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dc.contributor.authorMateos, Silvia-
dc.contributor.authorCarrera, Francisco J.-
dc.contributor.authorPage, M. J.-
dc.contributor.authorWatson, M. G.-
dc.contributor.authorCorral, Amalia-
dc.contributor.authorTedds, J. A.-
dc.contributor.authorEbrero, Jacobo-
dc.contributor.authorKrumpe, M.-
dc.contributor.authorSchwope, A.-
dc.contributor.authorCeballos, María Teresa-
dc.date.accessioned2012-03-09T11:21:14Z-
dc.date.available2012-03-09T11:21:14Z-
dc.date.issued2010-02-
dc.identifier.citationAstronomy and Astrophysics 510: A35 (2010)es_ES
dc.identifier.issn0004-6361-
dc.identifier.urihttp://hdl.handle.net/10261/46852-
dc.description.abstract[Aims]: We discuss the broad band X-ray properties of one of the largest samples of X-ray selected type-1 AGN to date (487 objects in total), drawn from the XMM-Newton Wide Angle Survey (XWAS). The objects presented in this work cover 2-10 keV (rest-frame) luminosities from ~1042-1045 erg s-1 and are detected up to redshift ~4. We constrain the overall properties of the broad band continuum, soft excess and X-ray absorption, along with their dependence on the X-ray luminosity and redshift. We discuss the implications for models of AGN emission. [Methods]: We fitted the observed 0.2-12 keV broad band spectra with various models to search for X-ray absorption and soft excess. The F-test was used with a significance threshold of 99% to statistically accept the detection of additional spectral components. [Results]: We constrained the mean spectral index of the broad band X-ray continuum to (Γ) = 1.96 ± 0.02 with intrinsic dispersion (Γ) = 0.27 +o.01 -0.02. The continuum becomes harder at faint fluxes and at higher redshifts and hard (2-10 keV) luminosities. The dependence of Γ with flux is likely due to undetected absorption rather than to spectral variation. We found a strong dependence of the detection efficiency of objects on the spectral shape. We expect this effect to have an impact on the measured mean continuum shapes of sources at different redshifts and luminosities. We detected excess absorption in >~3% of our objects, with rest-frame column densities ~a few * 1022 cm-2. The apparent mismatch between the optical classification and X-ray properties of these objects is a challenge for the standard orientation-based AGN unification model. We found that the fraction of objects with detected soft excess is ~36%. Using a thermal model, we constrained the soft excess mean rest-frame temperature and intrinsic dispersion to kT ~ 100 eV and kT ~ 34 eV. The origin of the soft excess as thermal emission from the accretion disk or Compton scattered disk emission is ruled out on the basis of the temperatures detected and the lack of correlation of the soft excess temperature with the hard X-ray luminosity over more than 2 orders of magnitude in luminosity. Furthermore, the high luminosities of the soft excess rule out an origin in the host galaxy.es_ES
dc.description.sponsorshipSM, MW and JAT acknowledge support from the UK STFC research council. FJC acknowledges financial support for this work from the Spanish Ministerio de Educacion y Ciencia under project ESP2006-13608- C02-01. AC acknowledges financial support from the Spanish Ministerio de Educacion y Ciencia fellowship and also from the MIUR and The Italian Space Agency (ASI) grants PRIN−MUR 2006−02−5203 and n. I/088/06/0. MK acknowledges support from the NASA grant NNX08AX50G and NNX07AG02G.es_ES
dc.language.isoenges_ES
dc.publisherEDP Scienceses_ES
dc.relation.isversionofPublisher's version-
dc.rightsopenAccesses_ES
dc.subjectGalaxies: activees_ES
dc.subjectX-rays: galaxieses_ES
dc.subjectMethods: observationales_ES
dc.subjectSurveyses_ES
dc.titleThe XMM-Newton Wide Angle Survey (XWAS): the X-ray spectrum of type-1 AGNes_ES
dc.typeartículoes_ES
dc.identifier.doi10.1051/0004-6361/200913187-
dc.description.peerreviewedPeer reviewedes_ES
dc.relation.publisherversionhttp://dx.doi.org/10.1051/0004-6361/200913187es_ES
dc.identifier.e-issn1432-0746-
dc.contributor.funderNational Aeronautics and Space Administration (US)-
dc.contributor.funderMinisterio de Educación y Ciencia (España)-
dc.identifier.funderhttp://dx.doi.org/10.13039/100000104es_ES
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