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dc.contributor.authorBallo, Lucía-
dc.contributor.authorHeras, F. J. H.-
dc.contributor.authorBarcons, Xavier-
dc.contributor.authorCarrera, Francisco J.-
dc.date.accessioned2014-12-16T10:30:31Z-
dc.date.available2014-12-16T10:30:31Z-
dc.date.issued2012-
dc.identifierdoi: 10.1051/0004-6361/201117464-
dc.identifierissn: 0004-6361-
dc.identifiere-issn: 1432-0746-
dc.identifier.citationAstronomy and Astrophysics 545: A66 (2012)-
dc.identifier.urihttp://hdl.handle.net/10261/108766-
dc.description.abstract[Context]: X-ray emission from active galactic nuclei (AGN) is dominated by the accretion disk around a supermassive black hole. The radio luminosity, however, has not such a clear origin except in the most powerful sources where jets are evident. The origin (and even the very existence) of the local bi-modal distribution in radio-loudness is also a debated issue. [Aims]: By analysing X-ray, optical and radio properties of a large sample of type 1 AGN and quasars (QSOs) up to z > 2, where the bulk of this population resides, we aim to explore the interplay between radio and X-ray emission in AGN, in order to further our knowledge on the origin of radio emission, and its relation to accretion. [Methods]: We analyse a large (∼800 sources) sample of type 1 AGN and QSOs selected from the 2XMMi XMM-Newton X-ray source catalogue, cross-correlated with the SDSS DR7 spectroscopic catalogue, covering a redshift range from z ∼ 0.3 to z ∼ 2.3. Supermassive black hole masses are estimated from the Mg ii emission line, bolometric luminosities from the X-ray data, and radio emission or upper limits from the FIRST catalogue. [Results]: Most of the sources accrete close to the Eddington limit and the distribution in radio-loudness does not appear to have a bi-modal behaviour. We confirm that radio-loud AGN are also X-ray loud, with an X-ray-to-optical ratio up to twice that of radio-quiet objects, even excluding the most extreme strongly jetted sources. By analysing complementary radio-selected control samples, we find evidence that these conclusions are not an effect of the X-ray selection, but are likely a property of the dominant QSO population. [Conclusions]: Our findings are best interpreted in a context where radio emission in AGN, with the exception of a minority of beamed sources, arises from very close to the accretion disk and is therefore heavily linked to X-ray emission. We also speculate that the radio-loud/radio-quiet dichotomy might either be an evolutionary effect that developed well after the QSO peak epoch, or an effect of incompleteness in small samples. © ESO, 2012.-
dc.description.sponsorshipFunding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. L.B. acknowledges support from the Spanish Ministry of Science and Innovation through a “Juan de la Cierva” fellowship. Financial support for this work was provided by the Spanish Ministry of Economy and Competitiveness through research grant AYA2010-21490-C02-01 FJHH acknowledges support from CSIC through the undergraduate research programme “JAE-Introducción a la investigación”.-
dc.publisherEDP Sciences-
dc.relation.isversionofPublisher's version-
dc.rightsopenAccess-
dc.subjectGalaxies: active-
dc.subjectX-rays: galaxies-
dc.subjectQuasars: emission lines-
dc.subjectRadio continuum: galaxies-
dc.subjectQuasars: general-
dc.titleExploring X-ray and radio emission of type 1 AGN up to z ∼ 2.3-
dc.typeartículo-
dc.relation.publisherversionhttp://dx.doi.org/10.1051/0004-6361/201117464-
dc.date.updated2014-12-16T10:30:31Z-
dc.description.versionPeer Reviewed-
dc.language.rfc3066eng-
dc.contributor.funderAlfred P. Sloan Foundation-
dc.contributor.funderNational Science Foundation (US)-
dc.contributor.funderDepartment of Energy (US)-
dc.contributor.funderNational Aeronautics and Space Administration (US)-
dc.contributor.funderMinistry of Education, Culture, Sports, Science and Technology (Japan)-
dc.contributor.funderMax Planck Society-
dc.contributor.funderHigher Education Funding Council for England-
dc.contributor.funderMinisterio de Ciencia e Innovación (España)-
dc.contributor.funderMinisterio de Economía y Competitividad (España)-
dc.contributor.funderConsejo Superior de Investigaciones Científicas (España)-
dc.identifier.funderhttp://dx.doi.org/10.13039/100000879es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/100000001es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/100000104es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100001700es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100004189es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100000384es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100004837es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100003329es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100003339es_ES
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