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dc.contributor.authorRanalli, Piero
dc.contributor.authorComastri, Andrea
dc.contributor.authorVignali, Cristian
dc.contributor.authorCarrera Troyano, Francisco Jesús 
dc.contributor.authorCappelluti, Nico
dc.contributor.authorGilli, Roberto
dc.contributor.authorPuccetti, Simonetta
dc.contributor.authorBrandt, William Nielsen
dc.contributor.authorBrunner, Hermann
dc.contributor.authorBrusa, Marcella
dc.contributor.authorGeorgantopoulos, Ioannis
dc.contributor.authorIwasawa, Kazushi
dc.contributor.authorMainieri, Vincenzo
dc.contributor.otherUniversidad de Cantabriaes_ES
dc.date.accessioned2013-12-26T12:40:30Z
dc.date.available2013-12-26T12:40:30Z
dc.date.issued2013-07
dc.identifier.issn0004-6361
dc.identifier.issn1432-0746
dc.identifier.urihttp://hdl.handle.net/10902/4092
dc.description.abstractNuclear obscuration plays a key role in the initial phases of AGN growth, yet not many highly obscured active galactic nuclei (AGN) are currently known beyond the local Universe, and their search is an active topic of research. The XMM-Newton survey in the Chandra Deep Field South (XMM-CDFS) aims at detecting and studying the spectral properties of a significant number of obscured and Compton-thick (NH ≳ 1024 cm-2) AGN. The large effective area of XMM-Newton in the 2–10 and 5–10 keV bands, coupled with a 3.45 Ms nominal exposure time (2.82 and 2.45 Ms after light curve cleaning for MOS and PN, respectively), allows us to build clean samples in both bands, and makes the XMM-CDFS the deepest XMM-Newton survey currently published in the 5–10 keV band. The large multi-wavelength and spectroscopic coverage of the CDFS area allows for an immediate and abundant scientific return. In this paper, we present the data reduction of the XMM-CDFS observations, the method for source detection in the 2–10 and 5–10 keV bands, and the resulting catalogues. A number of 339 and 137 sources are listed in the above bands with flux limits of 6.6 × 10-16 and 9.5 × 10-16 erg s-1 cm-2, respectively. The flux limits at 50% of the maximum sky coverage are 1.8 × 10-15 and 4.0 × 10-15 erg s-1 cm-2, respectively. The catalogues have been cross-correlated with the Chandra ones: 315 and 130 identifications have been found with a likelihood-ratio method, respectively. A number of 15 new sources, previously undetected by Chandra, is found; 5 of them lie in the 4 Ms area. Redshifts, either spectroscopic or photometric, are available for ~ 95% of the sources. The number counts in both bands are presented and compared to other works. The survey coverage has been calculated with the help of two extensive sets of simulations, one set per band. The simulations have been produced with a newly-developed simulator, written with the aim of the most careful reproduction of the background spatial properties. For this reason, we present a detailed decomposition of the XMM-Newton background into its components: cosmic, particle, and residual soft protons.The three components have different spatial distributions. The importance of these three components depends on the band and on the camera; the particle background is the most important one (80–90% of the background counts), followed by the soft protons (4–20%).es_ES
dc.format.extent22 p.es_ES
dc.language.isoenges_ES
dc.publisherEDP Scienceses_ES
dc.rights© ESO, 2013es_ES
dc.sourceAstronomy and Astrophysics, Vol. 555, Art. Num. A42 (2013)es_ES
dc.subject.otherCatalogses_ES
dc.subject.otherSurveyses_ES
dc.subject.otherGalaxies: activees_ES
dc.subject.otherMethods: data analysises_ES
dc.subject.otherX-rays: generales_ES
dc.titleThe XMM deep survey in the CDF-S III. Point source catalogue and number counts in the hard X-rayses_ES
dc.typeinfo:eu-repo/semantics/articlees_ES
dc.relation.publisherVersionhttp://dx.doi.org/10.1051/0004-6361/201321211es_ES
dc.rights.accessRightsopenAccesses_ES
dc.identifier.DOI10.1051/0004-6361/201321211
dc.type.versionpublishedVersiones_ES


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