The early phases of galaxy clusters formation in IR: Coupling hydrodynamical simulations with GRASIL-3D
EntityUAM. Departamento de Física Teórica
PublisherOxford University Press
10.1093/mnras/stv676Monthly Notices of the Royal Astronomical Society 450.2 (2015): 1320-1332
ISSN0035-8711 (print); 1365-2966 (online)
Funded byCRF 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
ProjectGobierno de España. AYA2009-12792-C03-03; Gobierno de España. AYA2012-31101; info:eu-repo/grantAgreement/EC/FP7/269264
SubjectsDust, extinction; Galaxies: clusters: general; Hydrodynamics; Infrared: galaxies; Radiative transfer; Submillimetre: galaxies; Física
NoteThis 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 reserved
Rights© 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
Esta obra está bajo una Licencia Creative Commons Atribución 4.0 Internacional.
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 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 mode
Google Scholar:Granato, Gian Luigi - Ragone-Figueroa, Cinthia - Domínguez Tenreiro, Rosa María - Obreja, Aura Catalina - Borgani, Stefano - De Lucia, Gabriella - Murante, Giuseppe
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