Browse
this table...

XMMCFRSCAT - XMM-Newton/Canada-France Redshift Survey Fields X-Ray Sources

HEASARC
Archive

Overview

This table contains the X-ray source catalogs for the XMM-Newton surveys of the 3 and 14 hours Right Ascension (hereafter 3-h and 14-h, respectively) fields from the Canada-France Redshift Survey. (These fields are also known as the Groth Strip). The X-ray sources cover the 0.5-10 keV flux range from ~2 x 10^-15 - 10^-13 erg/cm^2^/s. The authors have used a subset of the XMM-Newton sources, which have Chandra positions, to determine the best method of obtaining optical identifications of sources with only XMM-Newton positions. They have found optical identifications for 79% of the XMM-Newton sources for which there were deep optical images. The sources without optical identifications are likely to be optically fainter and have higher redshifts than the sources with identifications. The authors have estimated 'photometric redshifts' for the identified sources, calibrating their method using ~200 galaxies in the fields with spectroscopic redshifts. They find that the redshift distribution has a strong peak at z~0.7.

Catalog Bibcode

2004MNRAS.350..785W

References

XMM-Newton surveys of the Canada-France Redshift Survey fields -
II. The X-ray catalogues, the properties of the host galaxies and the redshift
distribution.
    Waskett T.J., Eales S.A., Gear W.K., McCracken H.J., Brodwin M., Nandra K.,
    Laird E.S., Lilly S.
   <Mon. Not. R. Astron. Soc., 350, 785-797 (2004)>
   =2004MNRAS.350..785W    (SIMBAD/NED BibCode)

Provenance

This table was created by the HEASARC in July 2005 based on CDS table J/MNRAS/350/785/tablea12.dat (the merged Tables A1 and A2 from the published paper).

HEASARC Implementation

The tabular material containing the optical counterparts information of these X-ray sources (the data given in Tables A3 - A6 in the published paper) is presented in the HEASARC Browse table called XMMCFRSOID, and can be also be accessed for any given X-ray source by clicking on the link labelled 'Optical' in the Related Links column on the query results page.

Parameters

Name
The X-ray source designation as recommended by the Dictionary of Nomenclature of Celestial Objects, using the prefix '[WEG2004] 3h ' for the 146 objects from the 3-h field and '[WEG2004] 14h ' for the 154 objects from the 14-h field, and a running number ordered by total number of counts detected in the full X-ray band, with the source with the greatest number being listed first. Due to vignetting, this order is approximately but not exactly the same as the order by X-ray flux.

Counts
The total counts in the full X-ray band for the source.

RA
The Right Ascension of the X-ray source in the selected equinox, as measured by the source detection software. This was given in J2000 equatorial coordinates to a precision of 0.00001 degrees in the original table.

Dec
The Declination of the X-ray source in the selected equinox, as measured by the source detection software. This was given in J2000 equatorial coordinates to a precision of 0.00001 degrees in the original table.

LII
The Galactic Longitude of the X-ray source.

BII
The Galactic Latitude of the X-ray source.

SB_Flux
The flux in the soft (0.5 - 2 keV) band, in erg/s/cm^2, as measured by the source detection software, and based on a photon index of 1.7.

SB_Flux_Error
The RMS uncertainty in the soft-band flux, in erg/s/cm^2.

HB_Flux
The flux in the hard (2 - 10 keV) band, in erg/s/cm^2, as measured by the source detection software, and based on a photon index of 1.7.

HB_Flux_Error
The RMS uncertainty in the hard-band flux, in erg/s/cm^2.

Flux
The flux in the total (0.5 - 10 keV) band, in erg/s/cm^2, as measured by the source detection software, and based on a photon index of 1.7.

Flux_Error
The RMS uncertainty in the total-band flux, in erg/s/cm^2.

PN_HR
The PN Camera hardness ratio HR, as given by the source detection procedure, where HR = (N(H)-N(S))/(N(H)+N(S)), and N(H) and N(S) are the counts observed for a source in the hard (2 - 10 keV) and soft (0.5 - 2 keV) bands, respectively, after correction for vignetting. Thus, higher values of the hardness ratio indicate a harder spectrum.

PN_HR_Error
The RMS uncertainty in the PN hardness ratio.

MOS1_HR
The MOS1 Camera hardness ratio HR, as given by the source detection procedure, where HR = (N(H)-N(S))/(N(H)+N(S)), and N(H) and N(S) are the counts observed for a source in the hard (2 - 10 keV) and soft (0.5 - 2 keV) bands, respectively, after correction for vignetting. Thus, higher values of the hardness ratio indicate a harder spectrum.

MOS1_HR_Error
The RMS uncertainty in the MOS1 hardness ratio.

MOS2_HR
The MOS2 Camera hardness ratio HR, as given by the source detection procedure, where HR = (N(H)-N(S))/(N(H)+N(S)), and N(H) and N(S) are the counts observed for a source in the hard (2 - 10 keV) and soft (0.5 - 2 keV) bands, respectively, after correction for vignetting. Thus, higher values of the hardness ratio indicate a harder spectrum.

MOS2_HR_Error
The RMS uncertainty in the MOS2 hardness ratio.

Notes
Codes for additional notes, as follows:

              -: lies outside Canada-France Deep Fields survey (CFDF) map
              c: lies within Chandra map (X-ray property)
              d: d = detected by Chandra (X-ray property)
              e: extended source (X-ray property)
              q: known QSO
              s: object with a stellar profile
              *: in 3h, sources 7 and 19 are in fact the same source split into
                  two owing to its lying on a PN chip gap
  

Contact Person

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

Page Author: Browse Software Development Team
Last Modified: 19-Jul-2005