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Glossary of WSA attributes

This Glossary alphabetically lists all attributes used in the UKIDSSDR7 database(s) held in the WSA. If you would like to have more information about the schema tables please use the UKIDSSDR7 Schema Browser (other Browser versions).
A B C D E F G H I J K L M
N O P Q R S T U V W X Y Z

M

NameSchema TableDatabaseDescriptionTypeLengthUnitDefault ValueUnified Content Descriptor
M1 glimpse_hrc_inter, glimpse_mca_inter GLIMPSE Number of detections for band 1 int 4   -9  
M1_1_BG twoxmm XMM The M1 band 1 background map.
Made using a 12 x 12 nodes spline fit on the source-free individual-band images.		 real 4 counts/pixel    
M1_1_DET_ML twoxmm XMM M1 band 1 Maximum likelihood real 4      
M1_1_EXP twoxmm XMM The M1 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    
M1_1_FLUX twoxmm XMM M1 band 1 flux real 4 erg/cm**2/s    
M1_1_FLUX_ERR twoxmm XMM M1 band 1 flux error real 4 erg/cm**2/s    
M1_1_RATE twoxmm XMM M1 band 1 Count rates real 4 counts/s    
M1_1_RATE_ERR twoxmm XMM M1 band 1 Count rates error real 4 counts/s    
M1_1_VIG twoxmm XMM The M1 band 1 vignetting value. real 4      
M1_2_BG twoxmm XMM The M1 band 2 background map.
Made using a 12 x 12 nodes spline fit on the source-free individual-band images.		 real 4 counts/pixel    
M1_2_DET_ML twoxmm XMM M1 band 2 Maximum likelihood real 4      
M1_2_EXP twoxmm XMM The M1 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    
M1_2_FLUX twoxmm XMM M1 band 2 flux real 4 erg/cm**2/s    
M1_2_FLUX_ERR twoxmm XMM M1 band 2 flux error real 4 erg/cm**2/s    
M1_2_RATE twoxmm XMM M1 band 2 Count rates real 4 counts/s    
M1_2_RATE_ERR twoxmm XMM M1 band 2 Count rates error real 4 counts/s    
M1_2_VIG twoxmm XMM The M1 band 2 vignetting value. real 4      
M1_3_BG twoxmm XMM The M1 band 3 background map.
Made using a 12 x 12 nodes spline fit on the source-free individual-band images.		 real 4 counts/pixel    
M1_3_DET_ML twoxmm XMM M1 band 3 Maximum likelihood real 4      
M1_3_EXP twoxmm XMM The M1 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    
M1_3_FLUX twoxmm XMM M1 band 3 flux real 4 erg/cm**2/s    
M1_3_FLUX_ERR twoxmm XMM M1 band 3 flux error real 4 erg/cm**2/s    
M1_3_RATE twoxmm XMM M1 band 3 Count rates real 4 counts/s    
M1_3_RATE_ERR twoxmm XMM M1 band 3 Count rates error real 4 counts/s    
M1_3_VIG twoxmm XMM The M1 band 3 vignetting value. real 4      
M1_4_BG twoxmm XMM The M1 band 4 background map.
Made using a 12 x 12 nodes spline fit on the source-free individual-band images.		 real 4 counts/pixel    
M1_4_DET_ML twoxmm XMM M1 band 4 Maximum likelihood real 4      
M1_4_EXP twoxmm XMM The M1 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    
M1_4_FLUX twoxmm XMM M1 band 4 flux real 4 erg/cm**2/s    
M1_4_FLUX_ERR twoxmm XMM M1 band 4 flux error real 4 erg/cm**2/s    
M1_4_RATE twoxmm XMM M1 band 4 Count rates real 4 counts/s    
M1_4_RATE_ERR twoxmm XMM M1 band 4 Count rates error real 4 counts/s    
M1_4_VIG twoxmm XMM The M1 band 4 vignetting value. real 4      
M1_5_BG twoxmm XMM The M1 band 5 background map.
Made using a 12 x 12 nodes spline fit on the source-free individual-band images.		 real 4 counts/pixel    
M1_5_DET_ML twoxmm XMM M1 band 5 Maximum likelihood real 4      
M1_5_EXP twoxmm XMM The M1 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    
M1_5_FLUX twoxmm XMM M1 band 5 flux real 4 erg/cm**2/s    
M1_5_FLUX_ERR twoxmm XMM M1 band 5 flux error real 4 erg/cm**2/s    
M1_5_RATE twoxmm XMM M1 band 5 Count rates real 4 counts/s    
M1_5_RATE_ERR twoxmm XMM M1 band 5 Count rates error real 4 counts/s    
M1_5_VIG twoxmm XMM The M1 band 5 vignetting value. real 4      
M1_8_CTS twoxmm XMM Combined band source counts real 4 counts    
M1_8_CTS_ERR twoxmm XMM Combined band source counts 1 σ error real 4 counts    
M1_8_DET_ML twoxmm XMM M1 band 8 Maximum likelihood real 4      
M1_8_FLUX twoxmm XMM M1 band 8 flux real 4 erg/cm**2/s    
M1_8_FLUX_ERR twoxmm XMM M1 band 8 flux error real 4 erg/cm**2/s    
M1_8_RATE twoxmm XMM M1 band 8 Count rates real 4 counts/s    
M1_8_RATE_ERR twoxmm XMM M1 band 8 Count rates error real 4 counts/s    
M1_9_DET_ML twoxmm XMM M1 band 9 Maximum likelihood real 4      
M1_9_FLUX twoxmm XMM M1 band 9 flux real 4 erg/cm**2/s    
M1_9_FLUX_ERR twoxmm XMM M1 band 9 flux error real 4 erg/cm**2/s    
M1_9_RATE twoxmm XMM M1 band 9 Count rates real 4 counts/s    
M1_9_RATE_ERR twoxmm XMM M1 band 9 Count rates error real 4 counts/s    
M1_CHI2PROB twoxmm XMM The Chi² probability (based on the null hypothesis) that the source as detected by the M1 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      
M1_FILTER twoxmm XMM M1 filter. The options are Thick, Medium, Thin1, and Open, depending on the efficiency of the optical blocking. varchar 6      
M1_FLAG twoxmm XMM M1 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 M1 the flags are all set to False (default). Flag 10 is not used.		 varchar 12      
M1_HR1 twoxmm XMM The M1 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      
M1_HR1_ERR twoxmm XMM The 1 σ error of the M1 hardness ratio between the bands 1 & 2 real 4      
M1_HR2 twoxmm XMM The M1 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      
M1_HR2_ERR twoxmm XMM The 1 σ error of the M1 hardness ratio between the bands 2 & 3 real 4      
M1_HR3 twoxmm XMM The M1 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      
M1_HR3_ERR twoxmm XMM The 1 σ error of the M1 hardness ratio between the bands 3 & 4 real 4      
M1_HR4 twoxmm XMM The M1 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      
M1_HR4_ERR twoxmm XMM The 1 σ error of the M1 hardness ratio between the bands 4 & 5 real 4      
M1_MASKFRAC twoxmm 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      
M1_OFFAX twoxmm XMM The M1 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    
M1_ONTIME twoxmm XMM The M1 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    
M1_SUBMODE twoxmm XMM M1 observing mode. The options are full frame mode with the full FOV exposed, partial window mode with only parts of the central CCD exposed (in different sub-modes), and timing mode where the central CCD was not exposed ('Fast Uncompressed'). varchar 16      
M2 glimpse_hrc_inter, glimpse_mca_inter GLIMPSE Number of detections for band 2 int 4   -9  
M2_1_BG twoxmm XMM The M2 band 1 background map.
Made using a 12 x 12 nodes spline fit on the source-free individual-band images.		 real 4 counts/pixel    
M2_1_DET_ML twoxmm XMM M2 band 1 Maximum likelihood real 4      
M2_1_EXP twoxmm XMM The M2 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    
M2_1_FLUX twoxmm XMM M2 band 1 flux real 4 erg/cm**2/s    
M2_1_FLUX_ERR twoxmm XMM M2 band 1 flux error real 4 erg/cm**2/s    
M2_1_RATE twoxmm XMM M2 band 1 Count rates real 4 counts/s    
M2_1_RATE_ERR twoxmm XMM M2 band 1 Count rates error real 4 counts/s    
M2_1_VIG twoxmm XMM The M2 band 1 vignetting value. real 4      
M2_2_BG twoxmm XMM The M2 band 2 background map.
Made using a 12 x 12 nodes spline fit on the source-free individual-band images.		 real 4 counts/pixel    
M2_2_DET_ML twoxmm XMM M2 band 2 Maximum likelihood real 4      
M2_2_EXP twoxmm XMM The M2 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    
M2_2_FLUX twoxmm XMM M2 band 2 flux real 4 erg/cm**2/s    
M2_2_FLUX_ERR twoxmm XMM M2 band 2 flux error real 4 erg/cm**2/s    
M2_2_RATE twoxmm XMM M2 band 2 Count rates real 4 counts/s    
M2_2_RATE_ERR twoxmm XMM M2 band 2 Count rates error real 4 counts/s    
M2_2_VIG twoxmm XMM The M2 band 2 vignetting value. real 4      
M2_3_BG twoxmm XMM The M2 band 3 background map.
Made using a 12 x 12 nodes spline fit on the source-free individual-band images.		 real 4 counts/pixel    
M2_3_DET_ML twoxmm XMM M2 band 3 Maximum likelihood real 4      
M2_3_EXP twoxmm XMM The M2 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    
M2_3_FLUX twoxmm XMM M2 band 3 flux real 4 erg/cm**2/s    
M2_3_FLUX_ERR twoxmm XMM M2 band 3 flux error real 4 erg/cm**2/s    
M2_3_RATE twoxmm XMM M2 band 3 Count rates real 4 counts/s    
M2_3_RATE_ERR twoxmm XMM M2 band 3 Count rates error real 4 counts/s    
M2_3_VIG twoxmm XMM The M2 band 3 vignetting value. real 4      
M2_4_BG twoxmm XMM The M2 band 4 background map.
Made using a 12 x 12 nodes spline fit on the source-free individual-band images.		 real 4 counts/pixel    
M2_4_DET_ML twoxmm XMM M2 band 4 Maximum likelihood real 4      
M2_4_EXP twoxmm XMM The M2 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    
M2_4_FLUX twoxmm XMM M2 band 4 flux real 4 erg/cm**2/s    
M2_4_FLUX_ERR twoxmm XMM M2 band 4 flux error real 4 erg/cm**2/s    
M2_4_RATE twoxmm XMM M2 band 4 Count rates real 4 counts/s    
M2_4_RATE_ERR twoxmm XMM M2 band 4 Count rates error real 4 counts/s    
M2_4_VIG twoxmm XMM The M2 band 4 vignetting value. real 4      
M2_5_BG twoxmm XMM The M2 band 5 background map.
Made using a 12 x 12 nodes spline fit on the source-free individual-band images.		 real 4 counts/pixel    
M2_5_DET_ML twoxmm XMM M2 band 5 Maximum likelihood real 4      
M2_5_EXP twoxmm XMM The M2 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    
M2_5_FLUX twoxmm XMM M2 band 5 flux real 4 erg/cm**2/s    
M2_5_FLUX_ERR twoxmm XMM M2 band 5 flux error real 4 erg/cm**2/s    
M2_5_RATE twoxmm XMM M2 band 5 Count rates real 4 counts/s    
M2_5_RATE_ERR twoxmm XMM M2 band 5 Count rates error real 4 counts/s    
M2_5_VIG twoxmm XMM The M2 band 5 vignetting value. real 4      
M2_8_CTS twoxmm XMM Combined band source counts real 4 counts    
M2_8_CTS_ERR twoxmm XMM Combined band source counts 1 σ error real 4 counts    
M2_8_DET_ML twoxmm XMM M2 band 8 Maximum likelihood real 4      
M2_8_FLUX twoxmm XMM M2 band 8 flux real 4 erg/cm**2/s    
M2_8_FLUX_ERR twoxmm XMM M2 band 8 flux error real 4 erg/cm**2/s    
M2_8_RATE twoxmm XMM M2 band 8 Count rates real 4 counts/s    
M2_8_RATE_ERR twoxmm XMM M2 band 8 Count rates error real 4 counts/s    
M2_9_DET_ML twoxmm XMM M2 band 9 Maximum likelihood real 4      
M2_9_FLUX twoxmm XMM M2 band 9 flux real 4 erg/cm**2/s    
M2_9_FLUX_ERR twoxmm XMM M2 band 9 flux error real 4 erg/cm**2/s    
M2_9_RATE twoxmm XMM M2 band 9 Count rates real 4 counts/s    
M2_9_RATE_ERR twoxmm XMM M2 band 9 Count rates error real 4 counts/s    
M2_CHI2PROB twoxmm XMM The Chi² probability (based on the null hypothesis) that the source as detected by the M2 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      
M2_FILTER twoxmm XMM M2 filter. The options are Thick, Medium, Thin1, and Open, depending on the efficiency of the optical blocking. varchar 6      
M2_FLAG twoxmm XMM PN flag string made of the flags 1 - 12 (counted from left to right) for the M2 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 M2 the flags are all set to False (default). Flag 10 is not used.		 varchar 12      
M2_HR1 twoxmm XMM The M2 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      
M2_HR1_ERR twoxmm XMM The 1 σ error of the M2 hardness ratio between the bands 1 & 2 real 4      
M2_HR2 twoxmm XMM The M2 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      
M2_HR2_ERR twoxmm XMM The 1 σ error of the M2 hardness ratio between the bands 2 & 3 real 4      
M2_HR3 twoxmm XMM The M2 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      
M2_HR3_ERR twoxmm XMM The 1 σ error of the M2 hardness ratio between the bands 3 & 4 real 4      
M2_HR4 twoxmm XMM The M2 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      
M2_HR4_ERR twoxmm XMM The 1 σ error of the M2 hardness ratio between the bands 4 & 5 real 4      
M2_MASKFRAC twoxmm 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      
M2_OFFAX twoxmm XMM The M2 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    
M2_ONTIME twoxmm XMM The M2 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    
M2_SUBMODE twoxmm XMM M2 observing mode. The options are full frame mode with the full FOV exposed, partial window mode with only parts of the central CCD exposed (in different sub-modes), and timing mode where the central CCD was not exposed ('Fast Uncompressed'). varchar 16      
m2u Multiframe WSA Raw position of M2 U (N-S tilt) {image primary HDU keyword: M2_U} real 4 mrad -0.9999995e9  
m2u Multiframe WSACalib Raw position of M2 U (N-S tilt) {image primary HDU keyword: M2_U} real 4 mrad -0.9999995e9  
m2u Multiframe WSATransit Raw position of M2 U (N-S tilt) {image primary HDU keyword: M2_U} real 4 mrad -0.9999995e9  
m2v Multiframe WSA Raw position of M2 V (E-W tilt) {image primary HDU keyword: M2_V} real 4 mrad -0.9999995e9  
m2v Multiframe WSACalib Raw position of M2 V (E-W tilt) {image primary HDU keyword: M2_V} real 4 mrad -0.9999995e9  
m2v Multiframe WSATransit Raw position of M2 V (E-W tilt) {image primary HDU keyword: M2_V} real 4 mrad -0.9999995e9  
m2w Multiframe WSA Raw position of M2 W (axial rotation) {image primary HDU keyword: M2_W} real 4 mrad -0.9999995e9  
m2w Multiframe WSACalib Raw position of M2 W (axial rotation) {image primary HDU keyword: M2_W} real 4 mrad -0.9999995e9  
m2w Multiframe WSATransit Raw position of M2 W (axial rotation) {image primary HDU keyword: M2_W} real 4 mrad -0.9999995e9  
m2x Multiframe WSA Raw position of M2 X (E-W) {image primary HDU keyword: M2_X} real 4 millimetres -0.9999995e9  
m2x Multiframe WSACalib Raw position of M2 X (E-W) {image primary HDU keyword: M2_X} real 4 millimetres -0.9999995e9  
m2x Multiframe WSATransit Raw position of M2 X (E-W) {image primary HDU keyword: M2_X} real 4 millimetres -0.9999995e9  
m2y Multiframe WSA Raw position of M2 Y (N-S) {image primary HDU keyword: M2_Y} real 4 millimetres -0.9999995e9  
m2y Multiframe WSACalib Raw position of M2 Y (N-S) {image primary HDU keyword: M2_Y} real 4 millimetres -0.9999995e9  
m2y Multiframe WSATransit Raw position of M2 Y (N-S) {image primary HDU keyword: M2_Y} real 4 millimetres -0.9999995e9  
m2z Multiframe WSA Raw position of M2 Z (focus) {image primary HDU keyword: M2_Z} real 4 millimetres -0.9999995e9  
m2z Multiframe WSACalib Raw position of M2 Z (focus) {image primary HDU keyword: M2_Z} real 4 millimetres -0.9999995e9  
m2z Multiframe WSATransit Raw position of M2 Z (focus) {image primary HDU keyword: M2_Z} real 4 millimetres -0.9999995e9  
M3 glimpse_hrc_inter, glimpse_mca_inter GLIMPSE Number of detections for band 3 int 4   -9  
M3_6 glimpse1_hrc, glimpse1_mca, glimpse2_hrc, glimpse2_mca GLIMPSE Number of detections for 3.6um IRAC (Band 1) int 4   -9  
M3Temp Multiframe WSA M3 temperature {image primary HDU keyword: M3_TEMP} real 4 degrees_Kelvin -0.9999995e9  
M3Temp Multiframe WSACalib M3 temperature {image primary HDU keyword: M3_TEMP} real 4 degrees_Kelvin -0.9999995e9  
M3Temp Multiframe WSATransit M3 temperature {image primary HDU keyword: M3_TEMP} real 4 degrees_Kelvin -0.9999995e9  
M4 glimpse_hrc_inter, glimpse_mca_inter GLIMPSE Number of detections for band 4 int 4   -9  
M4_5 glimpse1_hrc, glimpse1_mca, glimpse2_hrc, glimpse2_mca GLIMPSE Number of detections for 4.5um IRAC (Band 2) int 4   -9  
M5_8 glimpse1_hrc, glimpse1_mca, glimpse2_hrc, glimpse2_mca GLIMPSE Number of detections for 5.8um IRAC (Band 3) int 4   -9  
M8_0 glimpse1_hrc, glimpse1_mca, glimpse2_hrc, glimpse2_mca GLIMPSE Number of detections for 8.0um IRAC (Band 4) int 4   -9  
mag1 glimpse_hrc_inter, glimpse_mca_inter GLIMPSE Magnitude in IRAC band 1 real 4 mag 99.999  
mag1_err glimpse_hrc_inter, glimpse_mca_inter GLIMPSE 1sigma mag error (IRAC band 1) real 4 mag 99.999  
mag2 glimpse_hrc_inter, glimpse_mca_inter GLIMPSE Magnitude in IRAC band 2 real 4 mag 99.999  
mag2_err glimpse_hrc_inter, glimpse_mca_inter GLIMPSE 1sigma mag error (IRAC band 2) real 4 mag 99.999  
mag3 glimpse_hrc_inter, glimpse_mca_inter GLIMPSE Magnitude in IRAC band 3 real 4 mag 99.999  
mag3_6 glimpse1_hrc, glimpse1_mca, glimpse2_hrc, glimpse2_mca GLIMPSE 3.6um IRAC (Band 1) magnitude real 4 mag 99.999  
mag3_6_err glimpse1_hrc, glimpse1_mca, glimpse2_hrc, glimpse2_mca GLIMPSE 3.6um IRAC (Band 1) 1 sigma error real 4 mag 99.999  
mag3_err glimpse_hrc_inter, glimpse_mca_inter GLIMPSE 1sigma mag error (IRAC band 3) real 4 mag 99.999  
mag4 glimpse_hrc_inter, glimpse_mca_inter GLIMPSE Magnitude in IRAC band 4 real 4 mag 99.999  
mag4_5 glimpse1_hrc, glimpse1_mca, glimpse2_hrc, glimpse2_mca GLIMPSE 4.5um IRAC (Band 2) magnitude real 4 mag 99.999  
mag4_5_err glimpse1_hrc, glimpse1_mca, glimpse2_hrc, glimpse2_mca GLIMPSE 4.5um IRAC (Band 2) 1 sigma error real 4 mag 99.999  
mag4_err glimpse_hrc_inter, glimpse_mca_inter GLIMPSE 1sigma mag error (IRAC band 4) real 4 mag 99.999  
mag5_8 glimpse1_hrc, glimpse1_mca, glimpse2_hrc, glimpse2_mca GLIMPSE 5.8um IRAC (Band 3) magnitude real 4 mag 99.999  
mag5_8_err glimpse1_hrc, glimpse1_mca, glimpse2_hrc, glimpse2_mca GLIMPSE 5.8um IRAC (Band 3) 1 sigma error real 4 mag 99.999  
mag8_0 glimpse1_hrc, glimpse1_mca, glimpse2_hrc, glimpse2_mca GLIMPSE 8.0um IRAC (Band 4) magnitude real 4 mag 99.999  
mag8_0_err glimpse1_hrc, glimpse1_mca, glimpse2_hrc, glimpse2_mca GLIMPSE 8.0um IRAC (Band 4) 1 sigma error real 4 mag 99.999  
MAG_AUTO mgcDetection MGC Kron-like elliptical aperture magnitude real 4 mag    
MAG_AUTO_DC mgcDetection MGC MAG_AUTO corrected for extinction real 4 mag    
MAG_ERR mgcDetection MGC Error for B_MGC real 4 mag    
MAG_ISO mgcDetection MGC Isophotal magnitude real 4 mag    
MAG_ISO_DC mgcDetection MGC MAG_ISO corrected for extinction real 4 mag    
MAG_ISOCOR mgcDetection MGC Gaussian corrected isophotal magnitude real 4 mag    
MAG_ISOCOR_DC mgcDetection MGC MAG_ISOCOR corrected for extinction real 4 mag    
magH glimpse1_hrc, glimpse1_mca, glimpse2_hrc, glimpse2_mca GLIMPSE 2MASS All-Sky PSC H Band magnitude real 4 mag 99.999  
magH_err glimpse1_hrc, glimpse1_mca, glimpse2_hrc, glimpse2_mca GLIMPSE 2MASS All-Sky PSC H Band 1 sigma error real 4 mag 99.999  
magJ glimpse1_hrc, glimpse1_mca, glimpse2_hrc, glimpse2_mca GLIMPSE 2MASS All-Sky PSC J Band magnitude real 4 mag 99.999  
magJ_err glimpse1_hrc, glimpse1_mca, glimpse2_hrc, glimpse2_mca GLIMPSE 2MASS All-Sky PSC J Band 1 sigma error real 4 mag 99.999  
magK glimpse1_hrc, glimpse1_mca, glimpse2_hrc, glimpse2_mca GLIMPSE 2MASS All-Sky PSC Ks Band magnitude real 4 mag 99.999  
magKs_err glimpse1_hrc, glimpse1_mca, glimpse2_hrc, glimpse2_mca GLIMPSE 2MASS All-Sky PSC Ks Band 1 sigma error real 4 mag 99.999  
maj firstSource FIRST major axes derived from the elliptical Gaussian model for the source after deconvolution. real 4 arcsec   EXTENSION_FWHM_MAJ
majAxis nvssSource NVSS Fitted (deconvolved) major axis of radio source real 4 arcsec   EXTENSION_FWHM_MAJ
major iras_psc IRAS Uncertainty ellipse major axis smallint 2 arcsec   ERROR
maskID Multiframe WSA UID of library object mask frame {image extension keyword: CIR_OPM} bigint 8   -99999999 ID_FRAME
maskID Multiframe WSACalib UID of library object mask frame {image extension keyword: CIR_OPM} bigint 8   -99999999 ID_FRAME
maskID Multiframe WSATransit UID of library object mask frame {image extension keyword: CIR_OPM} bigint 8   -99999999 ID_FRAME
masterObjID calSourceNeighbours, calSourceXSynopticSource WSACalib The unique ID in calSource (=sourceID) bigint 8     ID_MAIN
masterObjID calSourceXtwomass_psc WSACalib The unique ID in calSource (=objID) bigint 8     ID_MAIN
masterObjID calSourceXukirtFSstars WSACalib The unique ID in calDetection (=objID) bigint 8     ID_MAIN
masterObjID dxsSourceNeighbours, dxsSourceXDR7PhotoObj, dxsSourceXDetection, dxsSourceXStripe82PhotoObjAll, dxsSourceXtwomass_psc, dxsSourceXtwoxmm WSA The unique ID in dxsSource (=sourceID) bigint 8     ID_MAIN
masterObjID gcsSourceNeighbours, gcsSourceXDR5PhotoObj, gcsSourceXDR7PhotoObj, gcsSourceXtwomass_psc, gcsSourceXtwoxmm WSA The unique ID in gcsSource (=sourceID) bigint 8     ID_MAIN
masterObjID lasSourceNeighbours, lasSourceXDR2PhotoObj, lasSourceXDR3PhotoObj, lasSourceXDR5PhotoObj, lasSourceXDR5PhotoObjAll, lasSourceXDR7PhotoObj, lasSourceXDR7PhotoObjAll, lasSourceXSegueDR6PhotoObj, lasSourceXSegueDR6PhotoObjAll, lasSourceXStripe82PhotoObjAll, lasSourceXfirstSource, lasSourceXiras_psc, lasSourceXmgcDetection, lasSourceXnvssSource, lasSourceXrosat_bsc, lasSourceXrosat_fsc, lasSourceXtwomass_psc, lasSourceXtwomass_xsc, lasSourceXtwoxmm WSA The unique ID in lasSource (=sourceID) bigint 8     ID_MAIN
MATCH_1XMM twoxmm XMM The IAU name of the 1XMM source ID matched within radius of 3 arcsec and using the closest candidate. varchar 21      
MATCH_2XMMP twoxmm XMM The IAU name of the 2XMMp source ID matched within radius of 3" and using the closest candidate. varchar 22      
maxDec CurrentAstrometry WSACalib The maximum Dec (J2000) on the device float 8 Degrees -0.9999995e9 POS_EQ_DEC_MAIN
maxDec CurrentAstrometry WSATransit The maximum Dec (J2000) on the device float 8 Degrees -0.9999995e9 POS_EQ_DEC_MAIN
maxDec CurrentAstrometry, PreviousAstrometry WSA The maximum Dec (J2000) on the device float 8 Degrees -0.9999995e9 POS_EQ_DEC_MAIN
maxPllx calVariability WSACalib Upper limit of 90% confidence interval for parallax measurement real 4 mas -0.9999995e9  
The Variability table contains statistics from the set of observations of each source. At present, the mean ra and dec and the error in two tangential directions are calculated. The "ra" direction is defined as tangential to both the radial direction and the cartesian z-axis and the "dec" direction is defined as both the radial direction and the "ra" direction. Since the current model is just the mean and standard deviation of the data, then the chi-squared of the fit=1. Data from good frames across all bands go into the astrometric model determination. This will include bands in non-synoptic filters: the one observation in these bands can help. In future releases a fit will be made to the rms data as a function of magnitude in each band, as has already happened for photometric data and a motion model that incorporates proper motion (and possibly parallax) will be used. The motion model is a parameter in the VarFrameSetInfo table.
maxPllx dxsVariability, udsVariability WSA Upper limit of 90% confidence interval for parallax measurement real 4 mas -0.9999995e9  
The Variability table contains statistics from the set of observations of each source. At present, the mean ra and dec and the error in two tangential directions are calculated. The "ra" direction is defined as tangential to both the radial direction and the cartesian z-axis and the "dec" direction is defined as both the radial direction and the "ra" direction. Since the current model is just the mean and standard deviation of the data, then the chi-squared of the fit=1. Data from good frames across all bands go into the astrometric model determination. This will include bands in non-synoptic filters: the one observation in these bands can help. In future releases a fit will be made to the rms data as a function of magnitude in each band, as has already happened for photometric data and a motion model that incorporates proper motion (and possibly parallax) will be used. The motion model is a parameter in the VarFrameSetInfo table.
maxRa CurrentAstrometry WSACalib The maximum RA (J2000) on the device float 8 Degrees -0.9999995e9 POS_EQ_RA_OTHER
maxRa CurrentAstrometry WSATransit The maximum RA (J2000) on the device float 8 Degrees -0.9999995e9 POS_EQ_RA_OTHER
maxRa CurrentAstrometry, PreviousAstrometry WSA The maximum RA (J2000) on the device float 8 Degrees -0.9999995e9 POS_EQ_RA_OTHER
maxSeeing RequiredMosaic WSACalib The maximum allowed seeing for intermediate stacks real 4 arcsec    
maxSeeing RequiredMosaic WSATransit The maximum allowed seeing for intermediate stacks real 4 arcsec    
maxSeeing RequiredMosaic, RequiredStack WSA The maximum allowed seeing for intermediate stacks real 4 arcsec    
maxStelEll RequiredMosaic WSACalib The maximum allowed stellar ellipticity for intermediate stacks real 4      
maxStelEll RequiredMosaic WSATransit The maximum allowed stellar ellipticity for intermediate stacks real 4      
maxStelEll RequiredMosaic, RequiredStack WSA The maximum allowed stellar ellipticity for intermediate stacks real 4      
meanMjdObs calSynopticMergeLog WSACalib Mean modified julian date of frameset. float 8 days -0.9999995e9 TIME_DATE
mergedClass calSource, calSynopticSource WSACalib Class flag from available measurements (1|0|-1|-2|-3|-9=galaxy|noise|stellar|probableStar|probableGalaxy|saturated) smallint 2     CODE_MISC
Individual detection classifications are combined in the source merging process to produce a set of attributes for each merged source as follows. Presently, a basic classification table is defined that assigns reasonably accurate, self-consistent probability values for a given classification code:
FlagMeaning
Probability (%)
StarGalaxyNoiseSaturated
-9Saturated 0.0 0.0 5.095.0
-3Probable galaxy25.070.0 5.0 0.0
-2Probable star70.025.0 5.0 0.0
-1Star90.0 5.0 5.0 0.0
0Noise 5.0 5.090.0 0.0
+1Galaxy 5.090.0 5.0 0.0

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

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

mergedClass calSourceRemeasurement WSACalib Class flag based on list remeasurement prescription smallint 2     CODE_MISC
mergedClass dxsJKsource, gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, lasExtendedSource, lasPointSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource, reliableUdsSource WSA Class flag from available measurements (1|0|-1|-2|-3|-9=galaxy|noise|stellar|probableStar|probableGalaxy|saturated) smallint 2     CODE_MISC
mergedClass dxsSource, gcsSource, gpsSource, lasSource, udsSource WSA Class flag from available measurements (1|0|-1|-2|-3|-9=galaxy|noise|stellar|probableStar|probableGalaxy|saturated) smallint 2     CODE_MISC
Individual detection classifications are combined in the source merging process to produce a set of attributes for each merged source as follows. Presently, a basic classification table is defined that assigns reasonably accurate, self-consistent probability values for a given classification code:
FlagMeaning
Probability (%)
StarGalaxyNoiseSaturated
-9Saturated 0.0 0.0 5.095.0
-3Probable galaxy25.070.0 5.0 0.0
-2Probable star70.025.0 5.0 0.0
-1Star90.0 5.0 5.0 0.0
0Noise 5.0 5.090.0 0.0
+1Galaxy 5.090.0 5.0 0.0

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

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

mergedClass dxsSourceRemeasurement, gcsSourceRemeasurement, gpsSourceRemeasurement, lasSourceRemeasurement, udsSourceRemeasurement WSA Class flag based on list remeasurement prescription smallint 2     CODE_MISC
mergedClassStat calSource, calSynopticSource WSACalib Merged N(0,1) stellarness-of-profile statistic real 4   -0.9999995e9 STAT_PROP
This profile classification statistic is a continuously distributed, Gaussian N(0,1) (i.e. zero mean, unit variance) statistic formed from the available individual classification statistics by averaging them and multiplying by N1/2 such that cuts on mergedClassStat result in completeness being independent of number of frames an object appears on, but with reliability improving with the number of frames.
mergedClassStat dxsJKsource, gcsPointSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, lasExtendedSource, lasPointSource, lasYJHKsource, reliableDxsSource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource WSA Merged N(0,1) stellarness-of-profile statistic real 4   -0.9999995e9 STAT_PROP
mergedClassStat dxsSource, gcsSource, gpsSource, lasSource WSA Merged N(0,1) stellarness-of-profile statistic real 4   -0.9999995e9 STAT_PROP
This profile classification statistic is a continuously distributed, Gaussian N(0,1) (i.e. zero mean, unit variance) statistic formed from the available individual classification statistics by averaging them and multiplying by N1/2 such that cuts on mergedClassStat result in completeness being independent of number of frames an object appears on, but with reliability improving with the number of frames.
mergedClassStat reliableUdsSource WSA Merged S-Extractor classification statistic real 4   -0.9999995e9 STAT_PROP
mergedClassStat udsSource WSA Merged S-Extractor classification statistic real 4   -0.9999995e9 STAT_PROP
Inverse variance-weighted mean of the available individual passband S-Extractor classification statistics *ClassStat.
mergeLogTable Programme WSA Table name of curation log for source merging varchar 64     ??
mergeLogTable Programme WSACalib Table name of curation log for source merging varchar 64     ??
mergeLogTable Programme WSATransit Table name of curation log for source merging varchar 64     ??
mergeSwVersion calMergeLog, calSynopticMergeLog WSACalib version number of the software used to merge the frames real 4     ID_VERSION
mergeSwVersion dxsJKmergeLog, dxsMergeLog, gcsMergeLog, gcsZYJHKmergeLog, gpsJHKmergeLog, gpsMergeLog, lasMergeLog, lasYJHKmergeLog, udsMergeLog WSA version number of the software used to merge the frames real 4     ID_VERSION
method RequiredDiffImage WSA CASU difference image tool option string specifying the method to employ (recommended value=adaptive/back/zerosky) varchar 64     ??
method RequiredDiffImage WSACalib CASU difference image tool option string specifying the method to employ (recommended value=adaptive/back/zerosky) varchar 64     ??
method RequiredDiffImage WSATransit CASU difference image tool option string specifying the method to employ (recommended value=adaptive/back/zerosky) varchar 64     ??
MF1 glimpse_hrc_inter, glimpse_mca_inter GLIMPSE Flux calc mathod flag for band 1 flux int 4   -9  
MF2 glimpse_hrc_inter, glimpse_mca_inter GLIMPSE Flux calc mathod flag for band 2 flux int 4   -9  
MF3 glimpse_hrc_inter, glimpse_mca_inter GLIMPSE Flux calc mathod flag for band 3 flux int 4   -9  
MF3_6 glimpse1_hrc, glimpse1_mca, glimpse2_hrc, glimpse2_mca GLIMPSE Flux calculation method flag 3.6um IRAC (Band 1) int 4   -9  
MF4 glimpse_hrc_inter, glimpse_mca_inter GLIMPSE Flux calc mathod flag for band 4 flux int 4   -9  
MF4_5 glimpse1_hrc, glimpse1_mca, glimpse2_hrc, glimpse2_mca GLIMPSE Flux calculation method flag 4.5um IRAC (Band 2) int 4   -9  
MF5_8 glimpse1_hrc, glimpse1_mca, glimpse2_hrc, glimpse2_mca GLIMPSE Flux calculation method flag 5.8um IRAC (Band 3) int 4   -9  
MF8_0 glimpse1_hrc, glimpse1_mca, glimpse2_hrc, glimpse2_mca GLIMPSE Flux calculation method flag 8.0um IRAC (Band 4) int 4   -9  
mFlag rosat_bsc, rosat_fsc ROSAT source missed by SASS varchar 1     CODE_MISC
MGC_B_KCORR mgcGalaxyStruct MGC MGC B-band K-correction real 4   0.000  
MGC_BEST_Z mgcGalaxyStruct MGC Best redshift real 4   9.99999  
MGC_BEST_ZQUAL mgcGalaxyStruct MGC Quality of best redshift (0-2 = BAD, 3-5=GOOD, 9=Not observed) tinyint 1   9  
MGC_HLR_TRUE mgcGalaxyStruct MGC Seeing corrected Half light radius real 4 arcsecs    
MGC_SEEING mgcGalaxyStruct MGC Seeing of MGC field real 4 arcsecs    
MGC_SPEC_TYPE mgcGalaxyStruct MGC Best spectral type fit from Poggianti (1998)sample (type+age, i.e., el150 = E/S0 15.0Gyrs) varchar 8   none  
MGCFN mgcDetection MGC MGC field number int 4      
MGCID mgcBrightSpec, mgcDetection, mgcGalaxyStruct MGC MGC object ID bigint 8      
MGCZ_ZHELIO mgcBrightSpec MGC MGCz heliocentric redshift real 4      
MGCZ_ZQUAL mgcBrightSpec MGC MGCz redshift quality tinyint 1      
mHcon iras_psc IRAS Possible number of HCONs tinyint 1     NUMBER
min firstSource FIRST minor axes derived from the elliptical Gaussian model for the source after deconvolution. real 4 arcsec   EXTENSION_FWHM_MIN
minAxis nvssSource NVSS Fitted (deconvolved) minor axis of radio source real 4 arcsec   EXTENSION_FWHM_MIN
minDec CurrentAstrometry WSACalib The minimum Dec (J2000) on the device float 8 Degrees -0.9999995e9 POS_EQ_DEC_MAIN
minDec CurrentAstrometry WSATransit The minimum Dec (J2000) on the device float 8 Degrees -0.9999995e9 POS_EQ_DEC_MAIN
minDec CurrentAstrometry, PreviousAstrometry WSA The minimum Dec (J2000) on the device float 8 Degrees -0.9999995e9 POS_EQ_DEC_MAIN
minImageSize MultiframeDetector WSA Minimum size for images {catalogue extension keyword:  MINPIX} int 4 pixels -99999999 ??
Tunable parameter, in conjunction with the threshold above this determines how deep and how small "real" images can be. The default precludes many of the few pixel-hit cosmic rays from being considered since "real" images must have 4 contiguous simply-connected pixels in the union of the detection filter and data domains. For more details on image detection and parametersiation see the papers in CASU WFCAM/VISTA Publications.
minImageSize MultiframeDetector WSACalib Minimum size for images {catalogue extension keyword:  MINPIX} int 4 pixels -99999999 ??
Tunable parameter, in conjunction with the threshold above this determines how deep and how small "real" images can be. The default precludes many of the few pixel-hit cosmic rays from being considered since "real" images must have 4 contiguous simply-connected pixels in the union of the detection filter and data domains. For more details on image detection and parametersiation see the papers in CASU WFCAM/VISTA Publications.
minImageSize MultiframeDetector WSATransit Minimum size for images {catalogue extension keyword:  MINPIX} int 4 pixels -99999999 ??
Tunable parameter, in conjunction with the threshold above this determines how deep and how small "real" images can be. The default precludes many of the few pixel-hit cosmic rays from being considered since "real" images must have 4 contiguous simply-connected pixels in the union of the detection filter and data domains. For more details on image detection and parametersiation see the papers in CASU WFCAM/VISTA Publications.
minor iras_psc IRAS Uncertainty ellipse minor axis smallint 2 arcsec   ERROR
minPllx calVariability WSACalib Lower limit of 90% confidence interval for parallax measurement real 4 mas -0.9999995e9  
The Variability table contains statistics from the set of observations of each source. At present, the mean ra and dec and the error in two tangential directions are calculated. The "ra" direction is defined as tangential to both the radial direction and the cartesian z-axis and the "dec" direction is defined as both the radial direction and the "ra" direction. Since the current model is just the mean and standard deviation of the data, then the chi-squared of the fit=1. Data from good frames across all bands go into the astrometric model determination. This will include bands in non-synoptic filters: the one observation in these bands can help. In future releases a fit will be made to the rms data as a function of magnitude in each band, as has already happened for photometric data and a motion model that incorporates proper motion (and possibly parallax) will be used. The motion model is a parameter in the VarFrameSetInfo table.
minPllx dxsVariability, udsVariability WSA Lower limit of 90% confidence interval for parallax measurement real 4 mas -0.9999995e9  
The Variability table contains statistics from the set of observations of each source. At present, the mean ra and dec and the error in two tangential directions are calculated. The "ra" direction is defined as tangential to both the radial direction and the cartesian z-axis and the "dec" direction is defined as both the radial direction and the "ra" direction. Since the current model is just the mean and standard deviation of the data, then the chi-squared of the fit=1. Data from good frames across all bands go into the astrometric model determination. This will include bands in non-synoptic filters: the one observation in these bands can help. In future releases a fit will be made to the rms data as a function of magnitude in each band, as has already happened for photometric data and a motion model that incorporates proper motion (and possibly parallax) will be used. The motion model is a parameter in the VarFrameSetInfo table.
minRa CurrentAstrometry WSACalib The minimum RA (J2000) on the device float 8 Degrees -0.9999995e9 POS_EQ_RA_OTHER
minRa CurrentAstrometry WSATransit The minimum RA (J2000) on the device float 8 Degrees -0.9999995e9 POS_EQ_RA_OTHER
minRa CurrentAstrometry, PreviousAstrometry WSA The minimum RA (J2000) on the device float 8 Degrees -0.9999995e9 POS_EQ_RA_OTHER
mirrBottTempNW Multiframe WSA Mirror bottom temp. NW {image primary HDU keyword: MIRRBTNW} real 4 degrees_Celsius -0.9999995e9 PHYS_TEMP_MISC
mirrBottTempNW Multiframe WSACalib Mirror bottom temp. NW {image primary HDU keyword: MIRRBTNW} real 4 degrees_Celsius -0.9999995e9 PHYS_TEMP_MISC
mirrBottTempNW Multiframe WSATransit Mirror bottom temp. NW {image primary HDU keyword: MIRRBTNW} real 4 degrees_Celsius -0.9999995e9 PHYS_TEMP_MISC
mirrTempNE Multiframe WSA Mirror temperature NE {image primary HDU keyword: MIRR_NE} real 4 degrees_Celsius -0.9999995e9 PHYS_TEMP_MISC
mirrTempNE Multiframe WSACalib Mirror temperature NE {image primary HDU keyword: MIRR_NE} real 4 degrees_Celsius -0.9999995e9 PHYS_TEMP_MISC
mirrTempNE Multiframe WSATransit Mirror temperature NE {image primary HDU keyword: MIRR_NE} real 4 degrees_Celsius -0.9999995e9 PHYS_TEMP_MISC
mirrTempNW Multiframe WSA Mirror temperature NW {image primary HDU keyword: MIRR_NW} real 4 degrees_Celsius -0.9999995e9 PHYS_TEMP_MISC
mirrTempNW Multiframe WSACalib Mirror temperature NW {image primary HDU keyword: MIRR_NW} real 4 degrees_Celsius -0.9999995e9 PHYS_TEMP_MISC
mirrTempNW Multiframe WSATransit Mirror temperature NW {image primary HDU keyword: MIRR_NW} real 4 degrees_Celsius -0.9999995e9 PHYS_TEMP_MISC
mirrTempSE Multiframe WSA Mirror temperature SE {image primary HDU keyword: MIRR_SE} real 4 degrees_Celsius -0.9999995e9 PHYS_TEMP_MISC
mirrTempSE Multiframe WSACalib Mirror temperature SE {image primary HDU keyword: MIRR_SE} real 4 degrees_Celsius -0.9999995e9 PHYS_TEMP_MISC
mirrTempSE Multiframe WSATransit Mirror temperature SE {image primary HDU keyword: MIRR_SE} real 4 degrees_Celsius -0.9999995e9 PHYS_TEMP_MISC
mirrTempSW Multiframe WSA Mirror temperature SW {image primary HDU keyword: MIRR_SW} real 4 degrees_Celsius -0.9999995e9 PHYS_TEMP_MISC
mirrTempSW Multiframe WSACalib Mirror temperature SW {image primary HDU keyword: MIRR_SW} real 4 degrees_Celsius -0.9999995e9 PHYS_TEMP_MISC
mirrTempSW Multiframe WSATransit Mirror temperature SW {image primary HDU keyword: MIRR_SW} real 4 degrees_Celsius -0.9999995e9 PHYS_TEMP_MISC
mirrTopTempNW Multiframe WSA Mirror top temp. NW {image primary HDU keyword: MIRRTPNW} real 4 degrees_Celsius -0.9999995e9 PHYS_TEMP_MISC
mirrTopTempNW Multiframe WSACalib Mirror top temp. NW {image primary HDU keyword: MIRRTPNW} real 4 degrees_Celsius -0.9999995e9 PHYS_TEMP_MISC
mirrTopTempNW Multiframe WSATransit Mirror top temp. NW {image primary HDU keyword: MIRRTPNW} real 4 degrees_Celsius -0.9999995e9 PHYS_TEMP_MISC
MJD_START twoxmm XMM Modified Julian Date (i.e., JD - 2400000.5) of the start of the observation. float 8 days    
MJD_STOP twoxmm XMM Modified Julian Date (i.e., JD - 2400000.5) of the end of the observation. float 8      
mjdObs Multiframe WSA Modified Julian Date of the observation {image primary HDU keyword: MJD-OBS} float 8   -0.9999995e9 TIME_DATE
mjdObs Multiframe WSACalib Modified Julian Date of the observation {image primary HDU keyword: MJD-OBS} float 8   -0.9999995e9 TIME_DATE
mjdObs Multiframe WSATransit Modified Julian Date of the observation {image primary HDU keyword: MJD-OBS} float 8   -0.9999995e9 TIME_DATE
modDate rosat_bsc, rosat_fsc ROSAT date when source properties were changed (MM-DD-YYYY) datetime 8 mm-dd-yyyy   TIME_DATE
modelDistSecs calSourceXSynopticSourceBestMatch WSACalib separation from expected position given astrometric model in calSource variability. real 4 arcsec -0.9999995e9  
modelDistSecs dxsSourceXDetectionBestMatch WSA separation from expected position given astrometric model in dxsSource variability. real 4 arcsec -0.9999995e9  
modelDistSecs udsSourceXDetectionBestMatch WSA separation from expected position given astrometric model in udsSource variability. real 4 arcsec -0.9999995e9  
MORPH_TYPE mgcGalaxyStruct MGC SPD's EYEBALL morphology (1=E/S0, 2=Sabc, 3=Sd/Irr, 4=dE) tinyint 1   0  
morphClassFlag MultiframeDetector WSA Image morphological classifier flag, set if the classifier has been run. If so an object classification flag and a stellarness index is included in the binary table columns. {catalogue extension keyword:  CLASSIFD} tinyint 1   0 CODE_MISC
morphClassFlag MultiframeDetector WSACalib Image morphological classifier flag, set if the classifier has been run. If so an object classification flag and a stellarness index is included in the binary table columns. {catalogue extension keyword:  CLASSIFD} tinyint 1   0 CODE_MISC
morphClassFlag MultiframeDetector WSATransit Image morphological classifier flag, set if the classifier has been run. If so an object classification flag and a stellarness index is included in the binary table columns. {catalogue extension keyword:  CLASSIFD} tinyint 1   0 CODE_MISC
mosaicTool Programme WSA Name of mosaicing tool to be used varchar 8   NONE ??
mosaicTool Programme WSACalib Name of mosaicing tool to be used varchar 8   NONE ??
mosaicTool Programme WSATransit Name of mosaicing tool to be used varchar 8   NONE ??
motionModel calVarFrameSetInfo WSACalib Motion model used to produce BestMatch table. Values: static; proper motion; proper motion and parallax. varchar 32   static  
Motion model for frameset in question. This can be static: all objects in the frameset are assumed to be stationary; proper motion: all objects in the frameset are fit for a linear proper motion; proper motion and parallax: all objects in the frameset are fit for a linear proper motion and a parallax. In all cases, objects are assumed to be stars with small values of proper motion and parallax.
motionModel dxsVarFrameSetInfo, udsVarFrameSetInfo WSA Motion model used to produce BestMatch table. Values: static; proper motion; proper motion and parallax. varchar 32   static  
Motion model for frameset in question. This can be static: all objects in the frameset are assumed to be stationary; proper motion: all objects in the frameset are fit for a linear proper motion; proper motion and parallax: all objects in the frameset are fit for a linear proper motion and a parallax. In all cases, objects are assumed to be stars with small values of proper motion and parallax.
mp_flg twomass_psc 2MASS Minor Planet Flag. smallint 2     CODE_MISC
mp_key twomass_xsc 2MASS key to minor planet prediction DB record. int 4     ID_NUMBER
msbID Multiframe WSA Id min.-schedulable block {image primary HDU keyword: MSBID} varchar 64   NONE ID_NUMBER
msbID Multiframe WSACalib Id min.-schedulable block {image primary HDU keyword: MSBID} varchar 64   NONE ID_NUMBER
msbID Multiframe WSATransit Id min.-schedulable block {image primary HDU keyword: MSBID} varchar 64   NONE ID_NUMBER
msbRejected Multiframe WSA Cause of MSB rejection, default if not rejected {image primary HDU keyword: MSBFUD} varchar 256   NONE  
msbRejected Multiframe WSACalib Cause of MSB rejection, default if not rejected {image primary HDU keyword: MSBFUD} varchar 256   NONE  
msbRejected Multiframe WSATransit Cause of MSB rejection, default if not rejected {image primary HDU keyword: MSBFUD} varchar 256   NONE  
MU_EFF mgcBrightSpec MGC Effective surface brightness real 4 mag arcsec^-2    
muDec calVariability WSACalib Proper motion in Dec real 4 mas/yr -0.9999995e9 POS_EQ_PMDEC
The Variability table contains statistics from the set of observations of each source. At present, the mean ra and dec and the error in two tangential directions are calculated. The "ra" direction is defined as tangential to both the radial direction and the cartesian z-axis and the "dec" direction is defined as both the radial direction and the "ra" direction. Since the current model is just the mean and standard deviation of the data, then the chi-squared of the fit=1. Data from good frames across all bands go into the astrometric model determination. This will include bands in non-synoptic filters: the one observation in these bands can help. In future releases a fit will be made to the rms data as a function of magnitude in each band, as has already happened for photometric data and a motion model that incorporates proper motion (and possibly parallax) will be used. The motion model is a parameter in the VarFrameSetInfo table.
muDec dxsVariability, udsVariability WSA Proper motion in Dec real 4 mas/yr -0.9999995e9 POS_EQ_PMDEC
The Variability table contains statistics from the set of observations of each source. At present, the mean ra and dec and the error in two tangential directions are calculated. The "ra" direction is defined as tangential to both the radial direction and the cartesian z-axis and the "dec" direction is defined as both the radial direction and the "ra" direction. Since the current model is just the mean and standard deviation of the data, then the chi-squared of the fit=1. Data from good frames across all bands go into the astrometric model determination. This will include bands in non-synoptic filters: the one observation in these bands can help. In future releases a fit will be made to the rms data as a function of magnitude in each band, as has already happened for photometric data and a motion model that incorporates proper motion (and possibly parallax) will be used. The motion model is a parameter in the VarFrameSetInfo table.
muDec gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource WSA Proper motion in Dec direction real 4 mas/yr -0.9999995e9 POS_EQ_PMDEC
multiframeID allFrameSets, CurrentAstrometry, dxsDetection, dxsFrameSets, dxsListRemeasurement, dxsSourceXDetectionBestMatch, gcsDetection, gcsFrameSets, gcsListRemeasurement, gpsDetection, gpsFrameSets, gpsListRemeasurement, lasDetection, lasFrameSets, lasListRemeasurement, MultiframeDetector, PreviousAstrometry, PreviousMFDZP, ProgrammeFrame, UKIDSSDetection, udsDetection, udsFrameSets, udsListRemeasurement, udsSourceXDetectionBestMatch WSA the UID of the relevant multiframe bigint 8     ID_FRAME
multiframeID CurrentAstrometry, calDetection, calListRemeasurement WSACalib the UID of the relevant multiframe bigint 8     ID_FRAME
multiframeID CurrentAstrometry, ptsDetection WSATransit the UID of the relevant multiframe bigint 8     ID_FRAME
multiframeID Multiframe WSA UID of the multiframe (assigned sequentially by the archive ingest process) bigint 8     ID_FRAME
multiframeID Multiframe WSACalib UID of the multiframe (assigned sequentially by the archive ingest process) bigint 8     ID_FRAME
multiframeID Multiframe WSATransit UID of the multiframe (assigned sequentially by the archive ingest process) bigint 8     ID_FRAME
multiframeID Provenance WSA the UID of the component frame bigint 8     ID_FRAME
multiframeID Provenance WSACalib the UID of the component frame bigint 8     ID_FRAME
multiframeID Provenance WSATransit the UID of the component frame bigint 8     ID_FRAME
muRa calVariability WSACalib Proper motion in RA real 4 mas/yr -0.9999995e9 POS_EQ_PMRA
The Variability table contains statistics from the set of observations of each source. At present, the mean ra and dec and the error in two tangential directions are calculated. The "ra" direction is defined as tangential to both the radial direction and the cartesian z-axis and the "dec" direction is defined as both the radial direction and the "ra" direction. Since the current model is just the mean and standard deviation of the data, then the chi-squared of the fit=1. Data from good frames across all bands go into the astrometric model determination. This will include bands in non-synoptic filters: the one observation in these bands can help. In future releases a fit will be made to the rms data as a function of magnitude in each band, as has already happened for photometric data and a motion model that incorporates proper motion (and possibly parallax) will be used. The motion model is a parameter in the VarFrameSetInfo table.
muRa dxsVariability, udsVariability WSA Proper motion in RA real 4 mas/yr -0.9999995e9 POS_EQ_PMRA
The Variability table contains statistics from the set of observations of each source. At present, the mean ra and dec and the error in two tangential directions are calculated. The "ra" direction is defined as tangential to both the radial direction and the cartesian z-axis and the "dec" direction is defined as both the radial direction and the "ra" direction. Since the current model is just the mean and standard deviation of the data, then the chi-squared of the fit=1. Data from good frames across all bands go into the astrometric model determination. This will include bands in non-synoptic filters: the one observation in these bands can help. In future releases a fit will be made to the rms data as a function of magnitude in each band, as has already happened for photometric data and a motion model that incorporates proper motion (and possibly parallax) will be used. The motion model is a parameter in the VarFrameSetInfo table.
muRa gcsPointSource, gcsSource, gcsZYJHKsource, gpsJHKsource, gpsPointSource, gpsSource, lasExtendedSource, lasPointSource, lasSource, lasYJHKsource, reliableGcsPointSource, reliableGpsPointSource, reliableLasPointSource WSA Proper motion in RA direction real 4 mas/yr -0.9999995e9 POS_EQ_PMRA


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23/02/2010