Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/23355
Campo DC | Valore | Lingua |
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dc.contributor.author | GRANATO, Gian Luigi | en_US |
dc.contributor.author | Ragone-Figueroa, Cinthia | en_US |
dc.contributor.author | Domínguez-Tenreiro, Rosa | en_US |
dc.contributor.author | Obreja, Aura | en_US |
dc.contributor.author | BORGANI, STEFANO | en_US |
dc.contributor.author | DE LUCIA, GABRIELLA | en_US |
dc.contributor.author | MURANTE, Giuseppe | en_US |
dc.date.accessioned | 2020-03-18T15:18:54Z | - |
dc.date.available | 2020-03-18T15:18:54Z | - |
dc.date.issued | 2015 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/23355 | - |
dc.description | We thank the referee Dave Clements for his constructive comments, which substantially helped to improve the quality of the paper. We acknowledge useful exchange of ideas and information with Gianfranco De Zotti, Herve Dole, Samuel Farrens, Chris Hayward, Paolo Tozzi and Joana Santos. GLG acknowledges warm hospitality by IATE-Córdoba during the development of this work. We thank Volker Springel for making available to us the non-public version of the gadget3 code. Simulations have been carried out at the CINECA supercomputing Centre in Bologna, with CPU time assigned through ISCRA proposals and through an agreement with University of Trieste. CRF 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-C03-03. | - |
dc.description.abstract | We 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 2 Mpc 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 mode. | en_US |
dc.language.iso | eng | en_US |
dc.title | The early phases of galaxy clusters formation in IR: coupling hydrodynamical simulations with GRASIL-3D | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/stv676 | en_US |
dc.identifier.scopus | 2-s2.0-84937895369 | en_US |
dc.identifier.isi | 000356338500013 | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article/450/2/1320/981344 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 450 | en_US |
dc.relation.issue | 2 | en_US |
dc.relation.firstpage | 1320 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2015MNRAS.450.1320G | en_US |
dc.description.apc | no | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegherò il file al passo 5-Carica) | en_US |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.fulltext | With Fulltext | - |
item.grantfulltext | open | - |
item.languageiso639-1 | en | - |
item.openairetype | Article | - |
item.cerifentitytype | Publications | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
crisitem.author.dept | O.A. Trieste | - |
crisitem.author.dept | O.A. Trieste | - |
crisitem.author.dept | O.A. Trieste | - |
crisitem.author.dept | O.A. Trieste | - |
crisitem.author.orcid | 0000-0002-4480-6909 | - |
crisitem.author.orcid | 0000-0001-6151-6439 | - |
crisitem.author.orcid | 0000-0002-6220-9104 | - |
crisitem.author.orcid | 0000-0002-5155-130X | - |
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