X}	real	4	millimetres	-0.9999995e9
m2y	[nspid]Multiframe	WSA NonSurvey	Raw position of M2 Y (N-S) {image primary HDU keyword: M2_Y}	real	4	millimetres	-0.9999995e9
m2z	[nspid]Multiframe	WSA NonSurvey	Raw position of M2 Z (focus) {image primary HDU keyword: M2_Z}	real	4	millimetres	-0.9999995e9
M3Temp	[nspid]Multiframe	WSA NonSurvey	M3 temperature {image primary HDU keyword: M3_TEMP}	real	4	degrees_Kelvin	-0.9999995e9
maskID	[nspid]Multiframe	WSA NonSurvey	UID of library object mask frame {image extension keyword: CIR_OPM}	bigint	8		-99999999	ID_FRAME
masterObjID	[nspid]SourceNeighbours	WSA NonSurvey	The unique ID in u05b15Source (=sourceID)	bigint	8			ID_MAIN
masterObjID	[nspid]SourceNeighbours	WSA NonSurvey	The unique ID in u05b7Source (=sourceID)	bigint	8			ID_MAIN
masterObjID	[nspid]SourceNeighbours	WSA NonSurvey	The unique ID in u05bd1Source (=sourceID)	bigint	8			ID_MAIN
masterObjID	[nspid]SourceNeighbours	WSA NonSurvey	The unique ID in u05bj4Source (=sourceID)	bigint	8			ID_MAIN
masterObjID	[nspid]SourceNeighbours	WSA NonSurvey	The unique ID in u06a24Source (=sourceID)	bigint	8			ID_MAIN
masterObjID	[nspid]SourceNeighbours	WSA NonSurvey	The unique ID in u06a48Source (=sourceID)	bigint	8			ID_MAIN
masterObjID	[nspid]SourceNeighbours	WSA NonSurvey	The unique ID in u06ah43Source (=sourceID)	bigint	8			ID_MAIN
masterObjID	[nspid]SourceNeighbours	WSA NonSurvey	The unique ID in u06b13Source (=sourceID)	bigint	8			ID_MAIN
masterObjID	[nspid]SourceNeighbours	WSA NonSurvey	The unique ID in u06b24Source (=sourceID)	bigint	8			ID_MAIN
masterObjID	[nspid]SourceNeighbours	WSA NonSurvey	The unique ID in u06b36Source (=sourceID)	bigint	8			ID_MAIN
masterObjID	[nspid]SourceNeighbours	WSA NonSurvey	The unique ID in u07b29Source (=sourceID)	bigint	8			ID_MAIN
masterObjID	[nspid]SourceNeighbours	WSA NonSurvey	The unique ID in u07b36Source (=sourceID)	bigint	8			ID_MAIN
masterObjID	[nspid]SourceNeighbours	WSA NonSurvey	The unique ID in u07bd3Source (=sourceID)	bigint	8			ID_MAIN
masterObjID	[nspid]SourceNeighbours	WSA NonSurvey	The unique ID in u07bd4Source (=sourceID)	bigint	8			ID_MAIN
masterObjID	[nspid]SourceNeighbours	WSA NonSurvey	The unique ID in u07bh49Source (=sourceID)	bigint	8			ID_MAIN
masterObjID	[nspid]SourceNeighbours	WSA NonSurvey	The unique ID in userv1625Source (=sourceID)	bigint	8			ID_MAIN
masterObjID	[nspid]SourceNeighbours	WSA NonSurvey	The unique ID in userv1636Source (=sourceID)	bigint	8			ID_MAIN
masterObjID	[nspid]SourceNeighbours	WSA NonSurvey	The unique ID in userv1650Source (=sourceID)	bigint	8			ID_MAIN
masterObjID	[nspid]SourceNeighbours	WSA NonSurvey	The unique ID in userv1652Source (=sourceID)	bigint	8			ID_MAIN
masterObjID	[nspid]SourceNeighbours	WSA NonSurvey	The unique ID in userv1672Source (=sourceID)	bigint	8			ID_MAIN
masterObjID	[nspid]SourceNeighbours	WSA NonSurvey	The unique ID in userv1673Source (=sourceID)	bigint	8			ID_MAIN
masterObjID	[nspid]SourceNeighbours	WSA NonSurvey	The unique ID in userv1674Source (=sourceID)	bigint	8			ID_MAIN
masterObjID	[nspid]SourceNeighbours	WSA NonSurvey	The unique ID in userv1678Source (=sourceID)	bigint	8			ID_MAIN
masterObjID	[nspid]SourceNeighbours	WSA NonSurvey	The unique ID in userv1706Source (=sourceID)	bigint	8			ID_MAIN
masterObjID	[nspid]SourceNeighbours	WSA NonSurvey	The unique ID in userv1708Source (=sourceID)	bigint	8			ID_MAIN
masterObjID	[nspid]SourceNeighbours	WSA NonSurvey	The unique ID in userv1711Source (=sourceID)	bigint	8			ID_MAIN
masterObjID	[nspid]SourceNeighbours	WSA NonSurvey	The unique ID in userv1731Source (=sourceID)	bigint	8			ID_MAIN
masterObjID	[nspid]SourceNeighbours	WSA NonSurvey	The unique ID in userv1741Source (=sourceID)	bigint	8			ID_MAIN
masterObjID	[nspid]SourceNeighbours	WSA NonSurvey	The unique ID in userv1743Source (=sourceID)	bigint	8			ID_MAIN
masterObjID	[nspid]SourceNeighbours	WSA NonSurvey	The unique ID in userv1761Source (=sourceID)	bigint	8			ID_MAIN
masterObjID	[nspid]SourceNeighbours, [nspid]SourceXDetection	WSA NonSurvey	The unique ID in userv1707Source (=sourceID)	bigint	8			ID_MAIN
masterObjID	[nspid]SourceNeighbours, [nspid]SourceXtwomass_psc	WSA NonSurvey	The unique ID in u05a37Source (=sourceID)	bigint	8			ID_MAIN
maxDec	[nspid]CurrentAstrometry, [nspid]PreviousAstrometry	WSA NonSurvey	The maximum Dec (J2000) on the device	float	8	Degrees	-0.9999995e9	POS_EQ_DEC_MAIN
maxPllx	[nspid]Variability	WSA NonSurvey	Upper limit of 90% confidence interval for parallax measurement	real	4	mas	-0.9999995e9
			The Variability table contains statistics from the set of observations of each source. At present, the mean ra and dec and the error in two tangential directions are calculated. The "ra" direction is defined as tangential to both the radial direction and the cartesian z-axis and the "dec" direction is defined as both the radial direction and the "ra" direction. Since the current model is just the mean and standard deviation of the data, then the chi-squared of the fit=1. Data from good frames across all bands go into the astrometric model determination. This will include bands in non-synoptic filters: the one observation in these bands can help. In future releases a fit will be made to the rms data as a function of magnitude in each band, as has already happened for photometric data and a motion model that incorporates proper motion (and possibly parallax) will be used. The motion model is a parameter in the VarFrameSetInfo table.
maxRa	[nspid]CurrentAstrometry, [nspid]PreviousAstrometry	WSA NonSurvey	The maximum RA (J2000) on the device	float	8	Degrees	-0.9999995e9	POS_EQ_RA_OTHER
maxSeeing	[nspid]RequiredMosaic, [nspid]RequiredStack	WSA NonSurvey	The maximum allowed seeing for intermediate stacks	real	4	arcsec
maxStelEll	[nspid]RequiredMosaic, [nspid]RequiredStack	WSA NonSurvey	The maximum allowed stellar ellipticity for intermediate stacks	real	4
mergedClass	[nspid]Source	WSA NonSurvey	Class flag from available measurements (1|0|-1|-2|-3|-9=galaxy|noise|stellar|probableStar|probableGalaxy|saturated)	smallint	2			CODE_MISC
			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: Flag Meaning Probability (%) Star Galaxy Noise Saturated -9 Saturated 0.0 0.0 5.0 95.0 -3 Probable galaxy 25.0 70.0 5.0 0.0 -2 Probable star 70.0 25.0 5.0 0.0 -1 Star 90.0 5.0 5.0 0.0 0 Noise 5.0 5.0 90.0 0.0 +1 Galaxy 5.0 90.0 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.
mergedClassStat	[nspid]Source	WSA NonSurvey	Merged N(0,1) stellarness-of-profile statistic	real	4		-0.9999995e9	STAT_PROP
			This profile classification statistic is a continuously distributed, Gaussian N(0,1) (i.e. zero mean, unit variance) statistic formed from the available individual classification statistics by averaging them and multiplying by N1/2 such that cuts on mergedClassStat result in completeness being independent of number of frames an object appears on, but with reliability improving with the number of frames.
mergeLogTable	[nspid]Programme	WSA NonSurvey	Table name of curation log for source merging	varchar	64			??
mergeSwVersion	[nspid]MergeLog	WSA NonSurvey	version number of the software used to merge the frames	real	4			ID_VERSION
method	[nspid]RequiredDiffImage	WSA NonSurvey	CASU difference image tool option string specifying the method to employ (recommended value=adaptive/back/zerosky)	varchar	64			??
minDec	[nspid]CurrentAstrometry, [nspid]PreviousAstrometry	WSA NonSurvey	The minimum Dec (J2000) on the device	float	8	Degrees	-0.9999995e9	POS_EQ_DEC_MAIN
minImageSize	[nspid]MultiframeDetector	WSA NonSurvey	Minimum size for images {catalogue extension keyword:  MINPIX}	int	4	pixels	-99999999	??
			Tunable parameter, in conjunction with the threshold above this determines how deep and how small "real" images can be. The default precludes many of the few pixel-hit cosmic rays from being considered since "real" images must have 4 contiguous simply-connected pixels in the union of the detection filter and data domains. For more details on image detection and parametersiation see the papers in CASU WFCAM/VISTA Publications.
minPllx	[nspid]Variability	WSA NonSurvey	Lower limit of 90% confidence interval for parallax measurement	real	4	mas	-0.9999995e9
			The Variability table contains statistics from the set of observations of each source. At present, the mean ra and dec and the error in two tangential directions are calculated. The "ra" direction is defined as tangential to both the radial direction and the cartesian z-axis and the "dec" direction is defined as both the radial direction and the "ra" direction. Since the current model is just the mean and standard deviation of the data, then the chi-squared of the fit=1. Data from good frames across all bands go into the astrometric model determination. This will include bands in non-synoptic filters: the one observation in these bands can help. In future releases a fit will be made to the rms data as a function of magnitude in each band, as has already happened for photometric data and a motion model that incorporates proper motion (and possibly parallax) will be used. The motion model is a parameter in the VarFrameSetInfo table.
minRa	[nspid]CurrentAstrometry, [nspid]PreviousAstrometry	WSA NonSurvey	The minimum RA (J2000) on the device	float	8	Degrees	-0.9999995e9	POS_EQ_RA_OTHER
mirrBottTempNW	[nspid]Multiframe	WSA NonSurvey	Mirror bottom temp. NW {image primary HDU keyword: MIRRBTNW}	real	4	degrees_Celsius	-0.9999995e9	PHYS_TEMP_MISC
mirrTempNE	[nspid]Multiframe	WSA NonSurvey	Mirror temperature NE {image primary HDU keyword: MIRR_NE}	real	4	degrees_Celsius	-0.9999995e9	PHYS_TEMP_MISC
mirrTempNW	[nspid]Multiframe	WSA NonSurvey	Mirror temperature NW {image primary HDU keyword: MIRR_NW}	real	4	degrees_Celsius	-0.9999995e9	PHYS_TEMP_MISC
mirrTempSE	[nspid]Multiframe	WSA NonSurvey	Mirror temperature SE {image primary HDU keyword: MIRR_SE}	real	4	degrees_Celsius	-0.9999995e9	PHYS_TEMP_MISC
mirrTempSW	[nspid]Multiframe	WSA NonSurvey	Mirror temperature SW {image primary HDU keyword: MIRR_SW}	real	4	degrees_Celsius	-0.9999995e9	PHYS_TEMP_MISC
mirrTopTempNW	[nspid]Multiframe	WSA NonSurvey	Mirror top temp. NW {image primary HDU keyword: MIRRTPNW}	real	4	degrees_Celsius	-0.9999995e9	PHYS_TEMP_MISC
mjdObs	[nspid]Multiframe	WSA NonSurvey	Modified Julian Date of the observation {image primary HDU keyword: MJD-OBS}	float	8		-0.9999995e9	TIME_DATE
modelDistSecs	[nspid]SourceXDetectionBestMatch	WSA NonSurvey	separation from expected position given astrometric model in userv1707Source variability.	real	4	arcsec	-0.9999995e9
morphClassFlag	[nspid]MultiframeDetector	WSA NonSurvey	Image morphological classifier flag, set if the classifier has been run. If so an object classification flag and a stellarness index is included in the binary table columns. {catalogue extension keyword:  CLASSIFD}	tinyint	1		0	CODE_MISC
mosaicTool	[nspid]RequiredMosaic	WSA NonSurvey	Name of mosaicing tool to be used	varchar	8		'CASU'	??
motionModel	[nspid]VarFrameSetInfo	WSA NonSurvey	Motion model used to produce BestMatch table. Values: static;proper motion;proper motion and parallax.	varchar	32		static
			Motion model for frameset in question. This can be static: all objects in the frameset are assumed to be stationary; proper motion: all objects in the frameset are fit for a linear proper motion; proper motion and parallax: all objects in the frameset are fit for a linear proper motion and a parallax. In all cases, objects are assumed to be stars with small values of proper motion and parallax.
msbID	[nspid]Multiframe	WSA NonSurvey	Id min.-schedulable block {image primary HDU keyword: MSBID}	varchar	64		NONE	ID_NUMBER
msbRejected	[nspid]Multiframe	WSA NonSurvey	Cause of MSB rejection, default if not rejected {image primary HDU keyword: MSBFUD}	varchar	256		NONE
muDec	[nspid]Variability	WSA NonSurvey	Proper motion in Dec	real	4	mas/yr	-0.9999995e9	POS_EQ_PMDEC
			The Variability table contains statistics from the set of observations of each source. At present, the mean ra and dec and the error in two tangential directions are calculated. The "ra" direction is defined as tangential to both the radial direction and the cartesian z-axis and the "dec" direction is defined as both the radial direction and the "ra" direction. Since the current model is just the mean and standard deviation of the data, then the chi-squared of the fit=1. Data from good frames across all bands go into the astrometric model determination. This will include bands in non-synoptic filters: the one observation in these bands can help. In future releases a fit will be made to the rms data as a function of magnitude in each band, as has already happened for photometric data and a motion model that incorporates proper motion (and possibly parallax) will be used. The motion model is a parameter in the VarFrameSetInfo table.
multiframeID	[nspid]CurrentAstrometry, [nspid]Detection, [nspid]MultiframeDetector, [nspid]PreviousAstrometry, [nspid]PreviousMFDZP, [nspid]ProgrammeFrame, [nspid]SourceXDetectionBestMatch	WSA NonSurvey	the UID of the relevant multiframe	bigint	8			ID_FRAME
multiframeID	[nspid]Multiframe	WSA NonSurvey	UID of the multiframe (assigned sequentially by the archive ingest process)	bigint	8			ID_FRAME
multiframeID	[nspid]Provenance	WSA NonSurvey	the UID of the component frame	bigint	8			ID_FRAME
muRa	[nspid]Variability	WSA NonSurvey	Proper motion in RA	real	4	mas/yr	-0.9999995e9	POS_EQ_PMRA
			The Variability table contains statistics from the set of observations of each source. At present, the mean ra and dec and the error in two tangential directions are calculated. The "ra" direction is defined as tangential to both the radial direction and the cartesian z-axis and the "dec" direction is defined as both the radial direction and the "ra" direction. Since the current model is just the mean and standard deviation of the data, then the chi-squared of the fit=1. Data from good frames across all bands go into the astrometric model determination. This will include bands in non-synoptic filters: the one observation in these bands can help. In future releases a fit will be made to the rms data as a function of magnitude in each band, as has already happened for photometric data and a motion model that incorporates proper motion (and possibly parallax) will be used. The motion model is a parameter in the VarFrameSetInfo table.