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17 results on '"G. L. Granato"'

1. Machine learning to identify ICL and BCG in simulated galaxy clusters

Author

I Marini, S Borgani, A Saro, G Murante, G L Granato, C Ragone-Figueroa, G Taffoni, Marini, I, Borgani, S, Saro, A, Murante, G, L Granato, G, Ragone-Figueroa, C, and Taffoni, G

Subjects
methods: statistical, Cosmology and Nongalactic Astrophysics (astro-ph.CO), statistical [methods], FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, methods: data analysis, galaxies: stellar content, stellar content [galaxies], Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), data analysi [methods], Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Nowadays, Machine Learning techniques offer fast and efficient solutions for classification problems that would require intensive computational resources via traditional methods. We examine the use of a supervised Random Forest to classify stars in simulated galaxy clusters after subtracting the member galaxies. These dynamically different components are interpreted as the individual properties of the stars in the Brightest Cluster Galaxy (BCG) and IntraCluster Light (ICL). We employ matched stellar catalogues (built from the different dynamical properties of BCG and ICL) of 29 simulated clusters from the DIANOGA set to train and test the classifier. The input features are cluster mass, normalized particle cluster-centric distance, and rest-frame velocity. The model is found to correctly identify most of the stars, while the larger errors are exhibited at the BCG outskirt, where the differences between the physical properties of the two components are less obvious. We investigate the robustness of the classifier to numerical resolution, redshift dependence (up to $z=1$), and included astrophysical models. We claim that our classifier provides consistent results in simulations for $z 0.1$ \r200) is significantly affected by uncertainties in the classification process. In conclusion, this work suggests the importance of employing Machine Learning to speed up a computationally expensive classification in simulations., 19 pages, accepted to MNRAS

Published
2022

2. Comparison of star formation rates from Hα and infrared luminosity as seen byHerschel

Author

H. Domínguez Sánchez, M. Mignoli, F. Pozzi, F. Calura, A. Cimatti, C. Gruppioni, J. Cepa, M. Sánchez Portal, G. Zamorani, S. Berta, D. Elbaz, E. Le Floc'h, G. L. Granato, D. Lutz, R. Maiolino, F. Matteucci, P. Nair, R. Nordon, L. Pozzetti, L. Silva, J. Silverman, S. Wuyts, C. M. Carollo, T. Contini, J.-P. Kneib, O. Le Fèvre, S. J. Lilly, V. Mainieri, A. Renzini, M. Scodeggio, S. Bardelli, M. Bolzonella, A. Bongiorno, K. Caputi, G. Coppa, O. Cucciati, S. de la Torre, L. de Ravel, P. Franzetti, B. Garilli, A. Iovino, P. Kampczyk, C. Knobel, K. Kovač, F. Lamareille, J.-F. Le Borgne, V. Le Brun, C. Maier, B. Magnelli, R. Pelló, Y. Peng, E. Perez-Montero, E. Ricciardelli, L. Riguccini, M. Tanaka, L. A. M. Tasca, L. Tresse, D. Vergani, and E. Zucca

Subjects
Physics, Spiral galaxy, 010504 meteorology & atmospheric sciences, Star formation, Metallicity, Extinction (astronomy), Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Redshift, Galaxy, Luminosity, Space and Planetary Science, 0103 physical sciences, Emission spectrum, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract

We empirically test the relation between the SFR(LIR) derived from the infrared luminosity, LIR, and the SFR(Ha) derived from the Ha emission line luminosity using simple conversion relations. We use a sample of 474 galaxies at z = 0.06 - 0.46 with both Ha detection (from 20k zCOSMOS survey) and new far-IR Herschel data (100 and 160 {\mu}m). We derive SFR(Ha) from the Ha extinction corrected emission line luminosity. We find a very clear trend between E(B - V) and LIR that allows to estimate extinction values for each galaxy even if the Ha emission line measurement is not reliable. We calculate the LIR by integrating from 8 up to 1000 {\mu}m the SED that is best fitting our data. We compare SFR(Ha) with the SFR(LIR). We find a very good agreement between the two SFR estimates, with a slope of m = 1.01 \pm 0.03 in the SFR(LIR) vs SFR(Ha) diagram, a normalization constant of a = -0.08 \pm 0.03 and a dispersion of sigma = 0.28 dex.We study the effect of some intrinsic properties of the galaxies in the SFR(LIR)-SFR(Ha) relation, such as the redshift, the mass, the SSFR or the metallicity. The metallicity is the parameter that affects most the SFR comparison. The mean ratio of the two SFR estimators log[SFR(LIR)/SFR(Ha)] varies by approx. 0.6 dex from metal-poor to metal-rich galaxies (8.1 < log(O/H) + 12 < 9.2). This effect is consistent with the prediction of a theoretical model for the dust evolution in spiral galaxies. Considering different morphological types, we find a very good agreement between the two SFR indicators for the Sa, Sb and Sc morphologically classified galaxies, both in slope and normalization. For the Sd, irregular sample (Sd/Irr), the formal best-fit slope becomes much steeper (m = 1.62 \pm 0.43), but it is still consistent with 1 at the 1.5 sigma level, because of the reduced statistics of this sub-sample.

Published
2012
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3. The symbiosis between galaxies and SMBHs

Author

Andrea Lapi, G. L. Granato, L. Silva, and M. Cook

Subjects
Physics, Settore FIS/05 - Astronomia e Astrofisica, Star formation, Galaxy formation and evolution, Astronomy, Type-cD galaxy, Astrophysics, Galaxy merger, Interacting galaxy, Lenticular galaxy, Galaxy cluster, Galaxy
Published
2010

4. The molecular hydrogen explorer H2EX

Author

F. Boulanger, J. P. Maillard, P. Appleton, E. Falgarone, G. Lagache, B. Schulz, B. P. Wakker, A. Bressan, J. Cernicharo, V. Charmandaris, L. Drissen, G. Helou, T. Henning, T. L. Lim, E. A. Valentjin, A. Abergel, J. Le Bourlot, M. Bouzit, S. Cabrit, F. Combes, J. M. Deharveng, P. Desmet, H. Dole, C. Dumesnil, A. Dutrey, J. J. Fourmond, E. Gavila, R. Grangé, C. Gry, P. Guillard, S. Guilloteau, E. Habart, B. Huet, C. Joblin, M. Langer, Y. Longval, S. C. Madden, C. Martin, M. A. Miville-Deschênes, G. Pineau des Forêts, E. Pointecouteau, H. Roussel, L. Tresse, L. Verstraete, F. Viallefond, F. Bertoldi, J. Jorgensen, J. Bouwman, A. Carmona, O. Krause, A. Baruffolo, C. Bonoli, F. Bortoletto, L. Danese, G. L. Granato, C. Pernechele, R. Rampazzo, L. Silva, G. de Zotti, J. Pardo, M. Spaans, F. F. S. van der Tak, W. Wild, M. J. Ferlet, S. K. Ramsay Howat, M. D. Smith, B. Swinyard, G. S. Wright, G. Joncas, P. G. Martin, C. J. Davis, B. T. Draine, P. F. Goldsmith, A. K. Mainzer, P. Ogle, S. A. Rinehart, G. J. Stacey, A. G. G. M. Tielens, Institut d'astrophysique spatiale ( IAS ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Infrared Processing and Analysis Center ( IPAC ), California Institute of Technology ( CALTECH ), Laboratoire de Radioastronomie ( LRA ), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris ( FRDPENS ), Centre National de la Recherche Scientifique ( CNRS ) -École normale supérieure - Paris ( ENS Paris ) -Centre National de la Recherche Scientifique ( CNRS ) -École normale supérieure - Paris ( ENS Paris ), INAF - Osservatorio Astronomico di Padova ( OAPD ), Istituto Nazionale di Astrofisica ( INAF ), Centro de Investigaciones Biológicas ( CSIC ), Consejo Superior de Investigaciones Científicas [Spain] ( CSIC ), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique ( LERMA ), École normale supérieure - Paris ( ENS Paris ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université de Cergy Pontoise ( UCP ), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique ( CNRS ), D´epartement de Physique, de G´enie Physique et d'Optique and Observatoire du mont M´egantic, Université Laval, Max-Planck-Institut für Astronomie ( MPIA ), STFC Rutherford Appleton Laboratory ( RAL ), Science and Technology Facilities Council ( STFC ), Laboratoire d'Astrophysique de Marseille ( LAM ), Aix Marseille Université ( AMU ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National d'Etudes Spatiales ( CNES ) -Centre National de la Recherche Scientifique ( CNRS ), Dauphine Recherches en Management ( DRM ), Université Paris-Dauphine-Centre National de la Recherche Scientifique ( CNRS ), Observatoire aquitain des sciences de l'univers ( OASU ), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'Astrophysique de Bordeaux [Pessac] ( LAB ), Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux ( L3AB ), Thales Alenia Space, Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ), Centre d'étude spatiale des rayonnements ( CESR ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée ( DAPNIA ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Centro Nacional de Aceleradores, inconnu, Inconnu, Department of Mathematical Sciences, University of Bath, University of Bath [Bath], Max-Planck-Institut für Radioastronomie ( MPIFR ), Centre for Astrophysics and Planetary Science [Canterbury] ( CAPS ), University of Kent [Canterbury], Laboratoire des Lois de Comportement du Combustible ( LLCC ), Space Science and Technology Department [Didcot] ( RAL Space ), Science and Technology Facilities Council ( STFC ) -Science and Technology Facilities Council ( STFC ), National Center of Soybean Biotechnology, University of Missouri-Columbia, SRON Netherlands Institute for Space Research ( SRON ), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Infrared Processing and Analysis Center (IPAC), California Institute of Technology (CALTECH), Laboratoire de Radioastronomie (LRA), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Centro de Investigaciones Biológicas (CSIC), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Université Laval [Québec] (ULaval), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Dauphine Recherches en Management (DRM), Université Paris Dauphine-PSL-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Thales Alenia Space [Cannes], Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées, Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Max-Planck-Institut für Radioastronomie (MPIFR), Centre for Astrophysics and Planetary Science [Canterbury] (CAPS), Laboratoire de Modélisation Multi-échelles des Combustibles (LM2C), Service d'Etudes de Simulation du Comportement du combustibles (SESC), Département d'Etudes des Combustibles (DEC), CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Département d'Etudes des Combustibles (DEC), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Space Science and Technology Department [Didcot] (RAL Space), Science and Technology Facilities Council (STFC)-Science and Technology Facilities Council (STFC), University of Missouri [Columbia], University of Missouri System-University of Missouri System, SRON Netherlands Institute for Space Research (SRON), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, Université Paris sciences et lettres (PSL), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)

Subjects
Active galactic nucleus, Cosmic Vision, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Star formation, Galaxies, ISM, Disks, Astronomical instrumentation, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, symbols.namesake, Planet, Galaxy formation and evolution, Spectral resolution, Planck, Astrophysics::Galaxy Astrophysics, Physics, Molecular cloud, Astrophysics (astro-ph), Astronomy and Astrophysics, [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Galaxy, [ PHYS.ASTR.EP ] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU]Sciences of the Universe [physics], Space and Planetary Science, symbols, Astrophysics::Earth and Planetary Astrophysics
Abstract

The Molecular Hydrogen Explorer, H2EX, was proposed in response to the ESA 2015 - 2025 Cosmic Vision Call as a medium class space mission with NASA and CSA participations. The mission, conceived to understand the formation of galaxies, stars and planets from molecular hydrogen, is designed to observe the first rotational lines of the H2 molecule (28.2, 17.0, 12.3 and 9.7 micron) over a wide field, and at high spectral resolution. H2EX can provide an inventory of warm (> 100 K) molecular gas in a broad variety of objects, including nearby young star clusters, galactic molecular clouds, active galactic nuclei, local and distant galaxies. The rich array of molecular, atomic and ionic lines, as well as solid state features available in the 8 to 29 micron spectral range brings additional science dimensions to H2EX. We present the optical and mechanical design of the H2EX payload based on an innovative Imaging Fourier Transform Spectrometer (IFTS) fed by a 1.2m telescope. The 20'x20' field of view is imaged on two 1024x1024 Si:As detectors. The maximum resolution of 0.032 cm^-1 (FWHM) means a velocity resolution of 10 km s^-1 for the 0-0 S(3) line at 9.7 micron. This instrument offers the large field of view necessary to survey extended emission in the Galaxy and local Universe galaxies as well as to perform unbiased extragalactic and circumstellar disks surveys. The high spectral resolution makes H2EX uniquely suited to study the dynamics of H2 in all these environments. The mission plan is made of seven wide-field spectro-imaging legacy programs, from the cosmic web to galactic young star clusters, within a nominal two years mission. The payload has been designed to re-use the Planck platform and passive cooling design., Accepted for publication in Experimental Astronomy special issue on Cosmic Vision Proposals, 19 pages and 9 figures

Published
2009
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6. The European Large-Area ISO Survey (ELAIS): the final band-merged catalogue

Author

M. Rowan-Robinson, C. Lari, I. Perez-Fournon, E. A. Gonzalez-Solares, F. La Franca, M. Vaccari, S. Oliver, C. Gruppioni, P. Ciliegi, P. Héraudeau, S. Serjeant, A. Efstathiou, T. Babbedge, I. Matute, F. Pozzi, A. Franceschini, P. Vaisanen, A. Afonso-Luis, D. M. Alexander, O. Almaini, A. C. Baker, S. Basilakos, M. Barden, C. del Burgo, I. Bellas-Velidis, F. Cabrera-Guerra, R. Carballo, C. J. Cesarsky, D. L. Clements, H. Crockett, L. Danese, A. Dapergolas, B. Drolias, N. Eaton, E. Egami, D. Elbaz, D. Fadda, M. Fox, R. Genzel, P. Goldschmidt, J. I. Gonzalez-Serrano, M. Graham, G. L. Granato, E. Hatziminaoglou, U. Herbstmeier, M. Joshi, E. Kontizas, M. Kontizas, J. K. Kotilainen, D. Kunze, A. Lawrence, D. Lemke, M. J. D. Linden-Vørnle, R. G. Mann, I. Márquez, J. Masegosa, R. G. McMahon, G. Miley, V. Missoulis, B. Mobasher, T. Morel, H. Nørgaard-Nielsen, A. Omont, P. Papadopoulos, J.-L. Puget, D. Rigopoulou, B. Rocca-Volmerange, N. Sedgwick, L. Silva, T. Sumner, C. Surace, B. Vila-Vilaro, P. van der Werf, A. Verma, L. Vigroux, M. Villar-Martin, C. J. Willott, A. Carramiñana, R. Mujica, Universidad de Cantabria, Steward Observatory, University of Arizona, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, AUTRES, Space Telescope Science Institute (STSci), Science et Ingénierie des Matériaux et Procédés (SIMaP), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National Polytechnique de Grenoble (INPG)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Physics [Oxford], University of Oxford [Oxford], Centro de Fisica de Plasmas (GoLP), Instituto Superior Técnico, Universidade Técnica de Lisboa (IST), Imperial College London, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Oxford Astrophysics, Instituto de Astrofisica de Canarias (IAC), Dipartimento di Astronomia [Padova], Universita degli Studi di Padova, INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), Department of Physics and Astronomy [Milton Keynes], The Open University [Milton Keynes] (OU), Laboratoire de Physico-Chimie des Polymères et des Milieux Dispersés (PPMD), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de thermodynamique et physico-chimie métallurgiques (LTPCM), Institut National Polytechnique de Grenoble (INPG)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), University of Oxford, Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Padova = University of Padua (Unipd), Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National Polytechnique de Grenoble (INPG)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Department of Physics, Dipartimento di Astronomia, Université Pierre et Marie Curie - Paris 6 (UPMC)-ESPCI ParisTech-Centre National de la Recherche Scientifique (CNRS), Kapteyn Astronomical Institute, Rowan-Robinson M., Lari C., Perez-Fournon I., Gonzalez-Solares E. A., La Franca F., Vaccari M., Oliver S., Gruppioni C., Ciliegi P., Héraudeau P., Serjeant S., Efstathiou A., Babbedge T., Matute I., Pozzi F., Franceschini A., Vaisanen P., Afonso-Luis A., Alexander D. M., Almaini O., Baker A. C., Basilakos S., Barden M., del Burgo C., Bellas-Velidis I., Cabrera-Guerra F., Carballo R., Cesarsky C. J., Clements D. L., Crockett H., Danese L., Dapergolas A., Drolias B., Eaton N., Egami E., Elbaz D., Fadda D., Fox M., Genzel R., Goldschmidt P., Gonzalez-Serrano J. I., Graham M., Granato G. L., Hatziminaoglou E., Herbstmeier U., Joshi M., Kontizas E., Kontizas M., Kotilainen J. K., Kunze D., Lawrence A., Lemke D., Linden-Vørnle M. J. D., Mann R. G., Márquez I., Masegosa J., McMahon R. G., Miley G., Missoulis V., Mobasher B., Morel T., Nørgaard-Nielsen H., Omont A., Papadopoulos P., Puget J.-L., Rigopoulou D., Rocca-Volmerange B., Sedgwick N., Silva L., Sumner T., Surace C., Vila-Vilaro B., van der Werf P., Verma A., Vigroux L., Villar-Martin M., Willott C. J., Carramiñana A., and Mujica R.

Subjects
010504 meteorology & atmospheric sciences, galaxies : evolution, Infrared, galaxies: starburst, Astrophysics, HUBBLE-DEEP-FIELD, 01 natural sciences, X-RAY SURVEY, SOUTHERN FIELD, galaxies [Infrared], EXTRAGALACTIC SOURCE COUNTS, Astrophysics::Solar and Stellar Astrophysics, observations [Cosmology], 010303 astronomy & astrophysics, formation [Stars], Physics, infrared : galaxies, stars : formation, Astrophysics (astro-ph), STAR-FORMATION HISTORY, FORMATION RATES, cosmology : observations, Cirrus, galaxies : starburst, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, ACTIVE GALACTIC NUCLEI, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, infrared: galaxies, 0103 physical sciences, 170 MU-M, DATA REDUCTION, [INFO]Computer Science [cs], Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Luminous infrared galaxy, stars: formation, Spectral density, Astronomy and Astrophysics, Torus, Quasar, evolution [Galaxies], Redshift, Galaxy, starburst [Galaxies], Space and Planetary Science, cosmology: observations, HIGH-REDSHIFT, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

We present the final band-merged ELAIS catalogue at 6.7, 15, 90, and 175 $��$m, and the associated data at u,g,r,i,z,J,H,K, and 20cm. The origin of the survey, infrared and radio observations, data-reduction and optical identifications are briefly reviewed, and a summary of the area covered, and completeness limit for each infrared band is given. A detailed discussion of the band-merging and optical association strategy is given. The total catalogues consists of 2860 sources. For extragalactic sources observed in 3 or more infrared bands, colour-colour diagrams are presented and discussed in terms of the contributing infrared populations. Spectral energy distributions are shown for selected sources and compared with cirrus, M82 and Arp220 starburst, and AGN dust torus models. Spectroscopic redshifts are tabulated, where available. For the N1 and N2 areas, the INT ugriz Wide Field Survey, permits photometric redshifts to be estimated for galaxies and quasars. These agree well with the spectroscopic redshifts, within the uncertainty of the photometric method. The redshift distribution is given for selected ELAIS bands and colour-redshift diagrams are discussed. There is a high proportion of ultraluminous infrared galaxies in the ELAIS Catalogue ($> 10 %$ of 15 $��$m sources), many with Arp220-like colours. 10 hyperluminous infrared galaxies and 10 EROs are found in the survey. The large numbers of ultraluminous galaxies imply very strong evolution in the star-formation rate between z = 0 and 1., 21 pages, 31 figures. Accepted for publication in MNRAS

Published
2004
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7. The central dusty torus in the active nucleus of NGC 1068

Author

Helene Sol, Rainer Köhler, Olivier Chesneau, Julien Woillez, H. J. A. Röttgering, Klaus Meisenheimer, G. Weigelt, Andrea Richichi, P. T. de Zeeuw, Ch. Leinert, J.-W. Pel, Fabien Malbet, Guy Perrin, Annelie W. Glazenborg-Kluttig, Markus Schoeller, Didier Fraix-Burnet, George K. Miley, B. Heijligers, Walter Jaffe, Uwe Graser, L. B. F. M. Waters, Francesco Paresce, Frank Przygodda, G.-L. Granato, Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Max-Planck-Institut für Astronomie ( MPIA ), European Southern Observatory ( ESO ), Laboratoire d'Astrophysique de Grenoble ( LAOG ), Université Joseph Fourier - Grenoble 1 ( UJF ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Netherlands Institute for Radio Astronomy ( ASTRON ), INAF - Osservatorio Astronomico di Padova ( OAPD ), Istituto Nazionale di Astrofisica ( INAF ), Kapteyn Astronomical Institute ( KAPTEYN ASTRONOMICAL INSTITUTE ), Kapteyn Astronomical Institute, Observatoire de Paris - Site de Paris ( OP ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Centre National de la Recherche Scientifique ( CNRS ), Astronomical Institute Anton Pannekoek ( AI PANNEKOEK ), University of Amsterdam [Amsterdam] ( UvA ), Instituut voor Sterrenkunde ( INSTITUUT VOOR STERRENKUNDE ), Université Catholique de Louvain ( UCL ), Max-Planck-Institut für Radioastronomie ( MPIFR ), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, European Southern Observatory (ESO), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Netherlands Institute for Radio Astronomy (ASTRON), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Kapteyn Astronomical Institute [Groningen], University of Groningen [Groningen], Observatoire de Paris - Site de Paris (OP), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Instituut voor Sterrenkunde [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Max-Planck-Institut für Radioastronomie (MPIFR), and Low Energy Astrophysics (API, FNWI)

Subjects
INFRARED-SPECTRA, GALACTIC NUCLEI, Interferometry: optical, Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [ PHYS.ASTR.CO ] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 01 natural sciences, VLTI, Parsec, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysical jet, 0103 physical sciences, Emission spectrum, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Cosmic dust, Physics, Supermassive black hole, SPECTROSCOPY, Multidisciplinary, 010308 nuclear & particles physics, Astronomy, Torus, Galaxy, NGC 1068, Astrophysics::Earth and Planetary Astrophysics, EMISSION, Galaxies: AGN
Abstract

International audience; Active galactic nuclei (AGNs) display many energetic phenomena—broad emission lines, X-rays, relativistic jets, radio lobes—originating from matter falling onto a supermassive black hole. It is widely accepted that orientation effects play a major role in explaining the observational appearance of AGNs. Seen from certain directions, circum-nuclear dust clouds would block our view of the central powerhouse1,2. Indirect evidence suggests that the dust clouds form a parsec-sized torus-shaped distribution. This explanation, however, remains unproved, as even the largest telescopes have not been able to resolve the dust structures. Here we report interferometric mid-infrared observations that spatially resolve these structures in the galaxy NGC 1068. The observations reveal warm (320 K) dust in a structure 2.1 parsec thick and 3.4 parsec in diameter, surrounding a smaller hot structure. As such a configuration of dust clouds would collapse in a time much shorter than the active phase of the AGN3, this observation requires a continual input of kinetic energy to the cloud system from a source coexistent with the AGN.

Published
2004
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10. IR and X-Rays from IRASF10214+4724: A Hidden AGN?

Author

Luigi Danese, A. Franceschini, and G. L. Granato

Subjects
Physics, law, Bolometer, Radiative transfer, Flux, Astronomy, Spectral energy distribution, Astrophysics, Object (computer science), law.invention
Abstract

Under the assumption that a hidden AGN contributes a major part of the bolometric flux of the primeval object IRAS F10214+4724, we argue that sensitive X-ray observations would provide crucial information on the metal enriched gas present in the circumnuclear region.

Published
1996
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11. ON THE NATURE OF HYDROSTATIC EQUILIBRIUM IN GALAXY CLUSTERS.

Author

V. Biffi, S. Borgani, G. Murante, E. Rasia, S. Planelles, G. L. Granato, C. Ragone-Figueroa, A. M. Beck, M. Gaspari, and K. Dolag

Subjects
GALAXY clusters, HYDROSTATIC equilibrium, GALACTIC nuclei, GRAVITATION, RADIAL basis functions
Abstract

In this paper, we investigate the level of hydrostatic equilibrium (HE) in the intracluster medium of simulated galaxy clusters, extracted from state-of-the-art cosmological hydrodynamical simulations performed with the Smoothed-Particle-Hydrodynamic code GADGET-3. These simulations include several physical processes, among which are stellar and active galactic nucleus feedback, and have been performed with an improved version of the code that allows for a better description of hydrodynamical instabilities and gas mixing processes. Evaluating the radial balance between the gravitational and hydrodynamical forces via the gas accelerations generated, we effectively examine the level of HE in every object of the sample and its dependence on the radial distance from the center and on the classification of the cluster in terms of either cool-coreness or dynamical state. We find an average deviation of 10%–20% out to the virial radius, with no evident distinction between cool-core and non-cool-core clusters. Instead, we observe a clear separation between regular and disturbed systems, with a more significant deviation from HE for the disturbed objects. The investigation of the bias between the hydrostatic estimate and the total gravitating mass indicates that, on average, this traces the deviation from HE very well, even though individual cases show a more complex picture. Typically, in the radial ranges where mass bias and deviation from HE are substantially different, the gas is characterized by a significant amount of random motions (), relative to thermal ones. As a general result, the HE-deviation and mass bias, at a given distance from the cluster center, are not very sensitive to the temperature inhomogeneities in the gas. [ABSTRACT FROM AUTHOR]

Published
2016
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13. ARE THE BULK OF z > 2 HERSCHEL GALAXIES PROTO-SPHEROIDS?

Author

F. Pozzi, F. Calura, C. Gruppioni, G. L. Granato, G. Cresci, L. Silva, L. Pozzetti, F. Matteucci, and G. Zamorani

Subjects
STELLAR luminosity function, GALACTIC redshift, STELLAR mass, STAR formation, BANDWIDTH research
Abstract

We present a backward approach for the interpretation of the evolution of the near-IR and the far-IR luminosity functions (LFs) across the redshift range . In our method, late-type galaxies are treated by means of a parametric phenomenological method based on PEP/HerMES data up to z ∼ 4, whereas spheroids are described by means of a physically motivated backward model. The spectral evolution of spheroids is modeled by means of a single-mass model, associated with a present-day elliptical with a K-band luminosity comparable to the break of the local early-type LF. The formation of proto-spheroids is assumed to occurr across the redshift range . The key parameter is represented by the redshift at which half of all proto-spheroids are already formed. For this parameter, a statistical study indicates values between and . We assume as the fiducial value and show that this assumption allows us to describe accourately the redshift distributions and the source counts. By assuming at the far-IR flux limit of the PEP-COSMOS survey, the PEP-selected sources observed at can be explained as progenitors of local spheroids caught during their formation. We also test the effects of mass downsizing by dividing the spheroids into three populations of different present-day stellar masses. The results obtained in this case confirm the validity of our approach, i.e., that the bulk of proto-spheroids can be modeled by means of a single model that describes the evolution of galaxies at the break of the present-day early-type K-band LF. [ABSTRACT FROM AUTHOR]

Published
2015
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14. Characterizing diffused stellar light in simulated galaxy clusters

Author

G. De Lucia, Giuseppe Murante, Madhura Killedar, Stefano Borgani, Pierluigi Monaco, Klaus Dolag, Weiguang Cui, Gian Luigi Granato, V. Presotto, W., Cui, G., Murante, Monaco, Pierluigi, Borgani, Stefano, G. L., Granato, M., Killedar, G., De Lucia, V., Presotto, and K., Dolag

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Active galactic nucleus, formation [galaxies], Stellar mass, Metallicity, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, galaxies: clusters: general, galaxies: evolution, galaxies: formation, galaxies: statistics, galaxies: stellar content, cosmology: theory, Galaxy group, 0103 physical sciences, clusters: general [galaxies], statistic [galaxies], 010303 astronomy & astrophysics, evolution [galaxies], Astrophysics::Galaxy Astrophysics, Galaxy cluster, Physics, Supermassive black hole, theory [cosmology], 010308 nuclear & particles physics, Star formation, Astronomy, Astronomy and Astrophysics, stellar content [galaxies], Astrophysics - Astrophysics of Galaxies, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

[Abridged] In this paper, we carry out a detailed analysis of the performance of two different methods to identify the diffuse stellar light in cosmological hydrodynamical simulations of galaxy clusters. One method is based on a dynamical analysis of the stellar component. The second method is closer to techniques commonly employed in observational studies. Both the dynamical method and the method based on the surface brightness limit criterion are applied to the same set of hydrodynamical simulations for a large sample about 80 galaxy clusters. We find significant differences between the ICL and DSC fractions computed with the two corresponding methods, which amounts to about a factor of two for the AGN simulations, and a factor of four for the CSF set. We also find that the inclusion of AGN feedback boosts the DSC and ICL fractions by a factor of 1.5-2, respectively, while leaving the BCG+ICL and BCG+DSC mass fraction almost unchanged. The sum of the BCG and DSC mass stellar mass fraction is found to decrease from ~80 per cent in galaxy groups to ~60 per cent in rich clusters, thus in excess of what found from observational analysis. We identify the average surface brightness limits that yields the ICL fraction from the SBL method close to the DSC fraction from the dynamical method. These surface brightness limits turn out to be brighter in the CSF than in the AGN simulations. This is consistent with the finding that AGN feedback makes BCGs to be less massive and with shallower density profiles than in the CSF simulations. The BCG stellar component, as identified by both methods, are slightly older and more metal-rich than the stars in the diffuse component., 18 Pages, 15 figures. Matches to MNRAS published version

Published
2013
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15. Black hole accretion preferentially occurs in gas-rich galaxies

Author

Alberto Franceschini, P. Santini, Roberto Maiolino, F. Mannucci, Francesca Pozzi, Douglas Scott, Andrea Comastri, Fabio Vito, David J. Rosario, Dieter Lutz, Marcella Brusa, Cristian Vignali, Roberto Gilli, Carlotta Gruppioni, Duncan Farrah, Marco P. Viero, Gian Luigi Granato, Giovanni Cresci, F. Vito, R. Maiolino, P. Santini, M. Brusa, A. Comastri, G. Cresci, D. Farrah, A. Franceschini, R. Gilli, G. L. Granato, C. Gruppioni, D. Lutz, F. Mannucci, F. Pozzi, D. J. Rosario, D. Scott, M. Viero, and C. Vignali

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, FOS: Physical sciences, Astrophysics, macromolecular substances, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy merger, Disc galaxy, Peculiar galaxy, Astrophysics::Galaxy Astrophysics, Luminous infrared galaxy, Physics, Star formation, musculoskeletal, neural, and ocular physiology, Astronomy, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, nervous system, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Elliptical galaxy, Astrophysics::Earth and Planetary Astrophysics, methods: data analysi, galaxies: ISM, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We have investigated the gas content of a sample of several hundred AGN host galaxies at z$, Comment: Accepted for pubblication in MNRAS. 7 pages, 4 figures

Published
2014

16. Brightest cluster galaxies in cosmological simulations: achievements and limitations of active galactic nuclei feedback models

Author

Stefano Borgani, Giuseppe Murante, Weiguang Cui, C. Ragone-Figueroa, Gian Luigi Granato, C., Ragone Figueroa, G. L., Granato, G., Murante, Borgani, Stefano, and Cui, Weiguang

Subjects
Active galactic nucleus, NUMERICAL [METHODS], Ciencias Físicas, Astrophysics, 01 natural sciences, methods: numerical, cD, GENERAL [QUASARS], purl.org/becyt/ford/1 [https], quasars: general, HALOES [GALAXIES], 0103 physical sciences, Cluster (physics), galaxies: elliptical and lenticular, galaxies: evolution, galaxies: formation, galaxies: haloes, Brightest cluster galaxy, FORMATION [GALAXIES], 010303 astronomy & astrophysics, EVOLUTION [GALAXIES], Physics, 010308 nuclear & particles physics, haloe [galaxies], Astronomy, Astronomy and Astrophysics, purl.org/becyt/ford/1.3 [https], Galaxy, Astronomía, ELLIPTICAL AND LENTICULARS, CD [GALAXIES], Space and Planetary Science, elliptical and lenticular [galaxies], CIENCIAS NATURALES Y EXACTAS
Abstract

We analyse the basic properties of brightest cluster galaxies (BCGs) produced by state of the art cosmological zoom-in hydrodynamical simulations. These simulations have been run with different subgrid physics included. Here we focus on the results obtained with and without the inclusion of the prescriptions for supermassive black hole growth and of the ensuing active galactic nuclei (AGN) feedback. The latter process goes in the right direction of decreasing significantly the overall formation of stars. However, BCGs end up still containing too much stellar mass, a problem that increases with halo mass, and having an unsatisfactory structure. This is in the sense that their effective radii are too large, and that their density profiles feature a flattening on scales much larger than observed. We also find that our model of thermal AGN feedback has very little effect on the stellar velocity dispersions, which turn out to be very large. Taken together, these problems, which to some extent can be recognized also in other numerical studies typically dealing with smaller halo masses, indicate that on one hand present day subresolution models of AGN feedback are not effective enough in diminishing the global formation of stars in the most massive galaxies, but on the other hand they are relatively too effective in their centres. It is likely that a form of feedback generating large-scale gas outflows from BCGs precursors, and a more widespread effect over the galaxy volume, can alleviate these difficulties. Fil: Ragone Figueroa, Cinthia Judith. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina; Istituto Nazionale Di Astrofisica; Italia; Fil: Granato, Gian Luigi. Istituto Nazionale Di Astrofisica; Italia; Fil: Murante, Giuseppe. Istituto Nazionale Di Astrofisica; Italia; Fil: Borgani, Stefano. Istituto Nazionale Di Astrofisica; Italia; University of Trieste. Department of Physics. Astronomy Unit; Italia; Fil: Cui, Weiguang. Istituto Nazionale Di Astrofisica; Italia; University of Trieste. Department of Physics. Astronomy Unit; Italia

Published
2013

17. On the role of AGN feedback on the thermal and chemodynamical properties of the hot intra-cluster medium

Author

Gian Luigi Granato, Giuseppe Murante, Klaus Dolag, Madhura Killedar, D. Fabjan, S. Planelles, Stefano Borgani, C. Ragone-Figueroa, PLANELLES MIRA, Susana, Borgani, Stefano, D., Fabjan, Killedar, Madhura Akalank, G., Murante, G. L., Granato, C., Ragone Figueroa, and K., Dolag

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, methods: numerical, Intracluster medium, miscellaneou [cosmology], Radiative transfer, Cluster (physics), clusters: general [galaxies], Galaxy cluster, Astrophysics::Galaxy Astrophysics, Physics, Astronomy, numerical [methods], Astronomy and Astrophysics, galaxies: clusters: general, cosmology: miscellaneous, X-rays: galaxies, Redshift, galaxies [X-rays], Supernova, Stars, 13. Climate action, Space and Planetary Science, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present an analysis of the properties of the ICM in an extended set of cosmological hydrodynamical simulations of galaxy clusters and groups performed with the TreePM+SPH GADGET-3 code. Besides a set of non-radiative simulations, we carried out two sets of simulations including radiative cooling, star formation, metal enrichment and feedback from supernovae, one of which also accounts for the effect of feedback from AGN resulting from gas accretion onto super-massive black holes. These simulations are analysed with the aim of studying the relative role played by SN and AGN feedback on the general properties of the diffuse hot baryons in galaxy clusters and groups: scaling relations, temperature, entropy and pressure radial profiles, and ICM chemical enrichment. We find that simulations including AGN feedback produce scaling relations that are in good agreement with X-ray observations at all mass scales. However, our simulations are not able to account for the observed diversity between CC and NCC clusters: unlike for observations, we find that temperature and entropy profiles of relaxed and unrelaxed clusters are quite similar and resemble more the observed behaviour of NCC clusters. As for the pattern of metal enrichment, we find that an enhanced level of iron abundance is produced by AGN feedback with respect to the case of purely SN feedback. As a result, while simulations including AGN produce values of iron abundance in groups in agreement with observations, they over-enrich the ICM in massive clusters. The efficiency of AGN feedback in displacing enriched gas from halos into the inter-galactic medium at high redshift also creates a widespread enrichment in the outskirts of clusters and produces profiles of iron abundance whose slope is in better agreement with observations., 23 pages, 14 figures, 1 table, accepted for publication in MNRAS

Published
2013

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