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dc.contributor.authorMountrichas, G.-
dc.contributor.authorGeorgantopoulos, I.-
dc.contributor.authorOrdovás-Pascual, I.-
dc.contributor.authorCorral, Amalia-
dc.contributor.authorAkylas, A.-
dc.contributor.authorMateos, Silvia-
dc.contributor.authorCarrera, Francisco J.-
dc.contributor.authorBatziou, E.-
dc.date.accessioned2018-09-24T08:57:17Z-
dc.date.available2018-09-24T08:57:17Z-
dc.date.issued2017-
dc.identifierdoi: 10.1093/mnras/stx572-
dc.identifierissn: 0035-8711-
dc.identifiere-issn: 1365-2966-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society 468(3): 3042-3050 (2017)-
dc.identifier.urihttp://hdl.handle.net/10261/170078-
dc.description.abstractMid-infrared (IR) colour selection techniques have proved to be very efficient in finding active galactic nuclei (AGN). This is because the AGN heats the surrounding dust producing warm mid-IR colours. Using the Wide-field Infrared Survey Explorer 3.6, 4.5 and 12 μm colours, the largest sample of IR selected AGN has already been produced containing 1.4 million AGN over the whole sky. Here, we explore the X-ray properties of this AGN sample by cross-correlating it with the subsample of the 3XMM X-ray catalogue that has available X-ray spectra and at the same time optical spectroscopy from Sloan Digital Sky Survey (SDSS). Our goal is to find rare luminous obscured AGN. Our final sample contains 65 QSOs with log νLν ≥ 46.2 erg s−1. This IR luminosity cut corresponds to log  LX ≈ 45 erg s−1, at the median redshift of our sample (z = 2.3), that lies at the bright end of the X-ray luminosity function at z > 2. The X-ray spectroscopic analysis reveals seven obscured AGN having a column density NH > 1022 cm−2. Six of them show evidence for broad [C IV] absorption lines and five are classified as broad absorption line QSOs. We fit the optical spectra of our X-ray absorbed sources to estimate the optical reddening. We find that none of these show any obscuration according to the optical continuum. These sources add to the growing evidence for populations of luminous QSOs with evidence for substantial absorption by outflowing ionized material, similar to those expected to be emerging from their absorbing cocoons in the framework of AGN/galaxy co-evolution.-
dc.description.sponsorshipThe research leading to these results has received funding from the European Union’s Horizon 2020 Programme under the AHEAD project (grant agreement no. 654215). GM acknowledges financial support from the AHEAD project that is funded by the European Union as Research and Innovation Action under Grant no. 654215. FJC and IO-P acknowledge financial support through grant AYA2015-64346-C2-1-P (MINECO/FEDER). SM acknowledges financial support by the Spanish Ministry of Economy and Competitiveness through Grant no. AYA2016-76730-P. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the US Department of Energy Office of Science.-
dc.publisherRoyal Astronomical Society-
dc.publisherOxford University Press-
dc.relationMINECO/ICTI2013-2016/AYA2015-64346-C2-1-P-
dc.relationMINECO/ICTI2013-2016/AYA2016-76730-P-
dc.relationinfo:eu-repo/grantAgreement/EC/H2020/654215-
dc.relation.isversionofPublisher's version-
dc.rightsopenAccess-
dc.subjectBlack hole physics-
dc.subjectGalaxies: Seyfert-
dc.subjectGalaxies: haloes-
dc.subjectQuasars: general-
dc.subjectGalaxies: active-
dc.titleSearching for luminous absorbed sources in the WISE AGN catalogue-
dc.typeartículo-
dc.relation.publisherversionhttps://doi.org/10.1093/mnras/stx572-
dc.date.updated2018-09-24T08:57:18Z-
dc.description.versionPeer Reviewed-
dc.language.rfc3066eng-
dc.contributor.funderEuropean Commission-
dc.contributor.funderNational Science Foundation (US)-
dc.contributor.funderAlfred P. Sloan Foundation-
dc.contributor.funderMinisterio de Economía y Competitividad (España)-
dc.contributor.funderDepartment of Energy (US)-
dc.relation.csic-
dc.identifier.funderhttp://dx.doi.org/10.13039/501100003329es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/100000879es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100000780es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/100000001es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/100000015es_ES
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