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XMMOMSUSS - XMM-Newton Optical Monitor Serendipitous UV Source Survey Catalog, v2.0

HEASARC
Archive

Overview

The second release of the XMM-OM Serendipitous Ultra-violet Source Survey (XMM-SUSS2) is a catalog of optical/UV sources detected serendipitously by the Optical Monitor (OM) on-board the European Space Agency's (ESA's) XMM-Newton observatory. The data were processed in January 2014 at the European Space Astronomy Centre (ESAC, Madrid, Spain) and at Mullard Space Science Laboratory (MSSL, UCL, London, U.K.) by using the XMM Science Analysis Software (SAS) with some improved tasks which will be available in system version 14.0. The description of the previous release of the catalogue can be found in Page M.J. et al. (2012, MNRAS, 426, 903).

The catalog contains source detections drawn from 6,604 XMM-OM observations in optical and UV filters made between 2000 and 2012. In addition to covering a larger observation period, the second release differs from the previous one by inclusion of all the OM observations (not only those containing UV filters) and by performing source detection on stacked images, thus facilitating the detection of fainter sources.

The total number of entries in this second release is 5,595,331. They correspond to 4,008,879 sources, of which 692,223 have multiple entries in this source table, corresponding to different observations. For each entry, positional and photometric data (count rate, magnitude and flux) and quality flags for each measurement are provided.

U, B, V, UVW2, UVM2 and UVW1 refer to the filter bandpasses defined in the Source Properties: Filter Set section of the MSSL documentation for this catalog: http://www.mssl.ucl.ac.uk/www_astro/XMM-OM-SUSS/SourcePropertiesFilters.shtml.

The documentation on the first release of this catalog is available at http://www.mssl.ucl.ac.uk/www_astro/XMM-OM-SUSS/Summary.shtml.


Catalog Bibcode

2012MNRAS.426..903P

References

The XMM-OM Serendipitous Ultra-violet Source Survey (SUSS) has been created at the European Space Astronomy Centre (ESAC, Madrid, Spain) and at the University College London's (UCL's) Mullard Space Science Laboratory (MSSL) on behalf of ESA. This catalog is a partner resource to the 2XMM serendipitous X-ray source catalog. The reference paper given below, notice, refers to release 1.
The XMM-Newton serendipitous ultraviolet source survey catalogue.
   Page M. J., Brindle C., Talavera A., Still M., Rosen S. R., Yershov V. N.,
   Ziaeepour H., Mason K. O., Cropper M. S., Breeveld A. A., Loiseau N.,
   Mignani R., Smith A., Murdin P.
   <Mon. Not. Royal Astr. Soc., 426, 903-926 (2012)>
   =2012MNRAS.426..903P

Provenance

This HEASARC database table contains the second release of the XMM-OM SUSS catalog, XMM-SUSS2, released by ESA in February 2014, and obtained from the XMM-Newton Science Archive (http://xmm.esac.esa.int/xsa). It is also available at the HEASARC as the gzipped FITS file http://heasarc.gsfc.nasa.gov/FTP/xmm/data/catalogues/XMM-OM-SUSSv2.0-20140213.fits.gz.

Parameters

Name
The IAU-designated source name of format 'XMMOM JHHMMSS.S+DDMMSS'.

N_Summary
This is a reference number index for the XMM-Newton pointing in which the particular detection was made, providing a cross-referencing system allowing users to couple a source to its parent observation.

ObsID
Each XMM pointing has an exclusive 10-digit observation identification number or ObsID. This parameter contains the ObsID of the observation from which the source detection originates.

Src_Num
This is the unique reference number for the source, internal only to the XMM-SUSS2 catalog.

UVW2_Srcdist
This parameter provides the angular distance in arcseconds of the source from its nearest detected celestial neighbor in the specified band. It allows the user to assess the probability of source confusion, contamination or misidentification.

UVM2_Srcdist
This parameter provides the angular distance in arcseconds of the source from its nearest detected celestial neighbor in the specified band. It allows the user to assess the probability of source confusion, contamination or misidentification.

UVW1_Srcdist
This parameter provides the angular distance in arcseconds of the source from its nearest detected celestial neighbor in the specified band. It allows the user to assess the probability of source confusion, contamination or misidentification.

U_Srcdist
This parameter provides the angular distance in arcseconds of the source from its nearest detected celestial neighbor in the specified band. It allows the user to assess the probability of source confusion, contamination or misidentification.

B_Srcdist
This parameter provides the angular distance in arcseconds of the source from its nearest detected celestial neighbor in the specified band. It allows the user to assess the probability of source confusion, contamination or misidentification.

V_Srcdist
This parameter provides the angular distance in arcseconds of the source from its nearest detected celestial neighbor in the specified band. It allows the user to assess the probability of source confusion, contamination or misidentification.

RA
The measured Right Ascension of the source in the selected equinox. The on-board pointing 'knowledge' of the XMM-Newton spacecraft is good to a few arcsecs. All fields included within the XMM-SUSS2 catalog have had small order astrometric corrections performed upon them by correlating detected sources with the positions of USNO-B catalog optical objects. Note that the error provided in the error_radius parameter does not include the systematic uncertainty remaining after the astrometric correction. No proper motion corrections have been attempted.

Dec
The measured Declination of the source in the selected equinox. The on-board pointing 'knowledge' of the XMM-Newton spacecraft is good to a few arcsecs. All fields included within the XMM-SUSS2 catalog have had small order astrometric corrections performed upon them by correlating detected sources with the positions of USNO-B catalog optical objects. Note that the error provided in the error_radius parameter does not include the systematic uncertainty remaining after the astrometric correction. No proper motion corrections have been attempted.

Error_Radius
The statistical 1-sigma error in arcseconds attached to the measured source position. The RA and Dec errors are averaged with no weights to produce this parameter.

LII
The Galactic Longitude of the source.

BII
The Galactic Latitude of the source.

N_ObsID
Over the mission lifetime, XMM-Newton has revisited many fields or observed sources with overlapping fields. This field records the number of times a source has been detected during separate observations. Note that this is distinct from the number of times XMM has revisited the field. There may have been occasions where an observation was not deep enough to re-detect a specific source, or the source itself is variable. The criteria for matching a source over different epochs is that the positions are separated by < 1.5" and < 3 sigma. In cases where multiple sources within the same observation meet the matching criteria for another observation, the nearest source is adopted as the match.

UVW2_SNR
This parameter contains the significance of a source detection in the specified band above the data noise, in sigma. Data noise contains contributions from the background and source. Detector noise is negligible. Significance is calculated on raw count rates, uncorrected for photon coincidence losses.

UVM2_SNR
This parameter contains the significance of a source detection in the specified band above the data noise, in sigma. Data noise contains contributions from the background and source. Detector noise is negligible. Significance is calculated on raw count rates, uncorrected for photon coincidence losses.

UVW1_SNR
This parameter contains the significance of a source detection in the specified band above the data noise, in sigma. Data noise contains contributions from the background and source. Detector noise is negligible. Significance is calculated on raw count rates, uncorrected for photon coincidence losses.

U_SNR
This parameter contains the significance of a source detection in the specified band above the data noise, in sigma. Data noise contains contributions from the background and source. Detector noise is negligible. Significance is calculated on raw count rates, uncorrected for photon coincidence losses.

B_SNR
This parameter contains the significance of a source detection in the specified band above the data noise, in sigma. Data noise contains contributions from the background and source. Detector noise is negligible. Significance is calculated on raw count rates, uncorrected for photon coincidence losses.

V_SNR
This parameter contains the significance of a source detection in the specified band above the data noise, in sigma. Data noise contains contributions from the background and source. Detector noise is negligible. Significance is calculated on raw count rates, uncorrected for photon coincidence losses.

UVW2_Rate
This parameter contains the background-subtracted source count rate in the specified band corrected for coincidence loss using the standard calibration polynomial contained within the XMM CAL, in counts per second. Due to the nature of the OM detector, sources with count rates > 5 count/sec suffer from increasing quantities of photon coincidence loss where two photons arriving at the same location of the detector within one readout cycle cannot be distinguished. The effect is correctable using a count rate-dependent function up to corrected count rates of 400 count/sec.

UVW2_Rate_Error
The 1-sigma uncertainty in counts per second determined for the coincidence-corrected source count rate recorded in the corresponding count rate parameter for this band.

UVM2_Rate
This parameter contains the background-subtracted source count rate in the specified band corrected for coincidence loss using the standard calibration polynomial contained within the XMM CAL, in counts per second. Due to the nature of the OM detector, sources with count rates > 5 count/sec suffer from increasing quantities of photon coincidence loss where two photons arriving at the same location of the detector within one readout cycle cannot be distinguished. The effect is correctable using a count rate-dependent function up to corrected count rates of 400 count/sec.

UVM2_Rate_Error
The 1-sigma uncertainty in counts per second determined for the coincidence-corrected source count rate recorded in the corresponding count rate parameter for this band.

UVW1_Rate
This parameter contains the background-subtracted source count rate in the specified band corrected for coincidence loss using the standard calibration polynomial contained within the XMM CAL, in counts per second. Due to the nature of the OM detector, sources with count rates > 5 count/sec suffer from increasing quantities of photon coincidence loss where two photons arriving at the same location of the detector within one readout cycle cannot be distinguished. The effect is correctable using a count rate-dependent function up to corrected count rates of 400 count/sec.

UVW1_Rate_Error
The 1-sigma uncertainty in counts per second determined for the coincidence-corrected source count rate recorded in the corresponding count rate parameter for this band.

U_Rate
This parameter contains the background-subtracted source count rate in the specified band corrected for coincidence loss using the standard calibration polynomial contained within the XMM CAL, in counts per second. Due to the nature of the OM detector, sources with count rates > 5 count/sec suffer from increasing quantities of photon coincidence loss where two photons arriving at the same location of the detector within one readout cycle cannot be distinguished. The effect is correctable using a count rate-dependent function up to corrected count rates of 400 count/sec.

U_Rate_Error
The 1-sigma uncertainty in counts per second determined for the coincidence-corrected source count rate recorded in the corresponding count rate parameter for this band.

B_Rate
This parameter contains the background-subtracted source count rate in the specified band corrected for coincidence loss using the standard calibration polynomial contained within the XMM CAL, in counts per second. Due to the nature of the OM detector, sources with count rates > 5 count/sec suffer from increasing quantities of photon coincidence loss where two photons arriving at the same location of the detector within one readout cycle cannot be distinguished. The effect is correctable using a count rate-dependent function up to corrected count rates of 400 count/sec.

B_Rate_Error
The 1-sigma uncertainty in counts per second determined for the coincidence-corrected source count rate recorded in the corresponding count rate parameter for this band.

V_Rate
This parameter contains the background-subtracted source count rate in the specified band corrected for coincidence loss using the standard calibration polynomial contained within the XMM CAL, in counts per second. Due to the nature of the OM detector, sources with count rates > 5 count/sec suffer from increasing quantities of photon coincidence loss where two photons arriving at the same location of the detector within one readout cycle cannot be distinguished. The effect is correctable using a count rate-dependent function up to corrected count rates of 400 count/sec.

V_Rate_Error
The 1-sigma uncertainty in counts per second determined for the coincidence-corrected source count rate recorded in the corresponding count rate parameter for this band.

UVW2_Flux
This parameter contains the flux in the specified band calculated using the conversion factor (CF) contained within the XMM CAL, in erg/cm2/s/Angstrom. The conversion from coincidence-corrected source count rate to AB flux occurs through a simple filter-dependent, multiplicative factor: FILTER_FLUX = CF * FILTER_RATE.

UVW2_Flux_Error
The 1-sigma uncertainty determined for the flux of the source recorded in the corresponding band, in erg/cm2/s/Angstrom.

UVM2_Flux
This parameter contains the flux in the specified band calculated using the conversion factor (CF) contained within the XMM CAL, in erg/cm2/s/Angstrom. The conversion from coincidence-corrected source count rate to AB flux occurs through a simple filter-dependent, multiplicative factor: FILTER_FLUX = CF * FILTER_RATE.

UVM2_Flux_Error
The 1-sigma uncertainty determined for the flux of the source recorded in the corresponding band, in erg/cm2/s/Angstrom.

UVW1_Flux
This parameter contains the flux in the specified band calculated using the conversion factor (CF) contained within the XMM CAL, in erg/cm2/s/Angstrom. The conversion from coincidence-corrected source count rate to AB flux occurs through a simple filter-dependent, multiplicative factor: FILTER_FLUX = CF * FILTER_RATE.

UVW1_Flux_Error
The 1-sigma uncertainty determined for the flux of the source recorded in the corresponding band, in erg/cm2/s/Angstrom.

U_Flux
This parameter contains the flux in the specified band calculated using the conversion factor (CF) contained within the XMM CAL, in erg/cm2/s/Angstrom. The conversion from coincidence-corrected source count rate to AB flux occurs through a simple filter-dependent, multiplicative factor: FILTER_FLUX = CF * FILTER_RATE.

U_Flux_Error
The 1-sigma uncertainty determined for the flux of the source recorded in the corresponding band, in erg/cm2/s/Angstrom.

B_Flux
This parameter contains the flux in the specified band calculated using the conversion factor (CF) contained within the XMM CAL, in erg/cm2/s/Angstrom. The conversion from coincidence-corrected source count rate to AB flux occurs through a simple filter-dependent, multiplicative factor: FILTER_FLUX = CF * FILTER_RATE.

B_Flux_Error
The 1-sigma uncertainty determined for the flux of the source recorded in the corresponding band, in erg/cm2/s/Angstrom.

V_Flux
This parameter contains the flux in the specified band calculated using the conversion factor (CF) contained within the XMM CAL, in erg/cm2/s/Angstrom. The conversion from coincidence-corrected source count rate to AB flux occurs through a simple filter-dependent, multiplicative factor: FILTER_FLUX = CF * FILTER_RATE.

V_Flux_Error
The 1-sigma uncertainty determined for the flux of the source recorded in the corresponding band, in erg/cm2/s/Angstrom.

UVW2mag_Ab
This parameter contains the AB magnitude of the source in the specified band calculated using the zero point magnitude (AZP) contained within the XMM CAL. The conversion from coincidence-corrected source count rate to AB magnitude occurs through the standard logarithmic expression with filter-dependent, zero points: FILTERMAG_AB = AZP - 2.5log(FILTER_RATE).

UVW2mag_AB_Error
The 1-sigma uncertainty determined for the AB magnitude of the source recorded in the corresponding FILTERMAG_AB parameter.

UVM2mag_Ab
This parameter contains the AB magnitude of the source in the specified band calculated using the zero point magnitude (AZP) contained within the XMM CAL. The conversion from coincidence-corrected source count rate to AB magnitude occurs through the standard logarithmic expression with filter-dependent, zero points: FILTERMAG_AB = AZP - 2.5log(FILTER_RATE).

UVM2mag_AB_Error
The 1-sigma uncertainty determined for the AB magnitude of the source recorded in the corresponding FILTERMAG_AB parameter.

UVW1mag_Ab
This parameter contains the AB magnitude of the source in the specified band calculated using the zero point magnitude (AZP) contained within the XMM CAL. The conversion from coincidence-corrected source count rate to AB magnitude occurs through the standard logarithmic expression with filter-dependent, zero points: FILTERMAG_AB = AZP - 2.5log(FILTER_RATE).

UVW1mag_AB_Error
The 1-sigma uncertainty determined for the AB magnitude of the source recorded in the corresponding FILTERMAG_AB parameter.

Umag_Ab
This parameter contains the AB magnitude of the source in the specified band calculated using the zero point magnitude (AZP) contained within the XMM CAL. The conversion from coincidence-corrected source count rate to AB magnitude occurs through the standard logarithmic expression with filter-dependent, zero points: FILTERMAG_AB = AZP - 2.5log(FILTER_RATE).

Umag_AB_Error
The 1-sigma uncertainty determined for the AB magnitude of the source recorded in the corresponding FILTERMAG_AB parameter.

Bmag_Ab
This parameter contains the AB magnitude of the source in the specified band calculated using the zero point magnitude (AZP) contained within the XMM CAL. The conversion from coincidence-corrected source count rate to AB magnitude occurs through the standard logarithmic expression with filter-dependent, zero points: FILTERMAG_AB = AZP - 2.5log(FILTER_RATE).

Bmag_AB_Error
The 1-sigma uncertainty determined for the AB magnitude of the source recorded in the corresponding FILTERMAG_AB parameter.

Vmag_Ab
This parameter contains the AB magnitude of the source in the specified band calculated using the zero point magnitude (AZP) contained within the XMM CAL. The conversion from coincidence-corrected source count rate to AB magnitude occurs through the standard logarithmic expression with filter-dependent, zero points: FILTERMAG_AB = AZP - 2.5log(FILTER_RATE).

Vmag_AB_Error
The 1-sigma uncertainty determined for the AB magnitude of the source recorded in the corresponding FILTERMAG_AB parameter.

UVW2mag_Vega
This parameter contains the Vega (Johnson) magnitude of the source in the specified band calculated using the zero point magnitude (VZP) contained within the XMM CAL. The conversion from coincidence-corrected source count rate to Vega (Johnson) magnitude occurs through the standard logarithmic expression with filter-dependent, zero points: FILTERMAG_VEGA = VZP - 2.5log(FILTER_RATE).

UVW2mag_Vega_Error
The 1-sigma uncertainty determined for the Vega (Johnson) magnitude in the specified band of the source recorded in the corresponding FILTERMAG_VEGA parameter.

UVM2mag_Vega
This parameter contains the Vega (Johnson) magnitude of the source in the specified band calculated using the zero point magnitude (VZP) contained within the XMM CAL. The conversion from coincidence-corrected source count rate to Vega (Johnson) magnitude occurs through the standard logarithmic expression with filter-dependent, zero points: FILTERMAG_VEGA = VZP - 2.5log(FILTER_RATE).

UVM2mag_Vega_Error
The 1-sigma uncertainty determined for the Vega (Johnson) magnitude in the specified band of the source recorded in the corresponding FILTERMAG_VEGA parameter.

UVW1mag_Vega
This parameter contains the Vega (Johnson) magnitude of the source in the specified band calculated using the zero point magnitude (VZP) contained within the XMM CAL. The conversion from coincidence-corrected source count rate to Vega (Johnson) magnitude occurs through the standard logarithmic expression with filter-dependent, zero points: FILTERMAG_VEGA = VZP - 2.5log(FILTER_RATE).

UVW1mag_Vega_Error
The 1-sigma uncertainty determined for the Vega (Johnson) magnitude in the specified band of the source recorded in the corresponding FILTERMAG_VEGA parameter.

Umag_Vega
This parameter contains the Vega (Johnson) magnitude of the source in the specified band calculated using the zero point magnitude (VZP) contained within the XMM CAL. The conversion from coincidence-corrected source count rate to Vega (Johnson) magnitude occurs through the standard logarithmic expression with filter-dependent, zero points: FILTERMAG_VEGA = VZP - 2.5log(FILTER_RATE).

Umag_Vega_Error
The 1-sigma uncertainty determined for the Vega (Johnson) magnitude in the specified band of the source recorded in the corresponding FILTERMAG_VEGA parameter.

Bmag_Vega
This parameter contains the Vega (Johnson) magnitude of the source in the specified band calculated using the zero point magnitude (VZP) contained within the XMM CAL. The conversion from coincidence-corrected source count rate to Vega (Johnson) magnitude occurs through the standard logarithmic expression with filter-dependent, zero points: FILTERMAG_VEGA = VZP - 2.5log(FILTER_RATE).

Bmag_Vega_Error
The 1-sigma uncertainty determined for the Vega (Johnson) magnitude in the specified band of the source recorded in the corresponding FILTERMAG_VEGA parameter.

Vmag_Vega
This parameter contains the Vega (Johnson) magnitude of the source in the specified band calculated using the zero point magnitude (VZP) contained within the XMM CAL. The conversion from coincidence-corrected source count rate to Vega (Johnson) magnitude occurs through the standard logarithmic expression with filter-dependent, zero points: FILTERMAG_VEGA = VZP - 2.5log(FILTER_RATE).

Vmag_Vega_Error
The 1-sigma uncertainty determined for the Vega (Johnson) magnitude in the specified band of the source recorded in the corresponding FILTERMAG_VEGA parameter.

UVW2_Major_Axis
Using 1st order moment analysis, the size on the sky and ellipticity of sources is determined. This parameter records the full-width half-maximum (FWHM) in arcseconds of the source in the specified band along what is considered to be the long axis of the elliptical source. Note that not all sources in the sample are necessarily well-described by an ellipse.

UVM2_Major_Axis
Using 1st order moment analysis, the size on the sky and ellipticity of sources is determined. This parameter records the full-width half-maximum (FWHM) in arcseconds of the source in the specified band along what is considered to be the long axis of the elliptical source. Note that not all sources in the sample are necessarily well-described by an ellipse.

UVW1_Major_Axis
Using 1st order moment analysis, the size on the sky and ellipticity of sources is determined. This parameter records the full-width half-maximum (FWHM) in arcseconds of the source in the specified band along what is considered to be the long axis of the elliptical source. Note that not all sources in the sample are necessarily well-described by an ellipse.

U_Major_Axis
Using 1st order moment analysis, the size on the sky and ellipticity of sources is determined. This parameter records the full-width half-maximum (FWHM) in arcseconds of the source in the specified band along what is considered to be the long axis of the elliptical source. Note that not all sources in the sample are necessarily well-described by an ellipse.

B_Major_Axis
Using 1st order moment analysis, the size on the sky and ellipticity of sources is determined. This parameter records the full-width half-maximum (FWHM) in arcseconds of the source in the specified band along what is considered to be the long axis of the elliptical source. Note that not all sources in the sample are necessarily well-described by an ellipse.

V_Major_Axis
Using 1st order moment analysis, the size on the sky and ellipticity of sources is determined. This parameter records the full-width half-maximum (FWHM) in arcseconds of the source in the specified band along what is considered to be the long axis of the elliptical source. Note that not all sources in the sample are necessarily well-described by an ellipse.

UVW2_Minor_Axis
Using 1st order moment analysis, the size on the sky and ellipticity of sources is determined. This parameter records the full-width half-maximum (FWHM) in arcseconds of the source in the specified band along what is considered to be the short axis of the elliptical source. Note that not all sources in the sample are necessarily well-described by an ellipse.

UVM2_Minor_Axis
Using 1st order moment analysis, the size on the sky and ellipticity of sources is determined. This parameter records the full-width half-maximum (FWHM) in arcseconds of the source in the specified band along what is considered to be the short axis of the elliptical source. Note that not all sources in the sample are necessarily well-described by an ellipse

UVW1_Minor_Axis
Using 1st order moment analysis, the size on the sky and ellipticity of sources is determined. This parameter records the full-width half-maximum (FWHM) in arcseconds of the source in the specified band along what is considered to be the short axis of the elliptical source. Note that not all sources in the sample are necessarily well-described by an ellipse

U_Minor_Axis
Using 1st order moment analysis, the size on the sky and ellipticity of sources is determined. This parameter records the full-width half-maximum (FWHM) in arcseconds of the source in the specified band along what is considered to be the short axis of the elliptical source. Note that not all sources in the sample are necessarily well-described by an ellipse

B_Minor_Axis
Using 1st order moment analysis, the size on the sky and ellipticity of sources is determined. This parameter records the full-width half-maximum (FWHM) in arcseconds of the source in the specified band along what is considered to be the short axis of the elliptical source. Note that not all sources in the sample are necessarily well-described by an ellipse

V_Minor_Axis
Using 1st order moment analysis, the size on the sky and ellipticity of sources is determined. This parameter records the full-width half-maximum (FWHM) in arcseconds of the source in the specified band along what is considered to be the short axis of the elliptical source. Note that not all sources in the sample are necessarily well-described by an ellipse

UVW2_Position_Angle
The position angle on the sky in degrees subtended by the major axis of the source in the specified band and the direction of J2000 North. The angle increases as the axis rotates from north to east.

UVM2_Position_Angle
The position angle on the sky in degrees subtended by the major axis of the source in the specified band and the direction of J2000 North. The angle increases as the axis rotates from north to east.

UVW1_Position_Angle
The position angle on the sky in degrees subtended by the major axis of the source in the specified band and the direction of J2000 North. The angle increases as the axis rotates from north to east.

U_Position_Angle
The position angle on the sky in degrees subtended by the major axis of the source in the specified band and the direction of J2000 North. The angle increases as the axis rotates from north to east.

B_Position_Angle
The position angle on the sky in degrees subtended by the major axis of the source in the specified band and the direction of J2000 North. The angle increases as the axis rotates from north to east.

V_Position_Angle
The position angle on the sky in degrees subtended by the major axis of the source in the specified band and the direction of J2000 North. The angle increases as the axis rotates from north to east.

UVW2_Quality_Flags
Each source passes through an automatic screening process in order to isolate potential problems with either the location or brightness recorded within the catalog in the specified band. The results of these tests are stored in a Boolean sense (i.e passed or failed) within the 12-character string contained in this parameter. The meaning of each flag is summarized below, whereas a full description of the algorithms used to set the flags is presented in the Data Processing: Quality Flags documentation at http://www.mssl.ucl.ac.uk/www_astro/XMM-OM-SUSS/DataProcessingQualityFlags.shtml

The word 'source' below includes both the source and background extraction regions.

   Bit (Value)  Description

  bit 0 (value 1): source on a bad pixel
  bit 1 (value 2): source on a readout streak
  bit 2 (value 4): source on a smoke-ring
  bit 3 (value 8): source on a diffraction spike
  bit 4 (value 16): source affected by Mod-8 pattern
  bit 5 (value 32): source within the central enhancement
  bit 6 (value 64): source near a bright source
  bit 7 (value 128): source near the edge
  bit 8 (value 256): point source within an extended source
  bit 9 (value 512): weird source (bright pixel)
  bit 10 (value 1024): multiple exposure values within photometry aperture
  bit 11 (value 2048): the source is too bright (rate > 0.97 c/frame).
  

A source with FILTER_QUALITY_FLAGS = 'FFFFFFFFFFFF' passes all of the above tests. As an example, a source situated over a bad pixel, on a diffraction spike and at the edge of an image will have a parameter value of 'TFFTFFFTFFFF'.

UVM2_Quality_Flags
Each source passes through an automatic screening process in order to isolate potential problems with either the location or brightness recorded within the catalog in the specified band. The results of these tests are stored in a Boolean sense (i.e passed or failed) within the 12-character string contained in this parameter. The meaning of each flag is summarized below, whereas a full description of the algorithms used to set the flags is presented in the Data Processing: Quality Flags documentation at http://www.mssl.ucl.ac.uk/www_astro/XMM-OM-SUSS/DataProcessingQualityFlags.shtml

The word 'source' below includes both the source and background extraction regions.

   Bit (Value)  Description

  bit 0 (value 1): source on a bad pixel
  bit 1 (value 2): source on a readout streak
  bit 2 (value 4): source on a smoke-ring
  bit 3 (value 8): source on a diffraction spike
  bit 4 (value 16): source affected by Mod-8 pattern
  bit 5 (value 32): source within the central enhancement
  bit 6 (value 64): source near a bright source
  bit 7 (value 128): source near the edge
  bit 8 (value 256): point source within an extended source
  bit 9 (value 512): weird source (bright pixel)
  bit 10 (value 1024): multiple exposure values within photometry aperture
  bit 11 (value 2048): the source is too bright (rate > 0.97 c/frame).
  

A source with FILTER_QUALITY_FLAGS = 'FFFFFFFFFFFF' passes all of the above tests. As an example, a source situated over a bad pixel, on a diffraction spike and at the edge of an image will have a parameter value of 'TFFTFFFTFFFF'.

UVW1_Quality_Flags
Each source passes through an automatic screening process in order to isolate potential problems with either the location or brightness recorded within the catalog in the specified band. The results of these tests are stored in a Boolean sense (i.e passed or failed) within the 12-character string contained in this parameter. The meaning of each flag is summarized below, whereas a full description of the algorithms used to set the flags is presented in the Data Processing: Quality Flags documentation at http://www.mssl.ucl.ac.uk/www_astro/XMM-OM-SUSS/DataProcessingQualityFlags.shtml

The word 'source' below includes both the source and background extraction regions.

   Bit (Value)  Description

  bit 0 (value 1): source on a bad pixel
  bit 1 (value 2): source on a readout streak
  bit 2 (value 4): source on a smoke-ring
  bit 3 (value 8): source on a diffraction spike
  bit 4 (value 16): source affected by Mod-8 pattern
  bit 5 (value 32): source within the central enhancement
  bit 6 (value 64): source near a bright source
  bit 7 (value 128): source near the edge
  bit 8 (value 256): point source within an extended source
  bit 9 (value 512): weird source (bright pixel)
  bit 10 (value 1024): multiple exposure values within photometry aperture
  bit 11 (value 2048): the source is too bright (rate > 0.97 c/frame).
  

A source with FILTER_QUALITY_FLAGS = 'FFFFFFFFFFFF' passes all of the above tests. As an example, a source situated over a bad pixel, on a diffraction spike and at the edge of an image will have a parameter value of 'TFFTFFFTFFFF'.

U_Quality_Flags
Each source passes through an automatic screening process in order to isolate potential problems with either the location or brightness recorded within the catalog in the specified band. The results of these tests are stored in a Boolean sense (i.e passed or failed) within the 12-character string contained in this parameter. The meaning of each flag is summarized below, whereas a full description of the algorithms used to set the flags is presented in the Data Processing: Quality Flags documentation at http://www.mssl.ucl.ac.uk/www_astro/XMM-OM-SUSS/DataProcessingQualityFlags.shtml

The word 'source' below includes both the source and background extraction regions.

   Bit (Value)  Description

  bit 0 (value 1): source on a bad pixel
  bit 1 (value 2): source on a readout streak
  bit 2 (value 4): source on a smoke-ring
  bit 3 (value 8): source on a diffraction spike
  bit 4 (value 16): source affected by Mod-8 pattern
  bit 5 (value 32): source within the central enhancement
  bit 6 (value 64): source near a bright source
  bit 7 (value 128): source near the edge
  bit 8 (value 256): point source within an extended source
  bit 9 (value 512): weird source (bright pixel)
  bit 10 (value 1024): multiple exposure values within photometry aperture
  bit 11 (value 2048): the source is too bright (rate > 0.97 c/frame).
  

A source with FILTER_QUALITY_FLAGS = 'FFFFFFFFFFFF' passes all of the above tests. As an example, a source situated over a bad pixel, on a diffraction spike and at the edge of an image will have a parameter value of 'TFFTFFFTFFFF'.

B_Quality_Flags
Each source passes through an automatic screening process in order to isolate potential problems with either the location or brightness recorded within the catalog in the specified band. The results of these tests are stored in a Boolean sense (i.e passed or failed) within the 12-character string contained in this parameter. The meaning of each flag is summarized below, whereas a full description of the algorithms used to set the flags is presented in the Data Processing: Quality Flags documentation at http://www.mssl.ucl.ac.uk/www_astro/XMM-OM-SUSS/DataProcessingQualityFlags.shtml

The word 'source' below includes both the source and background extraction regions.

   Bit (Value)  Description

  bit 0 (value 1): source on a bad pixel
  bit 1 (value 2): source on a readout streak
  bit 2 (value 4): source on a smoke-ring
  bit 3 (value 8): source on a diffraction spike
  bit 4 (value 16): source affected by Mod-8 pattern
  bit 5 (value 32): source within the central enhancement
  bit 6 (value 64): source near a bright source
  bit 7 (value 128): source near the edge
  bit 8 (value 256): point source within an extended source
  bit 9 (value 512): weird source (bright pixel)
  bit 10 (value 1024): multiple exposure values within photometry aperture
  bit 11 (value 2048): the source is too bright (rate > 0.97 c/frame).
  

A source with FILTER_QUALITY_FLAGS = 'FFFFFFFFFFFF' passes all of the above tests. As an example, a source situated over a bad pixel, on a diffraction spike and at the edge of an image will have a parameter value of 'TFFTFFFTFFFF'.

V_Quality_Flags
Each source passes through an automatic screening process in order to isolate potential problems with either the location or brightness recorded within the catalog in the specified band. The results of these tests are stored in a Boolean sense (i.e passed or failed) within the 12-character string contained in this parameter. The meaning of each flag is summarized below, whereas a full description of the algorithms used to set the flags is presented in the Data Processing: Quality Flags documentation at http://www.mssl.ucl.ac.uk/www_astro/XMM-OM-SUSS/DataProcessingQualityFlags.shtml

The word 'source' below includes both the source and background extraction regions.

   Bit (Value)  Description

  bit 0 (value 1): source on a bad pixel
  bit 1 (value 2): source on a readout streak
  bit 2 (value 4): source on a smoke-ring
  bit 3 (value 8): source on a diffraction spike
  bit 4 (value 16): source affected by Mod-8 pattern
  bit 5 (value 32): source within the central enhancement
  bit 6 (value 64): source near a bright source
  bit 7 (value 128): source near the edge
  bit 8 (value 256): point source within an extended source
  bit 9 (value 512): weird source (bright pixel)
  bit 10 (value 1024): multiple exposure values within photometry aperture
  bit 11 (value 2048): the source is too bright (rate > 0.97 c/frame).
  

A source with FILTER_QUALITY_FLAGS = 'FFFFFFFFFFFF' passes all of the above tests. As an example, a source situated over a bad pixel, on a diffraction spike and at the edge of an image will have a parameter value of 'TFFTFFFTFFFF'.

UVW2_Extended_Flag
Sources which have spatial extents in the specified band consistent with the point spread function (PSF) of the detector are flagged with FILTER_EXTENDED_FLAG = 0. Sources with measured FWHM major-axes, FILTER_MAJOR_AXIS, greater than the calibrated PSF FWHM with > 3 sigma confidence are flagged with FILTER_EXTENDED_FLAG = 1. Calibrated PSF values for each filter are obtained from the XMM CAL.

UVM2_Extended_Flag
Sources which have spatial extents in the specified band consistent with the point spread function (PSF) of the detector are flagged with FILTER_EXTENDED_FLAG = 0. Sources with measured FWHM major-axes, FILTER_MAJOR_AXIS, greater than the calibrated PSF FWHM with > 3 sigma confidence are flagged with FILTER_EXTENDED_FLAG = 1. Calibrated PSF values for each filter are obtained from the XMM CAL.

UVW1_Extended_Flag
Sources which have spatial extents in the specified band consistent with the point spread function (PSF) of the detector are flagged with FILTER_EXTENDED_FLAG = 0. Sources with measured FWHM major-axes, FILTER_MAJOR_AXIS, greater than the calibrated PSF FWHM with > 3 sigma confidence are flagged with FILTER_EXTENDED_FLAG = 1. Calibrated PSF values for each filter are obtained from the XMM CAL.

U_Extended_Flag
Sources which have spatial extents in the specified band consistent with the point spread function (PSF) of the detector are flagged with FILTER_EXTENDED_FLAG = 0. Sources with measured FWHM major-axes, FILTER_MAJOR_AXIS, greater than the calibrated PSF FWHM with > 3 sigma confidence are flagged with FILTER_EXTENDED_FLAG = 1. Calibrated PSF values for each filter are obtained from the XMM CAL.

B_Extended_Flag
Sources which have spatial extents in the specified band consistent with the point spread function (PSF) of the detector are flagged with FILTER_EXTENDED_FLAG = 0. Sources with measured FWHM major-axes, FILTER_MAJOR_AXIS, greater than the calibrated PSF FWHM with > 3 sigma confidence are flagged with FILTER_EXTENDED_FLAG = 1. Calibrated PSF values for each filter are obtained from the XMM CAL.

V_Extended_Flag
Sources which have spatial extents in the specified band consistent with the point spread function (PSF) of the detector are flagged with FILTER_EXTENDED_FLAG = 0. Sources with measured FWHM major-axes, FILTER_MAJOR_AXIS, greater than the calibrated PSF FWHM with > 3 sigma confidence are flagged with FILTER_EXTENDED_FLAG = 1. Calibrated PSF values for each filter are obtained from the XMM CAL.


Contact Person

Questions regarding the XMMOMSUSS database table can be addressed to the HEASARC User Hotline.

Page Author: Browse Software Development Team
Last Modified: 13-Mar-2014