XMMCDFS210 - XMM-Newton Deep Survey in the CDF-S 2-10 keV Source Catalog
X-ray sources were detected in the 3-Ms XMM-Newton observations of the Chandra Deep Field South. Source detection was done in two steps, first using the PWXDetect software, and then using emldetect. 339 Sources detected by both programs are presented in the main tables, while 74 sources only detected by PWXDetect are presented in the supplementary tables. The 2-10 and 5-10 keV bands were analyzed separately.
This HEASARC table contains the main sample of 339 sources detected in the 2-10 keV band in the XMM-CDFS survey. (The table of 5-10 keV XMM-CDFS sources is also available at the HEASARC as the XMMCDFS510 table). This table does not include the 74 supplementary sources which were detected only with PWXDetect. These supplementary sources were on average detected at low significance; many of them were on the borders of the FOV; and a few were in crowded fields where EMLDetect had trouble separating the different PSF components. Nevertheless, 4 of these sources were bright enough that a spectrum could be extracted.
The XMM-Newton deep survey in the Chandra Deep Field South. III. Point source catalogue and number counts in the hard X-rays. Ranalli P., Comastri A., Vignali C., Carrera F.J., Cappelluti N., Gilli R., Puccetti S., Brandt W.N., Brunner H., Brusa M., Georgantopoulos I., Iwasawa K., Mainieri V. <Astron. Astrophys. 555, A42 (2013)> =2013A&A...555A..42R (SIMBAD/NED BibCode)
A uniquely identifying source number for each 2 - 10 keV source in the catalog. Specifically, this is the PWXDetect source number. It is referred to as the ID210 parameter in the original reference.
The 2 - 10 keV source designation in the standard IAU-recommended position-based format, i.e., 'XMMCDFS JHHMMSS.s-DDMMSS', where the prefix stands for 'XMM-Newton survey in the Chandra Deep Field South' and the numerical string is based on the J2000.0 equatorial coordinates of the source.
The Right Ascension of the XMM-Newton 2-10 keV source in the selected equinox. This was given in J2000.0 decimal degree to a precision of 10-4 degrees (0.36 arcseconds) in the original tables.
The Declination of the XMM-Newton 2-10 keV source in the selected equinox. This was given in J2000.0 decimal degree to a precision of 10-4 degrees (0.36 arcseconds) in the original tables.
The Galactic Longitude of the XMM-Newton 2-10 keV source.
The Galactic Latitude of the XMM-Newton 2-10 keV source.
The 1-sigma uncertainty in the position of the XMM-Newton 2-10 keV source, in arcseconds.
The net source counts (summed MOS1, MOS2 and PN) in the 2-10 keV band as determined by EMLDetect.
The 1-sigma uncertainty in the source counts (summed MOS1, MOS2 and PN) in the 2-10 keV band.
The expected background counts as determined by EMLDetect, in counts arcsec-2.
The net count rate of the XMM-Newton source in the 2-10 keV band as determined by EMLDetect, in ct s-1.
The 1-sigma uncertainty in the count rate of the XMM-Newton source in the 2-10 keV band, in ct s-1.
The flux of the XMM-Newton source in the 2-10 keV band as determined by EMLDetect, in erg s-1 cm-2. The flux to count rate conversion factor CF was calculated for a power-law spectrum with a slope Gamma = 1.7 (Mainieri et al. 2007, ApJS, 172, 368); the value is 1.86 x 1011 counts cm-2 erg-11 for the 2-10 keV band. Had the authors used a different slope (for example, 1.4 or 2.0), the conversion factor would have differed by 8-9%. The Galactic column density in the CDF-S direction is 8 x 1019 cm-2, so that the 2-10 keV band flux is not significantly affected and no correction for Galactic absorption is needed.
The 1-sigma uncertainty in the flux of the XMM-Newton source in the 2-10 keV band as determined by EMLDetect, in erg s-1 cm-2.
The significance (number of sigma) of the 2-10 keV source detection from PWXDetect.
The detection likelihood of the 2-10 keV source (from EMLDetect).
The PWXDetect wavelet scale for the detection, in arcseconds.
The source number of the Chandra Counterpart. The original reference for the Chandra counterpart source number is specified in the ref_cxo_source_number parameter value.
The original reference for the Chandra counterpart source number, as follows
E: Lehmer et al., 2005 ApJS, 161, 21, [LBA2005] NNN in SIMBAD, (blank): Xue et al., 2011 ApJS, 195, 10, [XLB2011] NNN in SIMBAD.
The redshift of the source.
The reference code for the source of the quoted redshift. The meaning of these codes is as follows:
Value Bibcode Author(s) Comment 1 2004A&A...428.1043L Le Fevre et al. 2 2004ApJS..155..271S Szokoly et al. 3 2004ApJS..155...73Z Zheng et al. 4 2005A&A...437..883M Mignoli et al. 5 2007A&A...465.1099R Ravikumar et al. 6 2008A&A...478...83V Vanzella et al. 7 2009A&A...494..443P Popesso et al. 8 2009ApJ...693.1713T Treister et al. 9 2010A&A...512A..12B Balestra et al. 10 2010ApJS..191..124S Silverman et al. 11 2013A&A...549A..63K Kurk et al. 12 2012MNRAS.425.2116C Cooper et al. 13 2011ApJ...742....3R Rafferty et al. 14 2008ApJS..179...19L Luo et al. 15 Keck spectra (2007-2008): no formal publication yet 16 Keck spectra (2010): no formal publication yet 17 2005ApJS..161...21L Lehmer et al. 18 VLT spectra: no formal publication yet 19 VIMOS/GOODS 21 2010ApJS..189..270C Cardamone et al. 22 2013arXiv1303.5556G Georgantopoulos et al. 23 2012A&A...546A..84I Iwasawa et al. 24 2009ApJS..183..295T Taylor et al. 25 2012MNRAS.427..520C Coppin et al.
This flag parameter is set to 1 to indicate that the quoted value is a spectroscopic redshift, and to 0 if it is a photometric redshift, or no redshift value is available.
The counterpart XMM-Newton CDFS 5-10 keV Catalog source number (called ID510 in the reference paper) for the 2-10 keV source.
The exposure time for the source averaged over the three EPIC cameras, in seconds (converted by the HEASARC from the ks units used in the original table).
Notes concerning the source, mainly about source blends and counterparts.