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dc.contributor.author Lagos Urbina, Claudia del Pilar
dc.contributor.author Padilla, Nelson David
dc.contributor.author Cora, Sofia Alejandra
dc.date.available 2018-04-20T14:08:38Z
dc.date.issued 2009-12
dc.identifier.citation Lagos Urbina, Claudia del Pilar; Padilla, Nelson David; Cora, Sofia Alejandra; Black hole spin and radio loudness in a LCDM universe; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 395; 12-2009; 625-636
dc.identifier.issn 0035-8711
dc.identifier.uri http://hdl.handle.net/11336/42804
dc.description.abstract We use a combination of a cosmological N-body simulation of the concordance cold dark matter paradigm and a semi-analytic model of galaxy formation to investigate the spin development of central supermassive black holes (BHs) and its relation to the BH host galaxy properties. In order to compute BH spins, we use the α model of Shakura & Sunyaev and consider the King et al. warped disc alignment criterion. The orientation of the accretion disc is inferred from the angular momentum of the source of accreted material, which bears a close relationship to the large-scale structure in the simulation. We find that the final BH spin depends almost exclusively on the accretion history and only weakly on the warped disc alignment. The main mechanisms of BH spin-up are found to be gas cooling processes and disc instabilities, a result that is only partially compatible with Monte Carlo models where the main spin-up mechanisms are major mergers and disc instabilities; the latter results are reproduced when implementing randomly oriented accretion discs in our model. Regarding the BH population, we find that more massive BHs, which are hosted by massive ellipticals, have higher spin values than less massive BHs, hosted by spiral galaxies. We analyse whether gas accretion rates and BH spins can be used as tracers of the radio loudness of active galactic nuclei (AGN). We find that the current observational indications of an increasing trend of radio-loud AGN fractions with stellar and BH mass can be easily obtained when placing lower limits on the BH spin, with a minimum influence from limits on the accretion rates; a model with random accretion disc orientations is unable to reproduce this trend. Our results favour a scenario where the BH spin is a key parameter to separate the radio-loud and radio-quiet galaxy populations.
dc.format application/pdf
dc.language.iso eng
dc.publisher Wiley Blackwell Publishing, Inc
dc.rights info:eu-repo/semantics/openAccess
dc.rights.uri https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.subject Galaxies
dc.subject Evolution of galaxies
dc.subject Formation of galaxies
dc.subject Active galaxies
dc.subject.classification Astronomía
dc.subject.classification Ciencias Físicas
dc.subject.classification CIENCIAS NATURALES Y EXACTAS
dc.title Black hole spin and radio loudness in a LCDM universe
dc.type info:eu-repo/semantics/article
dc.type info:ar-repo/semantics/artículo
dc.type info:eu-repo/semantics/publishedVersion
dc.date.updated 2018-04-19T18:31:30Z
dc.journal.volume 395
dc.journal.pagination 625-636
dc.journal.pais Reino Unido
dc.journal.ciudad Londres
dc.description.fil Fil: Lagos Urbina, Claudia del Pilar. Pontificia Universidad Católica de Chile; Chile
dc.description.fil Fil: Padilla, Nelson David. Pontificia Universidad Católica de Chile; Chile
dc.description.fil Fil: Cora, Sofia Alejandra. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
dc.journal.title Monthly Notices of the Royal Astronomical Society
dc.relation.alternativeid info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1111/j.1365-2966.2009.14451.x
dc.relation.alternativeid info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/395/2/625/993484
dc.conicet.fuente individual


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info:eu-repo/semantics/openAccess Excepto donde se diga explícitamente, este item se publica bajo la siguiente descripción: Creative Commons Attribution-NonCommercial-ShareAlike 2.5 Unported (CC BY-NC-SA 2.5)