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dc.contributor.authorGranato, Gian Luigi
dc.contributor.authorRagone-Figueroa, Cinthia
dc.contributor.authorDomínguez Tenreiro, Rosa María 
dc.contributor.authorObreja, Aura Catalina
dc.contributor.authorBorgani, Stefano
dc.contributor.authorDe Lucia, Gabriella
dc.contributor.authorMurante, Giuseppe
dc.contributor.otherUAM. Departamento de Física Teóricaes_ES
dc.date.accessioned2017-06-27T14:32:56Z
dc.date.available2017-06-27T14:32:56Z
dc.date.issued2015-04-10
dc.identifier.citationMonthly Notices of the Royal Astronomical Society 450.2 (2015): 1320-1332en_US
dc.identifier.issn0035-8711 (print)es_ES
dc.identifier.issn1365-2966 (online)es_ES
dc.identifier.urihttp://hdl.handle.net/10486/678792
dc.descriptionThis article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserveden_US
dc.description.abstractWe compute and study the infrared and sub-mm properties of high-redshift (z ≳ 1) simulated clusters and protoclusters. The results of a large set of hydrodynamical zoom-in simulations including active galactic nuclei (AGN) feedback, have been treated with the recently developed radiative transfer code GRASIL-3D, which accounts for the effect of dust reprocessing in an arbitrary geometry. Here, we have slightly generalized the code to adapt it to the present purpose. Then we have post-processed boxes of physical size 2Mpc encompassing each of the 24 most massive clusters identified at z = 0, at several redshifts between 0.5 and 3, producing IR and sub-mm mock images of these regions and spectral energy distributions (SEDs) of the radiation coming out from them. While this field is in its infancy from the observational point of view, rapid development is expected in the near future thanks to observations performed in the far-IR and sub-mm bands. Notably, we find that in this spectral regime our prediction are little affected by the assumption required by this post-processing, and the emission is mostly powered by star formation (SF) rather than accretion on to super massive black hole (SMBH). The comparison with the little observational information currently available, highlights that the simulated cluster regions never attain the impressive star formation rates suggested by these observations. This problem becomes more intriguing taking into account that the brightest cluster galaxies (BCGs) in the same simulations turn out to be too massive. It seems that the interplay between the feedback schemes and the star formation model should be revised, possibly incorporating a positive feedback modeen_US
dc.description.sponsorshipCRF acknowledges founding from the Consejo Nacional de Investigaciones Científicas y Técnicas de la República Argentina (CONICET), by the Secretaría de Ciencia y Técnica de la Universidad Nacional de Córdoba (SeCyT) and by the Fondo para la Investigación Científica y Tecnológica (FonCyT). This work has been supported by the PRIN-MIUR 201278X4FL Evolution of cosmic baryons funded by the Italian Ministry of Research, by the PRIN-INAF09 project Towards an Italian Network for Computational Cosmology, and by the INDARK INFN grant, by the MICINN and MINECO (Spain) through the grants AYA2009-12792-C03-03 and AYA2012-31101 from the PNAyA and by the European Commission’s Framework Program 7, through the International Research Staff Exchange Program LACEGAL.AO was financially supported through an FPI contract from AYA2009- 12792-C03-03en_US
dc.format.extent13 pag.es_ES
dc.format.mimetypeapplication/pdfen
dc.language.isoengen
dc.publisherOxford University Pressen_US
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen_US
dc.rights© 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Societyen_US
dc.subject.otherDust, extinctionen_US
dc.subject.otherGalaxies: clusters: generalen_US
dc.subject.otherHydrodynamicsen_US
dc.subject.otherInfrared: galaxiesen_US
dc.subject.otherRadiative transferen_US
dc.subject.otherSubmillimetre: galaxiesen_US
dc.titleThe early phases of galaxy clusters formation in IR: Coupling hydrodynamical simulations with GRASIL-3Den_US
dc.typearticleen
dc.subject.ecienciaFísicaes_ES
dc.relation.publisherversionhttp://dx.doi.org/10.1093/mnras/stv676es_ES
dc.identifier.doi10.1093/mnras/stv676es_ES
dc.identifier.publicationfirstpage1320es_ES
dc.identifier.publicationissue2es_ES
dc.identifier.publicationlastpage1332es_ES
dc.identifier.publicationvolume450es_ES
dc.relation.projectIDGobierno de España. AYA2009-12792-C03-03es_ES
dc.relation.projectIDGobierno de España. AYA2012-31101es_ES
dc.relation.projectIDinfo:eu-repo/grantAgreement/EC/FP7/269264es_ES
dc.type.versioninfo:eu-repo/semantics/publishedVersionen
dc.rights.ccReconocimientoes_ES
dc.rights.accessRightsopenAccessen
dc.authorUAMObreja , Aura Catalina (264543)
dc.facultadUAMFacultad de Ciencias


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