VSA Browser

Glossary of VSA attributes

This Glossary alphabetically lists all attributes used in the VSAv20110218 database(s) held in the VSA. If you would like to have more information about the schema tables please use the VSAv20110218 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

Name Schema Table Database Description Type Length Unit Default Value Unified Content Descriptor

PA combo17CDFSSource COMBO17 position angle, measured West to North real 4 deg

PA nvssSource NVSS [-90, 90] Position angle of fitted major axis real 4 degress POS_POS-ANG

pa first08Jul16Source, firstSource FIRST position angle (east of north) derived from the elliptical Gaussian model for the source real 4 degrees POS_POS-ANG

pa svNgc253Detection VSASVNGC253 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 svOrionDetection VSASVORION 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 ultravistaDetection VSAUltraVISTA ellipse fit orientation to x axis {catalogue TType keyword: Position_angle}
Angle of ellipse major axis wrt x axis counterclockwise. real 4 degrees POS_POS-ANG

pa ultravistaDetection, videoDetection VSAQC ellipse fit orientation to x axis {catalogue TType keyword: Position_angle}
Angle of ellipse major axis wrt x axis counterclockwise. real 4 degrees POS_POS-ANG

pa ultravistaListRemeasurement VSAUltraVISTA 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 ultravistaListRemeasurement, vhsDetection, vhsListRemeasurement, videoListRemeasurement, vikingDetection, vikingListRemeasurement, vmcDetection, vmcListRemeasurement, vvvDetection, vvvListRemeasurement VSAQC 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

pairingCriterion Programme VSAQC The pairing criterion for associating detections into merged sources real 4 Degrees ??

pairingCriterion Programme VSASVNGC253 The pairing criterion for associating detections into merged sources real 4 Degrees ??

pairingCriterion Programme VSASVORION The pairing criterion for associating detections into merged sources real 4 Degrees ??

pairingCriterion Programme VSAUltraVISTA The pairing criterion for associating detections into merged sources real 4 Degrees ??

pairingCriterion Programme VSAVHS The pairing criterion for associating detections into merged sources real 4 Degrees ??

pairingCriterion Programme VSAVIDEO The pairing criterion for associating detections into merged sources real 4 Degrees ??

pairingCriterion Programme VSAVIKING The pairing criterion for associating detections into merged sources real 4 Degrees ??

pairingCriterion Programme VSAVMC The pairing criterion for associating detections into merged sources real 4 Degrees ??

pairingCriterion Programme VSAVVV The pairing criterion for associating detections into merged sources real 4 Degrees ??

parallax ultravistaVariability VSAUltraVISTA Parallax of star 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.

parallax ultravistaVariability, videoVariability, vikingVariability, vmcVariability, vvvVariability VSAQC Parallax of star 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.

PARK grs_ngpSource, grs_ranSource, grs_sgpSource TWODFGRS k classification parameter = k / k_star real 4

PARMU grs_ngpSource, grs_ranSource, grs_sgpSource TWODFGRS mu classification parameter = mu / mu_star real 4

patternString Multiframe VSASVNGC253 SADT pattern ID {image primary HDU keyword: HIERARCH ESO OCS SADT PATTERN} varchar 64 NONE

patternString Multiframe VSASVORION SADT pattern ID {image primary HDU keyword: HIERARCH ESO OCS SADT PATTERN} varchar 64 NONE

patternString Multiframe VSAUltraVISTA SADT pattern ID {image primary HDU keyword: HIERARCH ESO OCS SADT PATTERN} varchar 64 NONE

patternString Multiframe VSAVHS SADT pattern ID {image primary HDU keyword: HIERARCH ESO OCS SADT PATTERN} varchar 64 NONE

patternString Multiframe VSAVIDEO SADT pattern ID {image primary HDU keyword: HIERARCH ESO OCS SADT PATTERN} varchar 64 NONE

patternString Multiframe VSAVIKING SADT pattern ID {image primary HDU keyword: HIERARCH ESO OCS SADT PATTERN} varchar 64 NONE

patternString Multiframe VSAVMC SADT pattern ID {image primary HDU keyword: HIERARCH ESO OCS SADT PATTERN} varchar 64 NONE

patternString Multiframe VSAVVV SADT pattern ID {image primary HDU keyword: HIERARCH ESO OCS SADT PATTERN} varchar 64 NONE

patternString ultravistaMultiframe, vhsMultiframe, videoMultiframe, vikingMultiframe, vmcMultiframe, vvvMultiframe VSAQC SADT pattern ID varchar 64 NONE

petroFlux svNgc253Detection VSASVNGC253 flux within circular aperture to k × r_p ; k = 2 {catalogue TType keyword: Petr_flux} real 4 ADU PHOT_INTENSITY_ADU

petroFlux svOrionDetection VSASVORION flux within circular aperture to k × r_p ; k = 2 {catalogue TType keyword: Petr_flux} real 4 ADU PHOT_INTENSITY_ADU

petroFlux ultravistaDetection VSAUltraVISTA flux within Petrosian radius circular aperture (SE: FLUX_PETRO) {catalogue TType keyword: Petr_flux} real 4 ADU PHOT_INTENSITY_ADU

petroFlux ultravistaDetection, videoDetection VSAQC flux within Petrosian radius circular aperture (SE: FLUX_PETRO) {catalogue TType keyword: Petr_flux} real 4 ADU PHOT_INTENSITY_ADU

petroFlux ultravistaListRemeasurement VSAUltraVISTA flux within circular aperture to k × r_p ; k = 2 {catalogue TType keyword: Petr_flux} real 4 ADU PHOT_INTENSITY_ADU

petroFlux ultravistaListRemeasurement, vhsDetection, vhsListRemeasurement, videoListRemeasurement, vikingDetection, vikingListRemeasurement, vmcDetection, vmcListRemeasurement, vvvDetection, vvvListRemeasurement VSAQC flux within circular aperture to k × r_p ; k = 2 {catalogue TType keyword: Petr_flux} real 4 ADU PHOT_INTENSITY_ADU

petroFluxErr svNgc253Detection VSASVNGC253 error on Petrosian flux {catalogue TType keyword: Petr_flux_err} real 4 ADU ERROR

petroFluxErr svOrionDetection VSASVORION error on Petrosian flux {catalogue TType keyword: Petr_flux_err} real 4 ADU ERROR

petroFluxErr ultravistaDetection VSAUltraVISTA error on Petrosian flux (SE: FLUXERR_PETRO) {catalogue TType keyword: Petr_flux_err} real 4 ADU ERROR

petroFluxErr ultravistaDetection, videoDetection VSAQC error on Petrosian flux (SE: FLUXERR_PETRO) {catalogue TType keyword: Petr_flux_err} real 4 ADU ERROR

petroFluxErr ultravistaListRemeasurement VSAUltraVISTA error on Petrosian flux {catalogue TType keyword: Petr_flux_err} real 4 ADU ERROR

petroFluxErr ultravistaListRemeasurement, vhsDetection, vhsListRemeasurement, videoListRemeasurement, vikingDetection, vikingListRemeasurement, vmcDetection, vmcListRemeasurement, vvvDetection, vvvListRemeasurement VSAQC error on Petrosian flux {catalogue TType keyword: Petr_flux_err} real 4 ADU ERROR

petroMag svNgc253Detection VSASVNGC253 Calibrated Petrosian magnitude within circular aperture r_p real 4 mag PHOT_INT-MAG

petroMag svOrionDetection VSASVORION Calibrated Petrosian magnitude within circular aperture r_p real 4 mag PHOT_INT-MAG

petroMag ultravistaDetection VSAUltraVISTA Calibrated Petrosian magnitude within circular aperture r_p real 4 mag PHOT_INT-MAG

petroMag ultravistaDetection, ultravistaListRemeasurement, vhsDetection, vhsListRemeasurement, videoDetection, videoListRemeasurement, vikingDetection, vikingListRemeasurement, vmcDetection, vmcListRemeasurement, vvvDetection, vvvListRemeasurement VSAQC Calibrated Petrosian magnitude within circular aperture r_p real 4 mag PHOT_INT-MAG

petroMagErr svNgc253Detection VSASVNGC253 error on calibrated Petrosian magnitude real 4 mag ERROR

petroMagErr svOrionDetection VSASVORION error on calibrated Petrosian magnitude real 4 mag ERROR

petroMagErr ultravistaDetection VSAUltraVISTA error on calibrated Petrosian magnitude real 4 mag ERROR

petroMagErr ultravistaDetection, ultravistaListRemeasurement, vhsDetection, vhsListRemeasurement, videoDetection, videoListRemeasurement, vikingDetection, vikingListRemeasurement, vmcDetection, vmcListRemeasurement, vvvDetection, vvvListRemeasurement VSAQC error on calibrated Petrosian magnitude real 4 mag ERROR

petroRad svNgc253Detection VSASVNGC253 r_p as defined in Yasuda et al. 2001 AJ 112 1104 {catalogue TType keyword: Petr_radius} real 4 pixels EXTENSION_RAD

petroRad svOrionDetection VSASVORION r_p as defined in Yasuda et al. 2001 AJ 112 1104 {catalogue TType keyword: Petr_radius} real 4 pixels EXTENSION_RAD

petroRad ultravistaDetection VSAUltraVISTA Petrosian radius (SE: PETRO_RADIUS*A_IMAGE) {catalogue TType keyword: Petr_radius} real 4 pixels EXTENSION_RAD

Since <FLUX>_RADIUS is expressed in multiples of the major axis, <FLUX>_RADIUS is multiplied by A_IMAGE to convert to pixels.

petroRad ultravistaDetection, videoDetection VSAQC Petrosian radius (SE: PETRO_RADIUS*A_IMAGE) {catalogue TType keyword: Petr_radius} real 4 pixels EXTENSION_RAD

Since <FLUX>_RADIUS is expressed in multiples of the major axis, <FLUX>_RADIUS is multiplied by A_IMAGE to convert to pixels.

petroRad ultravistaListRemeasurement VSAUltraVISTA r_p as defined in Yasuda et al. 2001 AJ 112 1104 {catalogue TType keyword: Petr_radius} real 4 pixels EXTENSION_RAD

petroRad ultravistaListRemeasurement, vhsDetection, vhsListRemeasurement, videoListRemeasurement, vikingDetection, vikingListRemeasurement, vmcDetection, vmcListRemeasurement, vvvDetection, vvvListRemeasurement VSAQC r_p as defined in Yasuda et al. 2001 AJ 112 1104 {catalogue TType keyword: Petr_radius} real 4 pixels EXTENSION_RAD

PF_DEC mgcBrightSpec MGC PFr object declination in deg (J2000) float 8

PF_JMK mgcBrightSpec MGC PFr J-K colour from 2MASS real 4

PF_K mgcBrightSpec MGC PFr K magnitude from 2MASS real 4

PF_NAME mgcBrightSpec MGC PFr object name varchar 8

PF_R mgcBrightSpec MGC PFr R magnitude from USNO real 4

PF_RA mgcBrightSpec MGC PFr object right ascension in deg (J2000) float 8

PF_Z mgcBrightSpec MGC PFr redshift real 4

PF_ZQUAL mgcBrightSpec MGC PFr redshift quality tinyint 1

pFlag rosat_bsc, rosat_fsc ROSAT possible problem with position determination varchar 1 CODE_MISC

pGalaxy svNgc253Source VSASVNGC253 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:

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(class_k)=Π_iP(class_k)_i / Σ_kΠ_iP(class_k)_i
where class_k is one of star|galaxy|noise|saturated, and i denotes the i^th 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.

pGalaxy svOrionSource VSASVORION 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:

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(class_k)=Π_iP(class_k)_i / Σ_kΠ_iP(class_k)_i
where class_k is one of star|galaxy|noise|saturated, and i denotes the i^th 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.

pGalaxy ultravistaSource VSAUltraVISTA 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:

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(class_k)=Π_iP(class_k)_i / Σ_kΠ_iP(class_k)_i
where class_k is one of star|galaxy|noise|saturated, and i denotes the i^th 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.

pGalaxy ultravistaSource, vhsSource, videoSource, vikingSource, vmcSource, vmcSynopticSource, vvvSource VSAQC 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:

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(class_k)=Π_iP(class_k)_i / Σ_kΠ_iP(class_k)_i
where class_k is one of star|galaxy|noise|saturated, and i denotes the i^th 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

ph_qual twomass_sixx2_psc 2MASS flag indicating photometric quality of source varchar 3

phaRange rosat_bsc, rosat_fsc ROSAT PHA range with highest detection likelihood varchar 1 CODE_MISC

pHeight svNgc253Detection VSASVNGC253 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

pHeight svOrionDetection VSASVORION 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

pHeight ultravistaDetection VSAUltraVISTA Highest pixel value above sky (SE: FLUX_MAX) {catalogue TType keyword: Peak_height}
In counts relative to local value of sky - also zeroth order aperture flux. real 4 ADU PHOT_COUNTS_MISC

pHeight ultravistaDetection, videoDetection VSAQC Highest pixel value above sky (SE: FLUX_MAX) {catalogue TType keyword: Peak_height}
In counts relative to local value of sky - also zeroth order aperture flux. real 4 ADU PHOT_COUNTS_MISC

pHeight ultravistaListRemeasurement VSAUltraVISTA 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

pHeight ultravistaListRemeasurement, vhsDetection, vhsListRemeasurement, videoListRemeasurement, vikingDetection, vikingListRemeasurement, vmcDetection, vmcListRemeasurement, vvvDetection, vvvListRemeasurement VSAQC 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 svNgc253Detection VSASVNGC253 Error in peak height {catalogue TType keyword: Peak_height_err} real 4 ADU ERROR

pHeightErr svOrionDetection VSASVORION Error in peak height {catalogue TType keyword: Peak_height_err} real 4 ADU ERROR

pHeightErr ultravistaDetection VSAUltraVISTA Error in peak height {catalogue TType keyword: Peak_height_err}
FLUX_MAX*FLUXERR_APER1 / FLUX_APER1 real 4 ADU ERROR

pHeightErr ultravistaDetection, videoDetection VSAQC Error in peak height {catalogue TType keyword: Peak_height_err}
FLUX_MAX*FLUXERR_APER1 / FLUX_APER1 real 4 ADU ERROR

pHeightErr ultravistaListRemeasurement VSAUltraVISTA Error in peak height {catalogue TType keyword: Peak_height_err} real 4 ADU ERROR

pHeightErr ultravistaListRemeasurement, vhsDetection, vhsListRemeasurement, videoListRemeasurement, vikingDetection, vikingListRemeasurement, vmcDetection, vmcListRemeasurement, vvvDetection, vvvListRemeasurement VSAQC 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

phot_flag combo17CDFSSource COMBO17 flags on photometry: bit 0-7 (corresponding to values 0-128) are original SExtractor flags, bit 9-11 set by COMBO-17 photometry, bit 9 indicates only potential problem from bright neighbours or reflexes from the optics (check images), bit 10 indicates uncorrected hot pixels, bit 11 is set interactively when photometry is erroneous smallint 2

photZPCat MultiframeDetector VSASVNGC253 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.

photZPCat MultiframeDetector VSASVORION 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.

photZPCat MultiframeDetector VSAUltraVISTA 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.

photZPCat MultiframeDetector VSAVHS 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.

photZPCat MultiframeDetector VSAVIDEO 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.

photZPCat MultiframeDetector VSAVIKING 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.

photZPCat MultiframeDetector VSAVMC 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.

photZPCat MultiframeDetector VSAVVV 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.

photZPCat PreviousMFDZP VSASVNGC253 Photometric zeropoint for default extinction in catalogue header real 4 mag -0.9999995e9

photZPCat PreviousMFDZP VSASVORION Photometric zeropoint for default extinction in catalogue header real 4 mag -0.9999995e9

photZPCat PreviousMFDZP VSAUltraVISTA Photometric zeropoint for default extinction in catalogue header real 4 mag -0.9999995e9

photZPCat PreviousMFDZP VSAVHS Photometric zeropoint for default extinction in catalogue header real 4 mag -0.9999995e9

photZPCat PreviousMFDZP VSAVIDEO Photometric zeropoint for default extinction in catalogue header real 4 mag -0.9999995e9

photZPCat PreviousMFDZP VSAVIKING Photometric zeropoint for default extinction in catalogue header real 4 mag -0.9999995e9

photZPCat PreviousMFDZP VSAVMC Photometric zeropoint for default extinction in catalogue header real 4 mag -0.9999995e9

photZPCat PreviousMFDZP VSAVVV Photometric zeropoint for default extinction in catalogue header real 4 mag -0.9999995e9

photZPCat ultravistaMultiframeDetector, vhsMultiframeDetector, videoMultiframeDetector, vikingMultiframeDetector, vmcMultiframeDetector, vvvMultiframeDetector VSAQC Photometric zero point for default extinction for the catalogue data real 4 mags -0.9999995e9 ??

photZPErrCat MultiframeDetector VSASVNGC253 Photometric zero point error for the catalogue data {catalogue extension keyword: MAGZRR} 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.

photZPErrCat MultiframeDetector VSASVORION Photometric zero point error for the catalogue data {catalogue extension keyword: MAGZRR} 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.

photZPErrCat MultiframeDetector VSAUltraVISTA Photometric zero point error for the catalogue data {catalogue extension keyword: MAGZRR} 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.

photZPErrCat MultiframeDetector VSAVHS Photometric zero point error for the catalogue data {catalogue extension keyword: MAGZRR} 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.

photZPErrCat MultiframeDetector VSAVIDEO Photometric zero point error for the catalogue data {catalogue extension keyword: MAGZRR} 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.

photZPErrCat MultiframeDetector VSAVIKING Photometric zero point error for the catalogue data {catalogue extension keyword: MAGZRR} 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.

photZPErrCat MultiframeDetector VSAVMC Photometric zero point error for the catalogue data {catalogue extension keyword: MAGZRR} 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.

photZPErrCat MultiframeDetector VSAVVV Photometric zero point error for the catalogue data {catalogue extension keyword: MAGZRR} 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.

photZPErrCat PreviousMFDZP VSASVNGC253 Photometric zeropoint error in catalogue header real 4 mag -0.9999995e9

photZPErrCat PreviousMFDZP VSASVORION Photometric zeropoint error in catalogue header real 4 mag -0.9999995e9

photZPErrCat PreviousMFDZP VSAUltraVISTA Photometric zeropoint error in catalogue header real 4 mag -0.9999995e9

photZPErrCat PreviousMFDZP VSAVHS Photometric zeropoint error in catalogue header real 4 mag -0.9999995e9

photZPErrCat PreviousMFDZP VSAVIDEO Photometric zeropoint error in catalogue header real 4 mag -0.9999995e9

photZPErrCat PreviousMFDZP VSAVIKING Photometric zeropoint error in catalogue header real 4 mag -0.9999995e9

photZPErrCat PreviousMFDZP VSAVMC Photometric zeropoint error in catalogue header real 4 mag -0.9999995e9

photZPErrCat PreviousMFDZP VSAVVV Photometric zeropoint error in catalogue header real 4 mag -0.9999995e9

photZPErrCat ultravistaMultiframeDetector, vhsMultiframeDetector, videoMultiframeDetector, vikingMultiframeDetector, vmcMultiframeDetector, vvvMultiframeDetector VSAQC Photometric zero point error for the catalogue data real 4 mags -0.9999995e9 ??

picoi Multiframe VSASVNGC253 PI-COI name. {image primary HDU keyword: PI-COI} varchar 64 NONE

picoi Multiframe VSASVORION PI-COI name. {image primary HDU keyword: PI-COI} varchar 64 NONE

picoi Multiframe VSAUltraVISTA PI-COI name. {image primary HDU keyword: PI-COI} varchar 64 NONE

picoi Multiframe VSAVHS PI-COI name. {image primary HDU keyword: PI-COI} varchar 64 NONE

picoi Multiframe VSAVIDEO PI-COI name. {image primary HDU keyword: PI-COI} varchar 64 NONE

picoi Multiframe VSAVIKING PI-COI name. {image primary HDU keyword: PI-COI} varchar 64 NONE

picoi Multiframe VSAVMC PI-COI name. {image primary HDU keyword: PI-COI} varchar 64 NONE

picoi Multiframe VSAVVV PI-COI name. {image primary HDU keyword: PI-COI} varchar 64 NONE

picoi ultravistaMultiframe, vhsMultiframe, videoMultiframe, vikingMultiframe, vmcMultiframe, vvvMultiframe VSAQC PI-COI name. varchar 64 NONE

PID_R spectra SIXDF PID number read from R frame int 4

PID_V spectra SIXDF PID number read from V frame int 4

PIVOT_R spectra SIXDF R pivot number smallint 2

PIVOT_V spectra SIXDF V pivot number smallint 2

pixelSize RequiredMosaic VSASVNGC253 The final pixel size of the mosaic real 4 arcsec ??

pixelSize RequiredMosaic VSASVORION The final pixel size of the mosaic real 4 arcsec ??

pixelSize RequiredMosaic VSAUltraVISTA The final pixel size of the mosaic real 4 arcsec ??

pixelSize RequiredMosaic VSAVHS The final pixel size of the mosaic real 4 arcsec ??

pixelSize RequiredMosaic VSAVIDEO The final pixel size of the mosaic real 4 arcsec ??

pixelSize RequiredMosaic VSAVIKING The final pixel size of the mosaic real 4 arcsec ??

pixelSize RequiredMosaic VSAVMC The final pixel size of the mosaic real 4 arcsec ??

pixelSize RequiredMosaic VSAVVV The final pixel size of the mosaic real 4 arcsec ??

PMAG grs_ngpSource, grs_ranSource, grs_sgpSource TWODFGRS Unmatched raw APM profile integrated mag real 4

pmDec ukirtFSstars VSASVNGC253 Proper motion in Dec real 4 arcsec per year 0.0

pmDec ukirtFSstars VSASVORION Proper motion in Dec real 4 arcsec per year 0.0

pmDec ukirtFSstars VSAUltraVISTA Proper motion in Dec real 4 arcsec per year 0.0

pmDec ukirtFSstars VSAVHS Proper motion in Dec real 4 arcsec per year 0.0

pmDec ukirtFSstars VSAVIDEO Proper motion in Dec real 4 arcsec per year 0.0

pmDec ukirtFSstars VSAVIKING Proper motion in Dec real 4 arcsec per year 0.0

pmDec ukirtFSstars VSAVMC Proper motion in Dec real 4 arcsec per year 0.0

pmDec ukirtFSstars VSAVVV Proper motion in Dec real 4 arcsec per year 0.0

pmRA ukirtFSstars VSASVNGC253 Proper motion in RA real 4 arcsec per year 0.0

pmRA ukirtFSstars VSASVORION Proper motion in RA real 4 arcsec per year 0.0

pmRA ukirtFSstars VSAUltraVISTA Proper motion in RA real 4 arcsec per year 0.0

pmRA ukirtFSstars VSAVHS Proper motion in RA real 4 arcsec per year 0.0

pmRA ukirtFSstars VSAVIDEO Proper motion in RA real 4 arcsec per year 0.0

pmRA ukirtFSstars VSAVIKING Proper motion in RA real 4 arcsec per year 0.0

pmRA ukirtFSstars VSAVMC Proper motion in RA real 4 arcsec per year 0.0

pmRA ukirtFSstars VSAVVV Proper motion in RA real 4 arcsec per year 0.0

PN_1_BG twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM The PN band 1 background map.
Made using a 12 x 12 nodes spline fit on the source-free individual-band images. real 4 counts/pixel

PN_1_DET_ML twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 1 Maximum likelihood real 4

PN_1_EXP twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM The PN band 1 exposure map, combining the mirror vignetting, detector efficiency, bad pixels and CCD gaps.
The PSF weighted mean of the area of the subimages (radius 60 arcseconds) in the individual-band exposure maps. real 4 s

PN_1_FLUX twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 1 flux real 4 erg/cm**2/s

PN_1_FLUX_ERR twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 1 flux error real 4 erg/cm**2/s

PN_1_RATE twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 1 Count rates real 4 counts/s

PN_1_RATE_ERR twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 1 Count rates error real 4 counts/s

PN_1_VIG twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM The PN band 1 vignetting value. real 4

PN_2_BG twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM The PN band 2 background map.
Made using a 12 x 12 nodes spline fit on the source-free individual-band images. real 4 counts/pixel

PN_2_DET_ML twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 2 Maximum likelihood real 4

PN_2_EXP twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM The PN band 2 exposure map, combining the mirror vignetting, detector efficiency, bad pixels and CCD gaps.
The PSF weighted mean of the area of the subimages (radius 60 arcseconds) in the individual-band exposure maps. real 4 s

PN_2_FLUX twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 2 flux real 4 erg/cm**2/s

PN_2_FLUX_ERR twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 2 flux error real 4 erg/cm**2/s

PN_2_RATE twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 2 Count rates real 4 counts/s

PN_2_RATE_ERR twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 2 Count rates error real 4 counts/s

PN_2_VIG twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM The PN band 2 vignetting value. real 4

PN_3_BG twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM The PN band 3 background map.
Made using a 12 x 12 nodes spline fit on the source-free individual-band images. real 4 counts/pixel

PN_3_DET_ML twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 3 Maximum likelihood real 4

PN_3_EXP twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM The PN band 3 exposure map, combining the mirror vignetting, detector efficiency, bad pixels and CCD gaps.
The PSF weighted mean of the area of the subimages (radius 60 arcseconds) in the individual-band exposure maps. real 4 s

PN_3_FLUX twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 3 flux real 4 erg/cm**2/s

PN_3_FLUX_ERR twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 3 flux error real 4 erg/cm**2/s

PN_3_RATE twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 3 Count rates real 4 counts/s

PN_3_RATE_ERR twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 3 Count rates error real 4 counts/s

PN_3_VIG twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM The PN band 3 vignetting value. real 4

PN_4_BG twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM The PN band 4 background map.
Made using a 12 x 12 nodes spline fit on the source-free individual-band images. real 4 counts/pixel

PN_4_DET_ML twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 4 Maximum likelihood real 4

PN_4_EXP twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM The PN band 4 exposure map, combining the mirror vignetting, detector efficiency, bad pixels and CCD gaps.
The PSF weighted mean of the area of the subimages (radius 60 arcseconds) in the individual-band exposure maps. real 4 s

PN_4_FLUX twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 4 flux real 4 erg/cm**2/s

PN_4_FLUX_ERR twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 4 flux error real 4 erg/cm**2/s

PN_4_RATE twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 4 Count rates real 4 counts/s

PN_4_RATE_ERR twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 4 Count rates error real 4 counts/s

PN_4_VIG twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM The PN band 4 vignetting value. real 4

PN_5_BG twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM The PN band 5 background map.
Made using a 12 x 12 nodes spline fit on the source-free individual-band images. real 4 counts/pixel

PN_5_DET_ML twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 5 Maximum likelihood real 4

PN_5_EXP twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM The PN band 5 exposure map, combining the mirror vignetting, detector efficiency, bad pixels and CCD gaps.
The PSF weighted mean of the area of the subimages (radius 60 arcseconds) in the individual-band exposure maps. real 4 s

PN_5_FLUX twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 5 flux real 4 erg/cm**2/s

PN_5_FLUX_ERR twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 5 flux error real 4 erg/cm**2/s

PN_5_RATE twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 5 Count rates real 4 counts/s

PN_5_RATE_ERR twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 5 Count rates error real 4 counts/s

PN_5_VIG twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM The PN band 5 vignetting value. real 4

PN_8_CTS twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM Combined band source counts real 4 counts

PN_8_CTS_ERR twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM Combined band source counts 1 σ error real 4 counts

PN_8_DET_ML twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 8 Maximum likelihood real 4

PN_8_FLUX twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 8 flux real 4 erg/cm**2/s

PN_8_FLUX_ERR twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 8 flux error real 4 erg/cm**2/s

PN_8_RATE twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 8 Count rates real 4 counts/s

PN_8_RATE_ERR twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 8 Count rates error real 4 counts/s

PN_9_DET_ML twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 9 Maximum likelihood real 4

PN_9_FLUX twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 9 flux real 4 erg/cm**2/s

PN_9_FLUX_ERR twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 9 flux error real 4 erg/cm**2/s

PN_9_RATE twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 9 Count rates real 4 counts/s

PN_9_RATE_ERR twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN band 9 Count rates error real 4 counts/s

PN_CHI2PROB twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM The Chi² probability (based on the null hypothesis) that the source as detected by the PN camera is constant.
The Pearson approximation to Chi² for Poissonian data was used, in which the model is used as the estimator of its own variance . If more than one exposure (that is, time series) is available for this source the smallest value of probability was used. real 4

PN_FILTER twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN filter. The options are Thick, Medium, Thin1, Thin2, and Open, depending on the efficiency of the optical blocking. varchar 6

PN_FLAG twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN flag string made of the flags 1 - 12 (counted from left to right) for the PN source detection.
In case where the camera was not used in the source detection a dash is given. In case a source was not detected by the PN the flags are all set to False (default). Flag 10 is not used. varchar 12

PN_HR1 twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM The PN hardness ratio between the bands 1 & 2
In the case where the rate in one band is 0.0 (i.e., too faint to be detected in this band) the hardness ratio will be -1 or +1 which is only a lower or upper limit, respectively. real 4

PN_HR1_ERR twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM The 1 σ error of the PN hardness ratio between the bands 1 & 2 real 4

PN_HR2 twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM The PN hardness ratio between the bands 2 & 3
In the case where the rate in one band is 0.0 (i.e., too faint to be detected in this band) the hardness ratio will be -1 or +1 which is only a lower or upper limit, respectively. real 4

PN_HR2_ERR twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM The 1 σ error of the PN hardness ratio between the bands 2 & 3 real 4

PN_HR3 twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM The PN hardness ratio between the bands 3 & 4
In the case where the rate in one band is 0.0 (i.e., too faint to be detected in this band) the hardness ratio will be -1 or +1 which is only a lower or upper limit, respectively. real 4

PN_HR3_ERR twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM The 1 σ error of the PN hardness ratio between the bands 3 & 4 real 4

PN_HR4 twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM The PN hardness ratio between the bands 4 & 5
In the case where the rate in one band is 0.0 (i.e., too faint to be detected in this band) the hardness ratio will be -1 or +1 which is only a lower or upper limit, respectively. real 4

PN_HR4_ERR twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM The 1 σ error of the PN hardness ratio between the bands 4 & 5 real 4

PN_MASKFRAC twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM The PSF weighted mean of the detector coverage of a detection as derived from the detection mask.
Sources which have less than 0.15 of their PSF covered by the detector are considered as being not detected. real 4

PN_OFFAX twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM The PN offaxis angle (the distance between the detection position and the onaxis position on the respective detector).
The offaxis angle for a camera can be larger than 15 arcminutes when the detection is located outside the FOV of that camera. real 4 arcmin

PN_ONTIME twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM The PN ontime value (the total good exposure time (after GTI filtering) of the CCD where the detection is positioned).
If a source position falls into CCD gaps or outside of the detector it will have a NULL given. real 4 s

PN_SUBMODE twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM PN observing mode. The options are full frame mode with the full FOV exposed (in two sub-modes), and large window mode with only parts of the FOV exposed. varchar 23

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 svNgc253Source VSASVNGC253 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:

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(class_k)=Π_iP(class_k)_i / Σ_kΠ_iP(class_k)_i
where class_k is one of star|galaxy|noise|saturated, and i denotes the i^th 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.

pNoise svOrionSource VSASVORION 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:

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(class_k)=Π_iP(class_k)_i / Σ_kΠ_iP(class_k)_i
where class_k is one of star|galaxy|noise|saturated, and i denotes the i^th 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.

pNoise ultravistaSource VSAUltraVISTA 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:

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(class_k)=Π_iP(class_k)_i / Σ_kΠ_iP(class_k)_i
where class_k is one of star|galaxy|noise|saturated, and i denotes the i^th 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.

pNoise ultravistaSource, vhsSource, videoSource, vikingSource, vmcSource, vmcSynopticSource, vvvSource VSAQC 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:

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(class_k)=Π_iP(class_k)_i / Σ_kΠ_iP(class_k)_i
where class_k is one of star|galaxy|noise|saturated, and i denotes the i^th 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.

polFlux nvssSource NVSS Integrated linearly polarized flux density real 4 mJy PHOT_FLUX_LINEAR

polPA nvssSource NVSS [-90,90] The position angle of polFlux real 4 degress POS_POS-EQ

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 VSASVNGC253 orientation of image x-axis to N-S float 8 Degrees -0.9999995e9 POS_POS-ANG

posAngle CurrentAstrometry VSASVORION orientation of image x-axis to N-S float 8 Degrees -0.9999995e9 POS_POS-ANG

posAngle CurrentAstrometry VSAUltraVISTA orientation of image x-axis to N-S float 8 Degrees -0.9999995e9 POS_POS-ANG

posAngle CurrentAstrometry VSAVHS orientation of image x-axis to N-S float 8 Degrees -0.9999995e9 POS_POS-ANG

posAngle CurrentAstrometry VSAVIDEO orientation of image x-axis to N-S float 8 Degrees -0.9999995e9 POS_POS-ANG

posAngle CurrentAstrometry VSAVIKING orientation of image x-axis to N-S float 8 Degrees -0.9999995e9 POS_POS-ANG

posAngle CurrentAstrometry VSAVMC orientation of image x-axis to N-S float 8 Degrees -0.9999995e9 POS_POS-ANG

posAngle CurrentAstrometry VSAVVV orientation of image x-axis to N-S float 8 Degrees -0.9999995e9 POS_POS-ANG

posAngle RequiredMosaic VSASVORION Orientation of image x-axis to N-S real 4 deg -0.9999995e9

posAngle RequiredMosaic VSAUltraVISTA Orientation of image x-axis to N-S real 4 deg -0.9999995e9

posAngle RequiredMosaic VSAVHS Orientation of image x-axis to N-S real 4 deg -0.9999995e9

posAngle RequiredMosaic VSAVIDEO Orientation of image x-axis to N-S real 4 deg -0.9999995e9

posAngle RequiredMosaic VSAVIKING Orientation of image x-axis to N-S real 4 deg -0.9999995e9

posAngle RequiredMosaic VSAVMC Orientation of image x-axis to N-S real 4 deg -0.9999995e9

posAngle RequiredMosaic VSAVVV Orientation of image x-axis to N-S real 4 deg -0.9999995e9

posAngle RequiredMosaic, RequiredStack, RequiredTile VSASVNGC253 Orientation of image x-axis to N-S real 4 deg -0.9999995e9

posAngle ultravistaCurrentAstrometry, vhsCurrentAstrometry, videoCurrentAstrometry, vikingCurrentAstrometry, vmcCurrentAstrometry, vvvCurrentAstrometry VSAQC orientation of image x-axis to N-S float 8 Degrees -0.9999995e9 POS_POS-ANG

posAngleTolerance Programme VSAQC The position angle tolerance used when creating deep stacks and tiles real 4 Degrees ??

posAngleTolerance Programme VSASVNGC253 The position angle tolerance used when creating deep stacks and tiles real 4 Degrees ??

posAngleTolerance Programme VSASVORION The position angle tolerance used when creating deep stacks and tiles real 4 Degrees ??

posAngleTolerance Programme VSAUltraVISTA The position angle tolerance used when creating deep stacks and tiles real 4 Degrees ??

posAngleTolerance Programme VSAVHS The position angle tolerance used when creating deep stacks and tiles real 4 Degrees ??

posAngleTolerance Programme VSAVIDEO The position angle tolerance used when creating deep stacks and tiles real 4 Degrees ??

posAngleTolerance Programme VSAVIKING The position angle tolerance used when creating deep stacks and tiles real 4 Degrees ??

posAngleTolerance Programme VSAVMC The position angle tolerance used when creating deep stacks and tiles real 4 Degrees ??

posAngleTolerance Programme VSAVVV The position angle tolerance used when creating deep stacks and tiles real 4 Degrees ??

POSERR twoxmm, twoxmm_v1_2, twoxmmi_dr3_v1_0 XMM Total position uncertainty in arcseconds calculated by combining the statistical error RADEC_ERR and the systematic error SYSERR as follows: POSERR = SQRT ( RADEC_ERR² + SYSERR² ). real 4 arcsec

ppErrBits svNgc253Detection VSASVNGC253 additional WFAU post-processing error bits int 4 0 CODE_MISC

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

ppErrBits svOrionDetection VSASVORION additional WFAU post-processing error bits int 4 0 CODE_MISC

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

ppErrBits ultravistaDetection VSAUltraVISTA additional WFAU post-processing error bits int 4 0 CODE_MISC

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

ppErrBits ultravistaDetection, vhsDetection, videoDetection, vikingDetection, vmcDetection, vvvDetection VSAQC additional WFAU post-processing error bits int 4 0 CODE_MISC

Post-processing error quality bit flags assigned to detections in the archive curation procedure for survey data. From least to most significant byte in the 4-byte integer attribute byte 0 (bits 0 to 7) corresponds to information on generally innocuous conditions that are nonetheless potentially significant as regards the integrity of that detection; byte 1 (bits 8 to 15) corresponds to warnings; byte 2 (bits 16 to 23) corresponds to important warnings; and finally byte 3 (bits 24 to 31) corresponds to severe warnings:

Byte Bit Detection quality issue Threshold or bit mask Applies to

Decimal Hexadecimal

0 4 Deblended 16 0x00000010 All VDFS catalogues

0 6 Bad pixel(s) in default aperture 64 0x00000040 All VDFS catalogues

2 16 Close to saturated 65536 0x00010000 All VDFS catalogues

2 17 Photometric calibration probably subject to systematic error 131072 0x00020000 VVV only

2 22 Lies within a dither offset of the stacked frame boundary 4194304 0x00400000 All catalogues

2 23 Lies within the underexposed strip (or "ear") of a tile 8388608 0x00800000 All catalogues from tiles

In this way, the higher the error quality bit flag value, the more likely it is that the detection is spurious. The decimal threshold (column 4) gives the minimum value of the quality flag for a detection having the given condition (since other bits in the flag may be set also; the corresponding hexadecimal value, where each digit corresponds to 4 bits in the flag, can be easier to compute when writing SQL queries to test for a given condition). For example, to exclude all Ks band sources in the VHS having any error quality condition other than informational ones, include a predicate ... AND kppErrBits ≤ 255. See the SQL Cookbook and other online pages for further information.

ppErrBits ultravistaListRemeasurement VSAUltraVISTA additional WFAU post-processing error bits int 4 0 CODE_MISC

ppErrBits ultravistaListRemeasurement, vhsListRemeasurement, videoListRemeasurement, vikingListRemeasurement, vmcListRemeasurement, vvvListRemeasurement VSAQC additional WFAU post-processing error bits int 4 0 CODE_MISC

ppErrBitsStatus ProgrammeFrame VSAQC Bit flag to denote whether detection quality flagging has been done on this multiframe for this programme. int 4 0

ppErrBitsStatus ProgrammeFrame VSASVNGC253 Bit flag to denote whether detection quality flagging has been done on this multiframe for this programme. int 4 0

ppErrBitsStatus ProgrammeFrame VSASVORION Bit flag to denote whether detection quality flagging has been done on this multiframe for this programme. int 4 0

ppErrBitsStatus ProgrammeFrame VSAUltraVISTA Bit flag to denote whether detection quality flagging has been done on this multiframe for this programme. int 4 0

ppErrBitsStatus ProgrammeFrame VSAVHS Bit flag to denote whether detection quality flagging has been done on this multiframe for this programme. int 4 0

ppErrBitsStatus ProgrammeFrame VSAVIDEO Bit flag to denote whether detection quality flagging has been done on this multiframe for this programme. int 4 0

ppErrBitsStatus ProgrammeFrame VSAVIKING Bit flag to denote whether detection quality flagging has been done on this multiframe for this programme. int 4 0

ppErrBitsStatus ProgrammeFrame VSAVMC Bit flag to denote whether detection quality flagging has been done on this multiframe for this programme. int 4 0

ppErrBitsStatus ProgrammeFrame VSAVVV Bit flag to denote whether detection quality flagging has been done on this multiframe for this programme. int 4 0

previewv Multiframe VSASVNGC253 Version of previ {image primary HDU keyword: PREVIEWV} varchar 64 NONE

previewv Multiframe VSASVORION Version of previ {image primary HDU keyword: PREVIEWV} varchar 64 NONE

previewv Multiframe VSAUltraVISTA Version of previ {image primary HDU keyword: PREVIEWV} varchar 64 NONE

previewv Multiframe VSAVHS Version of previ {image primary HDU keyword: PREVIEWV} varchar 64 NONE

previewv Multiframe VSAVIDEO Version of previ {image primary HDU keyword: PREVIEWV} varchar 64 NONE

previewv Multiframe VSAVIKING Version of previ {image primary HDU keyword: PREVIEWV} varchar 64 NONE

previewv Multiframe VSAVMC Version of previ {image primary HDU keyword: PREVIEWV} varchar 64 NONE

previewv Multiframe VSAVVV Version of previ {image primary HDU keyword: PREVIEWV} varchar 64 NONE

previewv ultravistaMultiframe, vhsMultiframe, videoMultiframe, vikingMultiframe, vmcMultiframe, vvvMultiframe VSAQC Version of previ varchar 64 NONE

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

PRIORITY agntwomass, denisi, denisj, durukst, fsc, hes, hipass, nvss, rass, shapley, sumss, supercos, twomass SIXDF survey weight smallint 2

priOrSec svNgc253Source VSASVNGC253 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 VIRCam, 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 svOrionSource VSASVORION 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 VIRCam, 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 ultravistaSource VSAUltraVISTA 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 VIRCam, 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 ultravistaSource, vhsSource, videoSource, vikingSource, vmcSource, vvvSource VSAQC 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 VIRCam, 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 ultravistaSourceRemeasurement VSAUltraVISTA 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 VIRCam, 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 ultravistaSourceRemeasurement, vhsSourceRemeasurement, videoSourceRemeasurement, vikingSourceRemeasurement, vmcSourceRemeasurement, vvvSourceRemeasurement VSAQC 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 VIRCam, 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).

PROB grs_ngpSource, grs_ranSource, grs_sgpSource TWODFGRS psi classification parameter: for eyeballed galaxies: psi*1000 = (10000 + abs(jon) + psi*100); for eyeballed non-galaxies: psi*1000 = -(10000 + abs(jon) + psi*100) real 4

productID ProgrammeFrame VSAQC Product ID of deep stack frame (or intermediate stack if used as a deep stack). {image primary HDU keyword: PRODID} bigint 8 -99999999

productID ProgrammeFrame VSASVNGC253 Product ID of deep stack frame (or intermediate stack if used as a deep stack). {image primary HDU keyword: PRODID} bigint 8 -99999999

productID ProgrammeFrame VSASVORION Product ID of deep stack frame (or intermediate stack if used as a deep stack). {image primary HDU keyword: PRODID} bigint 8 -99999999

productID ProgrammeFrame VSAUltraVISTA Product ID of deep stack frame (or intermediate stack if used as a deep stack). {image primary HDU keyword: PRODID} bigint 8 -99999999

productID ProgrammeFrame VSAVHS Product ID of deep stack frame (or intermediate stack if used as a deep stack). {image primary HDU keyword: PRODID} bigint 8 -99999999

productID ProgrammeFrame VSAVIDEO Product ID of deep stack frame (or intermediate stack if used as a deep stack). {image primary HDU keyword: PRODID} bigint 8 -99999999

productID ProgrammeFrame VSAVIKING Product ID of deep stack frame (or intermediate stack if used as a deep stack). {image primary HDU keyword: PRODID} bigint 8 -99999999

productID ProgrammeFrame VSAVMC Product ID of deep stack frame (or intermediate stack if used as a deep stack). {image primary HDU keyword: PRODID} bigint 8 -99999999

productID ProgrammeFrame VSAVVV Product ID of deep stack frame (or intermediate stack if used as a deep stack). {image primary HDU keyword: PRODID} bigint 8 -99999999

productID RequiredDiffImage VSASVNGC253 A unique identifier assigned to each required difference image product entry int 4 ??

productID RequiredDiffImage VSASVORION A unique identifier assigned to each required difference image product entry int 4 ??

productID RequiredDiffImage VSAUltraVISTA A unique identifier assigned to each required difference image product entry int 4 ??

productID RequiredDiffImage VSAVHS A unique identifier assigned to each required difference image product entry int 4 ??

productID RequiredDiffImage VSAVIDEO A unique identifier assigned to each required difference image product entry int 4 ??

productID RequiredDiffImage VSAVIKING A unique identifier assigned to each required difference image product entry int 4 ??

productID RequiredDiffImage VSAVMC A unique identifier assigned to each required difference image product entry int 4 ??

productID RequiredDiffImage VSAVVV A unique identifier assigned to each required difference image product entry int 4 ??

productID RequiredMosaic VSASVNGC253 A unique identifier assigned to each required mosaic product entry int 4 ??

productID RequiredMosaic VSASVORION A unique identifier assigned to each required mosaic product entry int 4 ??

productID RequiredMosaic VSAUltraVISTA A unique identifier assigned to each required mosaic product entry int 4 ??

productID RequiredMosaic VSAVHS A unique identifier assigned to each required mosaic product entry int 4 ??

productID RequiredMosaic VSAVIDEO A unique identifier assigned to each required mosaic product entry int 4 ??

productID RequiredMosaic VSAVIKING A unique identifier assigned to each required mosaic product entry int 4 ??

productID RequiredMosaic VSAVMC A unique identifier assigned to each required mosaic product entry int 4 ??

productID RequiredMosaic VSAVVV A unique identifier assigned to each required mosaic product entry int 4 ??

productID RequiredStack VSASVNGC253 A unique identifier assigned to each required stack product entry int 4 ??

productID RequiredStack VSASVORION A unique identifier assigned to each required stack product entry int 4 ??

productID RequiredStack VSAUltraVISTA A unique identifier assigned to each required stack product entry int 4 ??

productID RequiredStack VSAVHS A unique identifier assigned to each required stack product entry int 4 ??

productID RequiredStack VSAVIDEO A unique identifier assigned to each required stack product entry int 4 ??

productID RequiredStack VSAVIKING A unique identifier assigned to each required stack product entry int 4 ??

productID RequiredStack VSAVMC A unique identifier assigned to each required stack product entry int 4 ??

productID RequiredStack VSAVVV A unique identifier assigned to each required stack product entry int 4 ??

productID RequiredStack, RequiredTile VSAQC A unique identifier assigned to each required stack product entry int 4 ??

PROGID agntwomass, denisi, denisj, durukst, fsc, hes, hipass, nvss, rass, shapley, sumss, supercos, twomass SIXDF programme ID smallint 2

PROGID target SIXDF highest priority programme ID smallint 2

PROGID_R spectra SIXDF programme ID in R frame varchar 32

PROGID_V spectra SIXDF programme ID in V frame varchar 32

programmeID ProductLinks VSASVORION the unique programme ID int 4 ID_SURVEY

programmeID ProductLinks VSAUltraVISTA the unique programme ID int 4 ID_SURVEY

programmeID ProductLinks VSAVHS the unique programme ID int 4 ID_SURVEY

programmeID ProductLinks VSAVIDEO the unique programme ID int 4 ID_SURVEY

programmeID ProductLinks VSAVIKING the unique programme ID int 4 ID_SURVEY

programmeID ProductLinks VSAVMC the unique programme ID int 4 ID_SURVEY

programmeID ProductLinks VSAVVV the unique programme ID int 4 ID_SURVEY

programmeID ProductLinks, ProgrammeCurationHistory, ProgrammeTable, RequiredDiffImage, RequiredFilters, RequiredListDrivenProduct, RequiredMosaic, RequiredNeighbours, RequiredStack, RequiredTile VSASVNGC253 the unique programme ID int 4 ID_SURVEY

programmeID Programme VSAQC UID of the archived programme coded as above int 4 ID_SURVEY

programmeID Programme VSASVNGC253 UID of the archived programme coded as above int 4 ID_SURVEY

programmeID Programme VSASVORION UID of the archived programme coded as above int 4 ID_SURVEY

programmeID Programme VSAUltraVISTA UID of the archived programme coded as above int 4 ID_SURVEY

programmeID Programme VSAVHS UID of the archived programme coded as above int 4 ID_SURVEY

programmeID Programme VSAVIDEO UID of the archived programme coded as above int 4 ID_SURVEY

programmeID Programme VSAVIKING UID of the archived programme coded as above int 4 ID_SURVEY

programmeID Programme VSAVMC UID of the archived programme coded as above int 4 ID_SURVEY

programmeID Programme VSAVVV UID of the archived programme coded as above int 4 ID_SURVEY

programmeID ProgrammeFrame VSAQC VSA assigned programme UID {image primary HDU keyword: HIERARCH ESO OBS PROG ID} int 4 -99999999 ID_SURVEY

programmeID ProgrammeFrame VSASVNGC253 VSA assigned programme UID {image primary HDU keyword: HIERARCH ESO OBS PROG ID} int 4 -99999999 ID_SURVEY

programmeID ProgrammeFrame VSASVORION VSA assigned programme UID {image primary HDU keyword: HIERARCH ESO OBS PROG ID} int 4 -99999999 ID_SURVEY

programmeID ProgrammeFrame VSAUltraVISTA VSA assigned programme UID {image primary HDU keyword: HIERARCH ESO OBS PROG ID} int 4 -99999999 ID_SURVEY

programmeID ProgrammeFrame VSAVHS VSA assigned programme UID {image primary HDU keyword: HIERARCH ESO OBS PROG ID} int 4 -99999999 ID_SURVEY

programmeID ProgrammeFrame VSAVIDEO VSA assigned programme UID {image primary HDU keyword: HIERARCH ESO OBS PROG ID} int 4 -99999999 ID_SURVEY

programmeID ProgrammeFrame VSAVIKING VSA assigned programme UID {image primary HDU keyword: HIERARCH ESO OBS PROG ID} int 4 -99999999 ID_SURVEY

programmeID ProgrammeFrame VSAVMC VSA assigned programme UID {image primary HDU keyword: HIERARCH ESO OBS PROG ID} int 4 -99999999 ID_SURVEY

programmeID ProgrammeFrame VSAVVV VSA assigned programme UID {image primary HDU keyword: HIERARCH ESO OBS PROG ID} int 4 -99999999 ID_SURVEY

programmeID SurveyProgrammes VSAQC VSA assigned programme UID {image primary HDU keyword: PROJECT} int 4 -99999999 ID_SURVEY

programmeID SurveyProgrammes VSASVNGC253 VSA assigned programme UID {image primary HDU keyword: PROJECT} int 4 -99999999 ID_SURVEY

programmeID SurveyProgrammes VSASVORION VSA assigned programme UID {image primary HDU keyword: PROJECT} int 4 -99999999 ID_SURVEY

programmeID SurveyProgrammes VSAUltraVISTA VSA assigned programme UID {image primary HDU keyword: PROJECT} int 4 -99999999 ID_SURVEY

programmeID SurveyProgrammes VSAVHS VSA assigned programme UID {image primary HDU keyword: PROJECT} int 4 -99999999 ID_SURVEY

programmeID SurveyProgrammes VSAVIDEO VSA assigned programme UID {image primary HDU keyword: PROJECT} int 4 -99999999 ID_SURVEY

programmeID SurveyProgrammes VSAVIKING VSA assigned programme UID {image primary HDU keyword: PROJECT} int 4 -99999999 ID_SURVEY

programmeID SurveyProgrammes VSAVMC VSA assigned programme UID {image primary HDU keyword: PROJECT} int 4 -99999999 ID_SURVEY

programmeID SurveyProgrammes VSAVVV VSA assigned programme UID {image primary HDU keyword: PROJECT} int 4 -99999999 ID_SURVEY

project Multiframe VSASVNGC253 Time-allocation code varchar 64 NONE REFER_CODE

project Multiframe VSASVORION Time-allocation code varchar 64 NONE REFER_CODE

project Multiframe VSAUltraVISTA Time-allocation code varchar 64 NONE REFER_CODE

project Multiframe VSAVHS Time-allocation code varchar 64 NONE REFER_CODE

project Multiframe VSAVIDEO Time-allocation code varchar 64 NONE REFER_CODE

project Multiframe VSAVIKING Time-allocation code varchar 64 NONE REFER_CODE

project Multiframe VSAVMC Time-allocation code varchar 64 NONE REFER_CODE

project Multiframe VSAVVV Time-allocation code varchar 64 NONE REFER_CODE

project ultravistaMultiframe, vhsMultiframe, videoMultiframe, vikingMultiframe, vmcMultiframe, vvvMultiframe VSAQC Time-allocation code varchar 64 NONE REFER_CODE

projp1 CurrentAstrometry VSASVNGC253 Old style WCS {image extension keyword: PROJP1} float 8 -9.999995e+08

projp1 CurrentAstrometry VSASVORION Old style WCS {image extension keyword: PROJP1} float 8 -9.999995e+08

projp1 CurrentAstrometry VSAUltraVISTA Old style WCS {image extension keyword: PROJP1} float 8 -9.999995e+08

projp1 CurrentAstrometry VSAVHS Old style WCS {image extension keyword: PROJP1} float 8 -9.999995e+08

projp1 CurrentAstrometry VSAVIDEO Old style WCS {image extension keyword: PROJP1} float 8 -9.999995e+08

projp1 CurrentAstrometry VSAVIKING Old style WCS {image extension keyword: PROJP1} float 8 -9.999995e+08

projp1 CurrentAstrometry VSAVMC Old style WCS {image extension keyword: PROJP1} float 8 -9.999995e+08

projp1 CurrentAstrometry VSAVVV Old style WCS {image extension keyword: PROJP1} float 8 -9.999995e+08

projp1 ultravistaCurrentAstrometry, vhsCurrentAstrometry, videoCurrentAstrometry, vikingCurrentAstrometry, vmcCurrentAstrometry, vvvCurrentAstrometry VSAQC Old style WCS float 8 -9.999995e+08

projp3 CurrentAstrometry VSASVNGC253 Old style WCS {image extension keyword: PROJP3} float 8 -9.999995e+08

projp3 CurrentAstrometry VSASVORION Old style WCS {image extension keyword: PROJP3} float 8 -9.999995e+08

projp3 CurrentAstrometry VSAUltraVISTA Old style WCS {image extension keyword: PROJP3} float 8 -9.999995e+08

projp3 CurrentAstrometry VSAVHS Old style WCS {image extension keyword: PROJP3} float 8 -9.999995e+08

projp3 CurrentAstrometry VSAVIDEO Old style WCS {image extension keyword: PROJP3} float 8 -9.999995e+08

projp3 CurrentAstrometry VSAVIKING Old style WCS {image extension keyword: PROJP3} float 8 -9.999995e+08

projp3 CurrentAstrometry VSAVMC Old style WCS {image extension keyword: PROJP3} float 8 -9.999995e+08

projp3 CurrentAstrometry VSAVVV Old style WCS {image extension keyword: PROJP3} float 8 -9.999995e+08

projp3 ultravistaCurrentAstrometry, vhsCurrentAstrometry, videoCurrentAstrometry, vikingCurrentAstrometry, vmcCurrentAstrometry, vvvCurrentAstrometry VSAQC Old style WCS float 8 -9.999995e+08

projp5 CurrentAstrometry VSASVNGC253 Old style WCS {image extension keyword: PROJP5} float 8 -9.999995e+08

projp5 CurrentAstrometry VSASVORION Old style WCS {image extension keyword: PROJP5} float 8 -9.999995e+08

projp5 CurrentAstrometry VSAUltraVISTA Old style WCS {image extension keyword: PROJP5} float 8 -9.999995e+08

projp5 CurrentAstrometry VSAVHS Old style WCS {image extension keyword: PROJP5} float 8 -9.999995e+08

projp5 CurrentAstrometry VSAVIDEO Old style WCS {image extension keyword: PROJP5} float 8 -9.999995e+08

projp5 CurrentAstrometry VSAVIKING Old style WCS {image extension keyword: PROJP5} float 8 -9.999995e+08

projp5 CurrentAstrometry VSAVMC Old style WCS {image extension keyword: PROJP5} float 8 -9.999995e+08

projp5 CurrentAstrometry VSAVVV Old style WCS {image extension keyword: PROJP5} float 8 -9.999995e+08

projp5 ultravistaCurrentAstrometry, vhsCurrentAstrometry, videoCurrentAstrometry, vikingCurrentAstrometry, vmcCurrentAstrometry, vvvCurrentAstrometry VSAQC Old style WCS float 8 -9.999995e+08

propPeriod Programme VSAQC the proprietory period for any data taken for this programme in months, e.g. 12 for open time. int 4 months TIME_PERIOD

propPeriod Programme VSASVNGC253 the proprietory period for any data taken for this programme in months, e.g. 12 for open time. int 4 months TIME_PERIOD

propPeriod Programme VSASVORION the proprietory period for any data taken for this programme in months, e.g. 12 for open time. int 4 months TIME_PERIOD

propPeriod Programme VSAUltraVISTA the proprietory period for any data taken for this programme in months, e.g. 12 for open time. int 4 months TIME_PERIOD

propPeriod Programme VSAVHS the proprietory period for any data taken for this programme in months, e.g. 12 for open time. int 4 months TIME_PERIOD

propPeriod Programme VSAVIDEO the proprietory period for any data taken for this programme in months, e.g. 12 for open time. int 4 months TIME_PERIOD

propPeriod Programme VSAVIKING the proprietory period for any data taken for this programme in months, e.g. 12 for open time. int 4 months TIME_PERIOD

propPeriod Programme VSAVMC the proprietory period for any data taken for this programme in months, e.g. 12 for open time. int 4 months TIME_PERIOD

propPeriod Programme VSAVVV 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 VSAQC Logical flag indicating whether a survey is proprietary or not (1=yes; 0=no) tinyint 1 ??

proprietary Survey VSASVNGC253 Logical flag indicating whether a survey is proprietary or not (1=yes; 0=no) tinyint 1 ??

proprietary Survey VSASVORION Logical flag indicating whether a survey is proprietary or not (1=yes; 0=no) tinyint 1 ??

proprietary Survey VSAUltraVISTA Logical flag indicating whether a survey is proprietary or not (1=yes; 0=no) tinyint 1 ??

proprietary Survey VSAVHS Logical flag indicating whether a survey is proprietary or not (1=yes; 0=no) tinyint 1 ??

proprietary Survey VSAVIDEO Logical flag indicating whether a survey is proprietary or not (1=yes; 0=no) tinyint 1 ??

proprietary Survey VSAVIKING Logical flag indicating whether a survey is proprietary or not (1=yes; 0=no) tinyint 1 ??

proprietary Survey VSAVMC Logical flag indicating whether a survey is proprietary or not (1=yes; 0=no) tinyint 1 ??

proprietary Survey VSAVVV 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 svNgc253Source VSASVNGC253 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:

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(class_k)=Π_iP(class_k)_i / Σ_kΠ_iP(class_k)_i
where class_k is one of star|galaxy|noise|saturated, and i denotes the i^th 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.

pSaturated svOrionSource VSASVORION 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:

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(class_k)=Π_iP(class_k)_i / Σ_kΠ_iP(class_k)_i
where class_k is one of star|galaxy|noise|saturated, and i denotes the i^th 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.

pSaturated ultravistaSource VSAUltraVISTA 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:

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(class_k)=Π_iP(class_k)_i / Σ_kΠ_iP(class_k)_i
where class_k is one of star|galaxy|noise|saturated, and i denotes the i^th 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.

pSaturated ultravistaSource, vhsSource, videoSource, vikingSource, vmcSource, vmcSynopticSource, vvvSource VSAQC 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:

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(class_k)=Π_iP(class_k)_i / Σ_kΠ_iP(class_k)_i
where class_k is one of star|galaxy|noise|saturated, and i denotes the i^th 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 svNgc253Detection VSASVNGC253 standard normalised variance of PSF fit {catalogue TType keyword: PSF_fit_chi2} real 4 -0.9999995e9 FIT_STDEV

psfFitChi2 svOrionDetection VSASVORION standard normalised variance of PSF fit {catalogue TType keyword: PSF_fit_chi2} real 4 -0.9999995e9 FIT_STDEV

psfFitChi2 ultravistaDetection VSAUltraVISTA Not available in SE output {catalogue TType keyword: PSF_fit_chi2} real 4 -0.9999995e9

psfFitChi2 ultravistaDetection, videoDetection VSAQC Not available in SE output {catalogue TType keyword: PSF_fit_chi2} real 4 -0.9999995e9

psfFitChi2 ultravistaListRemeasurement VSAUltraVISTA standard normalised variance of PSF fit {catalogue TType keyword: PSF_fit_chi2} real 4 -0.9999995e9 FIT_STDEV

psfFitChi2 ultravistaListRemeasurement, vhsDetection, vhsListRemeasurement, videoListRemeasurement, vikingDetection, vikingListRemeasurement, vmcDetection, vmcListRemeasurement, vvvDetection, vvvListRemeasurement VSAQC standard normalised variance of PSF fit {catalogue TType keyword: PSF_fit_chi2} real 4 -0.9999995e9 FIT_STDEV

psfFitDof svNgc253Detection VSASVNGC253 no. of degrees of freedom of PSF fit {catalogue TType keyword: PSF_fit_dof} smallint 2 -9999 STAT_N-DOF

psfFitDof svOrionDetection VSASVORION no. of degrees of freedom of PSF fit {catalogue TType keyword: PSF_fit_dof} smallint 2 -9999 STAT_N-DOF

psfFitDof ultravistaDetection VSAUltraVISTA Not available in SE output {catalogue TType keyword: PSF_fit_dof} smallint 2 -9999

psfFitDof ultravistaDetection, videoDetection VSAQC Not available in SE output {catalogue TType keyword: PSF_fit_dof} smallint 2 -9999

psfFitDof ultravistaListRemeasurement VSAUltraVISTA no. of degrees of freedom of PSF fit {catalogue TType keyword: PSF_fit_dof} smallint 2 -9999 STAT_N-DOF

psfFitDof ultravistaListRemeasurement, vhsDetection, vhsListRemeasurement, videoListRemeasurement, vikingDetection, vikingListRemeasurement, vmcDetection, vmcListRemeasurement, vvvDetection, vvvListRemeasurement VSAQC no. of degrees of freedom of PSF fit {catalogue TType keyword: PSF_fit_dof} smallint 2 -9999 STAT_N-DOF

psfFitX svNgc253Detection VSASVNGC253 PSF-fitted X coordinate {catalogue TType keyword: PSF_fit_X} real 4 pixels -0.9999995e9 POS_PLATE_X

psfFitX svOrionDetection VSASVORION PSF-fitted X coordinate {catalogue TType keyword: PSF_fit_X} real 4 pixels -0.9999995e9 POS_PLATE_X

psfFitX ultravistaDetection VSAUltraVISTA Not available in SE output {catalogue TType keyword: PSF_fit_X} real 4 -0.9999995e9

psfFitX ultravistaDetection, videoDetection VSAQC Not available in SE output {catalogue TType keyword: PSF_fit_X} real 4 -0.9999995e9

psfFitX ultravistaListRemeasurement VSAUltraVISTA PSF-fitted X coordinate {catalogue TType keyword: PSF_fit_X} real 4 pixels -0.9999995e9 POS_PLATE_X

psfFitX ultravistaListRemeasurement, vhsDetection, vhsListRemeasurement, videoListRemeasurement, vikingDetection, vikingListRemeasurement, vmcDetection, vmcListRemeasurement, vvvDetection, vvvListRemeasurement VSAQC PSF-fitted X coordinate {catalogue TType keyword: PSF_fit_X} real 4 pixels -0.9999995e9 POS_PLATE_X

psfFitXerr svNgc253Detection VSASVNGC253 Error on PSF-fitted X coordinate {catalogue TType keyword: PSF_fit_X_err} real 4 pixels -0.9999995e9 ERROR

psfFitXerr svOrionDetection VSASVORION Error on PSF-fitted X coordinate {catalogue TType keyword: PSF_fit_X_err} real 4 pixels -0.9999995e9 ERROR

psfFitXerr ultravistaDetection VSAUltraVISTA Not available in SE output {catalogue TType keyword: PSF_fit_X_err} real 4 -0.9999995e9

psfFitXerr ultravistaDetection, videoDetection VSAQC Not available in SE output {catalogue TType keyword: PSF_fit_X_err} real 4 -0.9999995e9

psfFitXerr ultravistaListRemeasurement VSAUltraVISTA Error on PSF-fitted X coordinate {catalogue TType keyword: PSF_fit_X_err} real 4 pixels -0.9999995e9 ERROR

psfFitXerr ultravistaListRemeasurement, vhsDetection, vhsListRemeasurement, videoListRemeasurement, vikingDetection, vikingListRemeasurement, vmcDetection, vmcListRemeasurement, vvvDetection, vvvListRemeasurement VSAQC Error on PSF-fitted X coordinate {catalogue TType keyword: PSF_fit_X_err} real 4 pixels -0.9999995e9 ERROR

psfFitY svNgc253Detection VSASVNGC253 PSF-fitted Y coordinate {catalogue TType keyword: PSF_fit_Y} real 4 pixels -0.9999995e9 POS_PLATE_Y

psfFitY svOrionDetection VSASVORION PSF-fitted Y coordinate {catalogue TType keyword: PSF_fit_Y} real 4 pixels -0.9999995e9 POS_PLATE_Y

psfFitY ultravistaDetection VSAUltraVISTA Not available in SE output {catalogue TType keyword: PSF_fit_Y} real 4 -0.9999995e9

psfFitY ultravistaDetection, videoDetection VSAQC Not available in SE output {catalogue TType keyword: PSF_fit_Y} real 4 -0.9999995e9

psfFitY ultravistaListRemeasurement VSAUltraVISTA PSF-fitted Y coordinate {catalogue TType keyword: PSF_fit_Y} real 4 pixels -0.9999995e9 POS_PLATE_Y

psfFitY ultravistaListRemeasurement, vhsDetection, vhsListRemeasurement, videoListRemeasurement, vikingDetection, vikingListRemeasurement, vmcDetection, vmcListRemeasurement, vvvDetection, vvvListRemeasurement VSAQC PSF-fitted Y coordinate {catalogue TType keyword: PSF_fit_Y} real 4 pixels -0.9999995e9 POS_PLATE_Y

psfFitYerr svNgc253Detection VSASVNGC253 Error on PSF-fitted Y coordinate {catalogue TType keyword: PSF_fit_y_err} real 4 pixels -0.9999995e9 ERROR

psfFitYerr svOrionDetection VSASVORION Error on PSF-fitted Y coordinate {catalogue TType keyword: PSF_fit_y_err} real 4 pixels -0.9999995e9 ERROR

psfFitYerr ultravistaDetection VSAUltraVISTA Not available in SE output {catalogue TType keyword: PSF_fit_y_err} real 4 -0.9999995e9

psfFitYerr ultravistaDetection, videoDetection VSAQC Not available in SE output {catalogue TType keyword: PSF_fit_y_err} real 4 -0.9999995e9

psfFitYerr ultravistaListRemeasurement VSAUltraVISTA Error on PSF-fitted Y coordinate {catalogue TType keyword: PSF_fit_y_err} real 4 pixels -0.9999995e9 ERROR

psfFitYerr ultravistaListRemeasurement, vhsDetection, vhsListRemeasurement, videoListRemeasurement, vikingDetection, vikingListRemeasurement, vmcDetection, vmcListRemeasurement, vvvDetection, vvvListRemeasurement VSAQC Error on PSF-fitted Y coordinate {catalogue TType keyword: PSF_fit_y_err} real 4 pixels -0.9999995e9 ERROR

psfFlux svNgc253Detection VSASVNGC253 PSF-fitted flux {catalogue TType keyword: PSF_flux} real 4 ADU -0.9999995e9 PHOT_INTENSITY_ADU

psfFlux svOrionDetection VSASVORION PSF-fitted flux {catalogue TType keyword: PSF_flux} real 4 ADU -0.9999995e9 PHOT_INTENSITY_ADU

psfFlux ultravistaDetection VSAUltraVISTA Not available in SE output {catalogue TType keyword: PSF_flux} real 4 -0.9999995e9

psfFlux ultravistaDetection, videoDetection VSAQC Not available in SE output {catalogue TType keyword: PSF_flux} real 4 -0.9999995e9

psfFlux ultravistaListRemeasurement VSAUltraVISTA PSF-fitted flux {catalogue TType keyword: PSF_flux} real 4 ADU -0.9999995e9 PHOT_INTENSITY_ADU

psfFlux ultravistaListRemeasurement, vhsDetection, vhsListRemeasurement, videoListRemeasurement, vikingDetection, vikingListRemeasurement, vmcDetection, vmcListRemeasurement, vvvDetection, vvvListRemeasurement VSAQC PSF-fitted flux {catalogue TType keyword: PSF_flux} real 4 ADU -0.9999995e9 PHOT_INTENSITY_ADU

psfFluxErr svNgc253Detection VSASVNGC253 Error on PSF-fitted flux {catalogue TType keyword: PSF_flux_err} real 4 ADU -0.9999995e9 ERROR

psfFluxErr svOrionDetection VSASVORION Error on PSF-fitted flux {catalogue TType keyword: PSF_flux_err} real 4 ADU -0.9999995e9 ERROR

psfFluxErr ultravistaDetection VSAUltraVISTA Not available in SE output {catalogue TType keyword: PSF_flux_err} real 4 -0.9999995e9

psfFluxErr ultravistaDetection, videoDetection VSAQC Not available in SE output {catalogue TType keyword: PSF_flux_err} real 4 -0.9999995e9

psfFluxErr ultravistaListRemeasurement VSAUltraVISTA Error on PSF-fitted flux {catalogue TType keyword: PSF_flux_err} real 4 ADU -0.9999995e9 ERROR

psfFluxErr ultravistaListRemeasurement, vhsDetection, vhsListRemeasurement, videoListRemeasurement, vikingDetection, vikingListRemeasurement, vmcDetection, vmcListRemeasurement, vvvDetection, vvvListRemeasurement VSAQC Error on PSF-fitted flux {catalogue TType keyword: PSF_flux_err} real 4 ADU -0.9999995e9 ERROR

psfMag svNgc253Detection VSASVNGC253 PSF-fitted calibrated magnitude real 4 mag -0.9999995e9 PHOT_PROFILE

psfMag svOrionDetection VSASVORION PSF-fitted calibrated magnitude real 4 mag -0.9999995e9 PHOT_PROFILE

psfMag ultravistaDetection VSAUltraVISTA Not available in SE output real 4 -0.9999995e9

psfMag ultravistaDetection, videoDetection VSAQC Not available in SE output real 4 -0.9999995e9

psfMag ultravistaListRemeasurement VSAUltraVISTA PSF-fitted calibrated magnitude real 4 mag -0.9999995e9 PHOT_PROFILE

psfMag ultravistaListRemeasurement, vhsDetection, vhsListRemeasurement, videoListRemeasurement, vikingDetection, vikingListRemeasurement, vmcDetection, vmcListRemeasurement, vvvDetection, vvvListRemeasurement VSAQC PSF-fitted calibrated magnitude real 4 mag -0.9999995e9 PHOT_PROFILE

psfMagErr svNgc253Detection VSASVNGC253 Error on PSF-fitted calibrated magnitude real 4 mag -0.9999995e9 ERROR

psfMagErr svOrionDetection VSASVORION Error on PSF-fitted calibrated magnitude real 4 mag -0.9999995e9 ERROR

psfMagErr ultravistaDetection VSAUltraVISTA Not available in SE output real 4 -0.9999995e9

psfMagErr ultravistaDetection, videoDetection VSAQC Not available in SE output real 4 -0.9999995e9

psfMagErr ultravistaListRemeasurement VSAUltraVISTA Error on PSF-fitted calibrated magnitude real 4 mag -0.9999995e9 ERROR

psfMagErr ultravistaListRemeasurement, vhsDetection, vhsListRemeasurement, videoListRemeasurement, vikingDetection, vikingListRemeasurement, vmcDetection, vmcListRemeasurement, vvvDetection, vvvListRemeasurement VSAQC Error on PSF-fitted calibrated magnitude real 4 mag -0.9999995e9 ERROR

pStar svNgc253Source VSASVNGC253 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:

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(class_k)=Π_iP(class_k)_i / Σ_kΠ_iP(class_k)_i
where class_k is one of star|galaxy|noise|saturated, and i denotes the i^th 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.

pStar svOrionSource VSASVORION 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:

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(class_k)=Π_iP(class_k)_i / Σ_kΠ_iP(class_k)_i
where class_k is one of star|galaxy|noise|saturated, and i denotes the i^th 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.

pStar ultravistaSource VSAUltraVISTA 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:

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(class_k)=Π_iP(class_k)_i / Σ_kΠ_iP(class_k)_i
where class_k is one of star|galaxy|noise|saturated, and i denotes the i^th 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.

pStar ultravistaSource, vhsSource, videoSource, vikingSource, vmcSource, vmcSynopticSource, vvvSource VSAQC 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:

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(class_k)=Π_iP(class_k)_i / Σ_kΠ_iP(class_k)_i
where class_k is one of star|galaxy|noise|saturated, and i denotes the i^th 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 VSASVNGC253 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

pv21 CurrentAstrometry VSASVORION 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

pv21 CurrentAstrometry VSAUltraVISTA 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

pv21 CurrentAstrometry VSAVHS 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

pv21 CurrentAstrometry VSAVIDEO 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

pv21 CurrentAstrometry VSAVIKING 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

pv21 CurrentAstrometry VSAVMC 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

pv21 CurrentAstrometry VSAVVV 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

pv21 ultravistaCurrentAstrometry, vhsCurrentAstrometry, videoCurrentAstrometry, vikingCurrentAstrometry, vmcCurrentAstrometry, vvvCurrentAstrometry VSAQC Coefficient for r term (use only with ZPN projection) float 8 -0.9999995e9 POS_TRANSF_PARAM

pv22 CurrentAstrometry VSASVNGC253 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

pv22 CurrentAstrometry VSASVORION 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

pv22 CurrentAstrometry VSAUltraVISTA 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

pv22 CurrentAstrometry VSAVHS 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

pv22 CurrentAstrometry VSAVIDEO 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

pv22 CurrentAstrometry VSAVIKING 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

pv22 CurrentAstrometry VSAVMC 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

pv22 CurrentAstrometry VSAVVV 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

pv22 ultravistaCurrentAstrometry, vhsCurrentAstrometry, videoCurrentAstrometry, vikingCurrentAstrometry, vmcCurrentAstrometry, vvvCurrentAstrometry VSAQC Coefficient for r**2 term (use only with ZPN projection) float 8 -0.9999995e9 POS_TRANSF_PARAM

pv23 CurrentAstrometry VSASVNGC253 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

pv23 CurrentAstrometry VSASVORION 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

pv23 CurrentAstrometry VSAUltraVISTA 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

pv23 CurrentAstrometry VSAVHS 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

pv23 CurrentAstrometry VSAVIDEO 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

pv23 CurrentAstrometry VSAVIKING 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

pv23 CurrentAstrometry VSAVMC 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

pv23 CurrentAstrometry VSAVVV 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

pv23 ultravistaCurrentAstrometry, vhsCurrentAstrometry, videoCurrentAstrometry, vikingCurrentAstrometry, vmcCurrentAstrometry, vvvCurrentAstrometry VSAQC Coefficient for r**3 term (use only with ZPN projection) float 8 -0.9999995e9 POS_TRANSF_PARAM

pv24 CurrentAstrometry VSASVNGC253 Coefficient for r**4 term (use only with ZPN projection) {image extension keyword: PV2_4}
transformation from pixel to celestial co-ordinates float 8 -0.9999995e9 POS_TRANSF_PARAM

pv24 CurrentAstrometry VSASVORION Coefficient for r**4 term (use only with ZPN projection) {image extension keyword: PV2_4}
transformation from pixel to celestial co-ordinates float 8 -0.9999995e9 POS_TRANSF_PARAM

pv24 CurrentAstrometry VSAUltraVISTA Coefficient for r**4 term (use only with ZPN projection) {image extension keyword: PV2_4}
transformation from pixel to celestial co-ordinates float 8 -0.9999995e9 POS_TRANSF_PARAM

pv24 CurrentAstrometry VSAVHS Coefficient for r**4 term (use only with ZPN projection) {image extension keyword: PV2_4}
transformation from pixel to celestial co-ordinates float 8 -0.9999995e9 POS_TRANSF_PARAM

pv24 CurrentAstrometry VSAVIDEO Coefficient for r**4 term (use only with ZPN projection) {image extension keyword: PV2_4}
transformation from pixel to celestial co-ordinates float 8 -0.9999995e9 POS_TRANSF_PARAM

pv24 CurrentAstrometry VSAVIKING Coefficient for r**4 term (use only with ZPN projection) {image extension keyword: PV2_4}
transformation from pixel to celestial co-ordinates float 8 -0.9999995e9 POS_TRANSF_PARAM

pv24 CurrentAstrometry VSAVMC Coefficient for r**4 term (use only with ZPN projection) {image extension keyword: PV2_4}
transformation from pixel to celestial co-ordinates float 8 -0.9999995e9 POS_TRANSF_PARAM

pv24 CurrentAstrometry VSAVVV Coefficient for r**4 term (use only with ZPN projection) {image extension keyword: PV2_4}
transformation from pixel to celestial co-ordinates float 8 -0.9999995e9 POS_TRANSF_PARAM

pv24 ultravistaCurrentAstrometry, vhsCurrentAstrometry, videoCurrentAstrometry, vikingCurrentAstrometry, vmcCurrentAstrometry, vvvCurrentAstrometry VSAQC Coefficient for r**4 term (use only with ZPN projection) float 8 -0.9999995e9 POS_TRANSF_PARAM

pv25 CurrentAstrometry VSASVNGC253 Coefficient for r**5 term (use only with ZPN projection) {image extension keyword: PV2_5}
transformation from pixel to celestial co-ordinates float 8 -0.9999995e9 POS_TRANSF_PARAM

pv25 CurrentAstrometry VSASVORION Coefficient for r**5 term (use only with ZPN projection) {image extension keyword: PV2_5}
transformation from pixel to celestial co-ordinates float 8 -0.9999995e9 POS_TRANSF_PARAM

pv25 CurrentAstrometry VSAUltraVISTA Coefficient for r**5 term (use only with ZPN projection) {image extension keyword: PV2_5}
transformation from pixel to celestial co-ordinates float 8 -0.9999995e9 POS_TRANSF_PARAM

pv25 CurrentAstrometry VSAVHS Coefficient for r**5 term (use only with ZPN projection) {image extension keyword: PV2_5}
transformation from pixel to celestial co-ordinates float 8 -0.9999995e9 POS_TRANSF_PARAM

pv25 CurrentAstrometry VSAVIDEO Coefficient for r**5 term (use only with ZPN projection) {image extension keyword: PV2_5}
transformation from pixel to celestial co-ordinates float 8 -0.9999995e9 POS_TRANSF_PARAM

pv25 CurrentAstrometry VSAVIKING Coefficient for r**5 term (use only with ZPN projection) {image extension keyword: PV2_5}
transformation from pixel to celestial co-ordinates float 8 -0.9999995e9 POS_TRANSF_PARAM

pv25 CurrentAstrometry VSAVMC Coefficient for r**5 term (use only with ZPN projection) {image extension keyword: PV2_5}
transformation from pixel to celestial co-ordinates float 8 -0.9999995e9 POS_TRANSF_PARAM

pv25 CurrentAstrometry VSAVVV Coefficient for r**5 term (use only with ZPN projection) {image extension keyword: PV2_5}
transformation from pixel to celestial co-ordinates float 8 -0.9999995e9 POS_TRANSF_PARAM

pv25 ultravistaCurrentAstrometry, vhsCurrentAstrometry, videoCurrentAstrometry, vikingCurrentAstrometry, vmcCurrentAstrometry, vvvCurrentAstrometry VSAQC Coefficient for r**5 term (use only with ZPN projection) 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

WFAU, Institute for Astronomy,
Royal Observatory, Blackford Hill
Edinburgh, EH9 3HJ, UK
Tel +44 131 668 8356 (office)
or +44 131 668 8100 (switchboard)

vsa-support@roe.ac.uk
21/02/2011