XMMOMSUSS - XMM-Newton Optical Monitor Serendipitous UV Source Survey Catalog, v6.1

Overview

The 2023 release of the XMM OM Serendipitous Ultraviolet Source Survey (XMM-SUSS6.1) Catalog, a catalog of optical/UV sources detected by the Optical Monitor (OM) on-board the European Space Agency's (ESA's) XMM-Newton observatory, spans the period of observations from 2000 to November 2022. The data processing was performed at the European Space Astronomy Centre (ESAC, Madrid, Spain) using the XMM Science Analysis Software system (SAS) versions 18 and 19. In addition to covering a larger observation period, this sixth release reflects a change in philosophy with regard to the origin of the incorporated data. In previous releases, the data were generated via a bespoke processing of the OM Observation Data Files (ODFs) while in this new release, the catalog has been guided by the XMM user community and the authors have sought to harmonize the contents of the catalog with those of the OM data in the XMM-Newton Science Archive (XSA), which derive from the standard XMM-Newton pipeline processing system. While the bespoke processing and pipeline systems are fundamentally very similar, they are not identical and the differences lead to some differences in the output.

The number of observations (OBSIDs) included in the catalog is 12,057. The total number of entries in this release is 9,920,390. They correspond to 6,659,554 unique sources, of which 1,225,117 have multiple entries in the 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. The description of the previous release of the catalog can be found in Page M.J. et al. (2012, MNRAS, 426, 903).

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.

There is a second, related table which gives a summary of the observations from which the XMM-SUSS6.1 sources listed in this table have been detected and measured. That summary table is available at the HEASARC as the XMMOMSUOB table.

Catalog Bibcode

2012MNRAS.426..903P

References

The XMM-OM Serendipitous Ultraviolet Source Survey (SUSS) has been created at the European Space Astronomy Centre (ESAC, Madrid, Spain). The reference paper given below, notice, refers to release 1 of the SUSS. The documentation on the first release of this catalog is also available at http://www.mssl.ucl.ac.uk/www_astro/XMM-OM-SUSS/Summary.shtml.

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 sixth release of the XMM-OM SUSS catalog, XMM-SUSS6.1, released by ESA in October 2023, obtained from the XMM-Newton Science Archive (http://xmm.esac.esa.int/xsa), and ingested into the HEASARC database in October 2023. It is also available at the HEASARC as the gzipped FITS file https://heasarc.gsfc.nasa.gov/FTP/xmm/data/catalogues/XMM-OM-SUSS6-1.1.fits.gz.

Quality Flag Values for the XMM SUSS Catalog

Each source detected in a specific filter 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 a 13-character string contained in this parameter which has the following meaning (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 central enhancement
  bit 6 (value 64)    source near a bright source
  bit 7 (value 128)   source near an edge
  bit 8 (value 256)   point source within extended source
  bit 9 (value 512)   very bright pixel within photometry aperture
  bit 10 (value 1024) multiple exposure values within photometry aperture
  bit 11 (value 2048) source is affected by the reduced sensitivity patch (see known issues below)
  bit 12 (value 4096) source is too bright (rate > 0.97 c/frame).

A source with FILTER_QUALITY_FLAGS = 'FFFFFFFFFFFFF' 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 'TFFTFFFTFFFFF'.

Source on a bad pixel: An object is flagged bad if the photometric aperture used to sum source counts or background includes a bad pixel, as recorded in the Calibration Access Layer of the XMM-Newton Project. All of these pixels are already stored in the quality map and the information is simply propagated to the source table.

Source on a Readout streak: Readout streaks occur because there is no shutter to block incident photons during the finite time the CCD takes to readout. The exact deadtime is dependent on detector windowing. Streaks occur over a small number of pixel columns, but stretch across all rows of the image, which is the CCD clocking direction during readout. Readout streaks present two problems: (1) Very bright field sources will bias potentially both the flux and positions of neighboring sources encroaching upon the readout streak, (2) A readout streak may potentially generate spurious source detections.

Source on a Smoke Ring: A smoke ring is an out of focus ghost image of a bright star caused by internal reflection of light within the detector window. The smoke ring is displaced in the radial direction away from the primary image due to the curvature of the detector window. The detector window reflectivity reduces with increasing photon energy so smoke rings are less frequently seen in the UV filter images. Sources lying in or near a smoke ring might have the photometry compromised by the smoke ring.

Source on a Diffraction Spike: The secondary mirror support vanes give rise to diffraction spikes in the brightest sources which provide undesirable image structure around neighboring sources and generate spurious sources.

Source affected by Mod-8 pattern: Sources with count rates approaching 1 count per image frame are subject to coincidence loss, which distorts the PSF and gives rise to a modulo-8 pattern in the region surrounding the source. The morphologies of such sources cannot be recovered and hence they are flagged during construction of the catalogue. At very high count rates, coincidence loss leads to saturation and the photometry of sources cannot be recovered. Occasionally, sources approaching saturation can lose counts due to integer wrap-around in individual pixels of the raw data. Photometry of sources approaching the saturation limits should always be treated with caution.

Source within central enhancement: Diffuse light from the sky background reflecting off a chamfer in the detector window housing causes an ring of emission, enhanced by a factor of 2, in the center of the detector image. Sources within this region are flagged whether or not the background level is large enough to have a significant effect on the photometry. The reflectivity of the ring reduces with increasing photon energy so this is less prominent in the UV filter images.

Source near a bright source: The structure around bright sources can lead to spurious sources being detected.

Source near edge: Photometry and astrometry will be compromised if a source is partly outside the imaged area. Sources for which any part of the photometric aperture lies outside the field of view are flagged. Since images covering different areas and lying at different angles can be stacked together, there can be more sources affected by this flag than might be expected.

Source within an extended source: Photometry of point sources is complicated if they overlap an extended source because both source and background aperture will include some contribution from the extended source. If any pixel of the photometric aperture of a point source is shared by an extended source, then the point source is flagged.

Very bright pixel lies within photometry aperture: Indicates that the source has an isolated extremely bright pixel within the photometry aperture.

Multiple exposure values within photometry aperture: In the case of stacked images, parts of the image can be built up of more exposure time than other parts. Photometry and astrometry will be compromised if any part of the photometric aperture has a different exposure time. This can also occur if data has been lost or corrupted.

Source is affected by the reduced sensitivity patch: Following the accidental observation of Jupiter by the OM in July 2017, a small region of the photocathode, near the center of the OM field of view, has reduced sensitivity - this is referred to as the Jupiter patch (JP). Much of this region is currently identified via 'bad pixels' in the bad pixel calibration table, and sources that are detected within the bad pixel region are flagged as such in the catalog. However, the region of reduced sensitivity is larger than that currently translated into the bad pixel map and sources in the shallow wings of the JP, beyond the mapped bad pixel area, are not flagged. In fact, the wings of the JP include the location of the pn boresight in the OM image (i.e. where sources (generally, XMM-Newton targets), placed at the pn boresight, appear within the OM field of view). The impact of the sensitivity loss at the pn boresight is filter-dependent but ranges from about 8% in the V filter, to around 3% in the UV filters (see CAL-TN-0019.pdf) at the epoch of the Jupiter observation. The degradation at the pn boresight has since continued to decline, by about 1% per year in the V band.

Source is too bright: At very high count rates, coincidence loss leads to saturation and the photometry of sources cannot be recovered. Occasionally, sources approaching saturation can lose counts due to integer wraparound in individual pixels of the raw data. Photometry of sources approaching the saturation limits should always be treated with caution. The saturation limit has been set at 0.97 counts per frame. For these sources the rates, fluxes and magnitudes have been removed.

Parameters

Entry_Number
This parameter contains a HEASARC-created unique sequential identification number for each entry in the catalog.

Name
The IAU-designated source name in the 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-SUSS4.1 catalog. Please, note that the number of entries in this table is larger that the total number of individual sources in the catalog because some sources were observed more than once.

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 arcseconds. All fields included within the XMM-SUSS4.1 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 arcseconds. All fields included within the XMM-SUSS4.1 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 standard error in arcseconds attached to the merged source position, i.e., (1/n)* sqrt(sum from 1 to n of err_k²), where err_k are the position errors of the n individual sources. Please note that input errors from the individual source-list files are first converted from pixels to arcseconds.

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
The significance (signal-to-noise) of a source detection in the specified band, in sigma. If more than one exposure contributed to the source entry, these values are the averaged values from the individual sources that were merged.

UVM2_SNR
The significance (signal-to-noise) of a source detection in the specified band, in sigma. If more than one exposure contributed to the source entry, these values are the averaged values from the individual sources that were merged.

UVW1_SNR
The significance (signal-to-noise) of a source detection in the specified band, in sigma. If more than one exposure contributed to the source entry, these values are the averaged values from the individual sources that were merged.

U_SNR
The significance (signal-to-noise) of a source detection in the specified band, in sigma. If more than one exposure contributed to the source entry, these values are the averaged values from the individual sources that were merged.

B_SNR
The significance (signal-to-noise) of a source detection in the specified band, in sigma. If more than one exposure contributed to the source entry, these values are the averaged values from the individual sources that were merged.

V_SNR
The significance (signal-to-noise) of a source detection in the specified band, in sigma. If more than one exposure contributed to the source entry, these values are the averaged values from the individual sources that were merged.

UVW2_Rate
The background-subtracted source count rate in the specified band corrected for coincidence losses and detector time degradation, in counts per second. These values are the averaged values, without weighting, from the individual sources that were merged into a source.

UVW2_Rate_Error
The standard error in the background-subtracted source count rate in the specified band, in ct s^-1, i.e., (1/n)* sqrt(sum from 1 to n of err_k²), where err_k are the errors of the n individual sources.

UVM2_Rate
The background-subtracted source count rate in the specified band corrected for coincidence losses and detector time degradation, in counts per second. These values are the averaged values, without weighting, from the individual sources that were merged into a source.

UVM2_Rate_Error
The standard error in the background-subtracted source count rate in the specified band, in ct s^-1, i.e., (1/n)* sqrt(sum from 1 to n of err_k²), where err_k are the errors of the n individual sources.

UVW1_Rate
The background-subtracted source count rate in the specified band corrected for coincidence losses and detector time degradation, in counts per second. These values are the averaged values, without weighting, from the individual sources that were merged into a source.

UVW1_Rate_Error
The standard error in the background-subtracted source count rate in the specified band, in ct s^-1, i.e., (1/n)* sqrt(sum from 1 to n of err_k²), where err_k are the errors of the n individual sources.

U_Rate
The background-subtracted source count rate in the specified band corrected for coincidence losses and detector time degradation, in counts per second. These values are the averaged values, without weighting, from the individual sources that were merged into a source.

U_Rate_Error
The standard error in the background-subtracted source count rate in the specified band, in ct s^-1, i.e., (1/n)* sqrt(sum from 1 to n of err_k²), where err_k are the errors of the n individual sources.

B_Rate
The background-subtracted source count rate in the specified band corrected for coincidence losses and detector time degradation, in counts per second. These values are the averaged values, without weighting, from the individual sources that were merged into a source.

B_Rate_Error
The standard error in the background-subtracted source count rate in the specified band, in ct s^-1, i.e., (1/n)* sqrt(sum from 1 to n of err_k²), where err_k are the errors of the n individual sources.

V_Rate
The background-subtracted source count rate in the specified band corrected for coincidence losses and detector time degradation, in counts per second. These values are the averaged values, without weighting, from the individual sources that were merged into a source.

V_Rate_Error
The standard error in the background-subtracted source count rate in the specified band, in ct s^-1, i.e., (1/n)* sqrt(sum from 1 to n of err_k²), where err_k are the errors of the n individual sources.

UVW2_Flux
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 standard error in the flux of the source recorded in the corresponding band, in erg/cm²/s/Angstrom.

UVM2_Flux
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 standard error in the flux of the source recorded in the corresponding band, in erg/cm²/s/Angstrom.

UVW1_Flux
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 standard error in the flux of the source recorded in the corresponding band, in erg/cm²/s/Angstrom.

U_Flux
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 standard error in the flux of the source recorded in the corresponding band, in erg/cm²/s/Angstrom.

B_Flux
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 standard error in the flux of the source recorded in the corresponding band, in erg/cm²/s/Angstrom.

V_Flux
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 standard error in the flux of the source recorded in the corresponding band, in erg/cm²/s/Angstrom.

UVW2mag_AB
The AB magnitude of the source in the specified band computed from the averaged count rate in this filter.

UVW2mag_AB_Error
The standard error in the AB magnitude of the source recorded in the corresponding FILTERMAG_AB parameter.

UVM2mag_AB
The AB magnitude of the source in the specified band computed from the averaged count rate in this filter.

UVM2mag_AB_Error
The standard error in the AB magnitude of the source recorded in the corresponding FILTERMAG_AB parameter.

UVW1mag_AB
The AB magnitude of the source in the specified band computed from the averaged count rate in this filter.

UVW1mag_AB_Error
The standard error in the AB magnitude of the source recorded in the corresponding FILTERMAG_AB parameter.

Umag_AB
The AB magnitude of the source in the specified band computed from the averaged count rate in this filter.

Umag_AB_Error
The standard error in the AB magnitude of the source recorded in the corresponding FILTERMAG_AB parameter.

Bmag_AB
The AB magnitude of the source in the specified band computed from the averaged count rate in this filter.

Bmag_AB_Error
The standard error in the AB magnitude of the source recorded in the corresponding FILTERMAG_AB parameter.

Vmag_AB
The AB magnitude of the source in the specified band computed from the averaged count rate in this filter.

Vmag_AB_Error
The standard error in the AB magnitude of the source recorded in the corresponding FILTERMAG_AB parameter.

UVW2mag_Vega
The Vega (Johnson) magnitude of the source in the specified band computed from the averaged count rate in this filter.

UVW2mag_Vega_Error
The standard error in the Vega (Johnson) magnitude in the specified band of the source recorded in the corresponding FILTERMAG_VEGA parameter.

UVM2mag_Vega
The Vega (Johnson) magnitude of the source in the specified band computed from the averaged count rate in this filter.

UVM2mag_Vega_Error
The standard error in the Vega (Johnson) magnitude in the specified band of the source recorded in the corresponding FILTERMAG_VEGA parameter.

UVW1mag_Vega
The Vega (Johnson) magnitude of the source in the specified band computed from the averaged count rate in this filter.

UVW1mag_Vega_Error
The standard error in the Vega (Johnson) magnitude in the specified band of the source recorded in the corresponding FILTERMAG_VEGA parameter.

Umag_Vega
The Vega (Johnson) magnitude of the source in the specified band computed from the averaged count rate in this filter.

Umag_Vega_Error
The standard error in the Vega (Johnson) magnitude in the specified band of the source recorded in the corresponding FILTERMAG_VEGA parameter.

Bmag_Vega
The Vega (Johnson) magnitude of the source in the specified band computed from the averaged count rate in this filter.

Bmag_Vega_Error
The standard error in the Vega (Johnson) magnitude in the specified band of the source recorded in the corresponding FILTERMAG_VEGA parameter.

Vmag_Vega
The Vega (Johnson) magnitude of the source in the specified band computed from the averaged count rate in this filter.

Vmag_Vega_Error
The standard error in 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 13-character string contained in this parameter. The meaning of these flags is discussed in the "Quality Flag Values for the XMM SUSS Catalog" section above.

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 13-character string contained in this parameter. The meaning of these flags is discussed in the "Quality Flag Values for the XMM SUSS Catalog" section above.

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 13-character string contained in this parameter. The meaning of these flags is discussed in the "Quality Flag Values for the XMM SUSS Catalog" section above.

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 13-character string contained in this parameter. The meaning of these flags is discussed in the "Quality Flag Values for the XMM SUSS Catalog" section above.

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 13-character string contained in this parameter. The meaning of these flags is discussed in the "Quality Flag Values for the XMM SUSS Catalog" section above.

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 13-character string contained in this parameter. The meaning of these flags is discussed in the "Quality Flag Values for the XMM SUSS Catalog" section above.

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.

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.

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.

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.

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.

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.

UVW2_Sky_Image
For the specified filter, this parameter shows whether (if set to 1) or not (if set to null) the entry was derived from a summed exposure made by stacking sky images taken within the same observation.

UVM2_Sky_Image
For the specified filter, this parameter shows whether (if set to 1) or not (if set to null) the entry was derived from a summed exposure made by stacking sky images taken within the same observation.

UVW1_Sky_Image
For the specified filter, this parameter shows whether (if set to 1) or not (if set to null) the entry was derived from a summed exposure made by stacking sky images taken within the same observation.

U_Sky_Image
For the specified filter, this parameter shows whether (if set to 1) or not (if set to null) the entry was derived from a summed exposure made by stacking sky images taken within the same observation.

B_Sky_Image
For the specified filter, this parameter shows whether (if set to 1) or not (if set to null) the entry was derived from a summed exposure made by stacking sky images taken within the same observation.

V_Sky_Image
For the specified filter, this parameter shows whether (if set to 1) or not (if set to null) the entry was derived from a summed exposure made by stacking sky images taken within the same observation.

Contact Person

Questions regarding the XMMOMSUSS database table can be addressed to the HEASARC Help Desk.

Page Author: Browse Software Development Team
Last Modified: Monday, 16-Sep-2024 17:37:20 EDT