Fossil group origins: V. the dependence of the luminosity function on the magnitude gap

Context. In nature we observe galaxy aggregations that span a wide range of magnitude gaps between the two first-ranked galaxies of a system (Δm12). Thus, there are systems with gaps close to zero (e.g., the Coma cluster), and at the other extreme of the distribution, the largest gaps are found amon...

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Autores: Zarattini, S., Aguerri, J. A. L., Sánchez-Janssen, R., Barrena, R., Boschin, W., del Burgo, C., Castro-Rodriguez, N., Corsini, E. M., D'Onghia, E., Girardi, M., Iglesias-Páramo, J., Kundert, A., Méndez-Abreu, J., Vílchez Medina, José Manuel
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2015
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/386402
Acceso en línea:http://hdl.handle.net/10261/386402
Access Level:acceso abierto
Palabra clave:Galaxies: clusters: general
Galaxies: groups: general
Galaxies: luminosity function, mass function
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network_name_str España
repository_id_str
dc.title.none.fl_str_mv Fossil group origins: V. the dependence of the luminosity function on the magnitude gap
title Fossil group origins: V. the dependence of the luminosity function on the magnitude gap
spellingShingle Fossil group origins: V. the dependence of the luminosity function on the magnitude gap
Zarattini, S.
Galaxies: clusters: general
Galaxies: groups: general
Galaxies: luminosity function, mass function
title_short Fossil group origins: V. the dependence of the luminosity function on the magnitude gap
title_full Fossil group origins: V. the dependence of the luminosity function on the magnitude gap
title_fullStr Fossil group origins: V. the dependence of the luminosity function on the magnitude gap
title_full_unstemmed Fossil group origins: V. the dependence of the luminosity function on the magnitude gap
title_sort Fossil group origins: V. the dependence of the luminosity function on the magnitude gap
dc.creator.none.fl_str_mv Zarattini, S.
Aguerri, J. A. L.
Sánchez-Janssen, R.
Barrena, R.
Boschin, W.
del Burgo, C.
Castro-Rodriguez, N.
Corsini, E. M.
D'Onghia, E.
Girardi, M.
Iglesias-Páramo, J.
Kundert, A.
Méndez-Abreu, J.
Vílchez Medina, José Manuel
author Zarattini, S.
author_facet Zarattini, S.
Aguerri, J. A. L.
Sánchez-Janssen, R.
Barrena, R.
Boschin, W.
del Burgo, C.
Castro-Rodriguez, N.
Corsini, E. M.
D'Onghia, E.
Girardi, M.
Iglesias-Páramo, J.
Kundert, A.
Méndez-Abreu, J.
Vílchez Medina, José Manuel
author_role author
author2 Aguerri, J. A. L.
Sánchez-Janssen, R.
Barrena, R.
Boschin, W.
del Burgo, C.
Castro-Rodriguez, N.
Corsini, E. M.
D'Onghia, E.
Girardi, M.
Iglesias-Páramo, J.
Kundert, A.
Méndez-Abreu, J.
Vílchez Medina, José Manuel
author2_role author
author
author
author
author
author
author
author
author
author
author
author
author
dc.contributor.none.fl_str_mv Ministerio de Economía y Competitividad (España)
European Research Council
Alfred P. Sloan Foundation
NASA
Junta de Andalucía
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Galaxies: clusters: general
Galaxies: groups: general
Galaxies: luminosity function, mass function
topic Galaxies: clusters: general
Galaxies: groups: general
Galaxies: luminosity function, mass function
description Context. In nature we observe galaxy aggregations that span a wide range of magnitude gaps between the two first-ranked galaxies of a system (Δm12). Thus, there are systems with gaps close to zero (e.g., the Coma cluster), and at the other extreme of the distribution, the largest gaps are found among the so-called fossil systems. The observed distribution of magnitude gaps is thought to be a consequence of the orbital decay of M. galaxies in massive halos and the associated growth of the central object. As a result, to first order the amplitude of this gap is a good statistical proxy for the dynamical age of a system of galaxies. Fossil and non-fossil systems could therefore have different galaxy populations that should be reflected in their luminosity functions. Aims. In this work we study, for the first time, the dependence of the luminosity function parameters on Δm12 using data obtained by the fossil group origins (FOGO) project. Methods. We constructed a hybrid luminosity function for 102 groups and clusters at z ≤ 0.25 using both photometric data from the SDSS-DR7 and redshifts from the DR7 and the FOGO surveys. The latter consists of ∼1200 new redshifts in 34 fossil system candidates. We stacked all the individual luminosity functions, dividing them into bins of Δm12, and studied their best-fit Schechter parameters. We additionally computed a i°relativei± luminosity function, expressed as a function of the central galaxy luminosity, which boosts our capacity to detect differences . especially at the bright end. Results. We find trends as a function of Δm12 at both the bright and faint ends of the luminosity function. In particular, at the bright end, the larger the magnitude gap, the fainter the characteristic magnitude M. The characteristic luminosity in systems with negligible gaps is more than a factor three brighter than in fossil-like ones. Remarkably, we also find differences at the faint end. In this region, the larger the gap, the flatter the faint-end slope 1á. Conclusions. The differences found at the bright end support a dissipationless, dynamical friction-driven merging model for the growth of the central galaxy in group-and cluster-sized halos. The differences in the faint end cannot be explained by this mechanism. Other processes . such as enhanced tidal disruption due to early infall and/or prevalence of eccentric orbits . may play a role. However, a larger sample of systems with Δm12 > 1.5 is needed to establish the differences at the faint end. © 2015 ESO.
publishDate 2015
dc.date.none.fl_str_mv 2015
2025
2025
2025
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
Publisher's version
info:eu-repo/semantics/publishedVersion
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/386402
url http://hdl.handle.net/10261/386402
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv #PLACEHOLDER_PARENT_METADATA_VALUE#
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info:eu-repo/grantAgreement/MINECO//AYA2013-43188-P
info:eu-repo/grantAgreement/MICINN//AYA2010-21887-C04-01
http://dx.doi.org/10.1051/0004-6361/201425506
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
dc.source.none.fl_str_mv reponame:DIGITAL.CSIC. Repositorio Institucional del CSIC
instname:Consejo Superior de Investigaciones Científicas (CSIC)
instname_str Consejo Superior de Investigaciones Científicas (CSIC)
reponame_str DIGITAL.CSIC. Repositorio Institucional del CSIC
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spelling Fossil group origins: V. the dependence of the luminosity function on the magnitude gapZarattini, S.Aguerri, J. A. L.Sánchez-Janssen, R.Barrena, R.Boschin, W.del Burgo, C.Castro-Rodriguez, N.Corsini, E. M.D'Onghia, E.Girardi, M.Iglesias-Páramo, J.Kundert, A.Méndez-Abreu, J.Vílchez Medina, José ManuelGalaxies: clusters: generalGalaxies: groups: generalGalaxies: luminosity function, mass functionContext. In nature we observe galaxy aggregations that span a wide range of magnitude gaps between the two first-ranked galaxies of a system (Δm12). Thus, there are systems with gaps close to zero (e.g., the Coma cluster), and at the other extreme of the distribution, the largest gaps are found among the so-called fossil systems. The observed distribution of magnitude gaps is thought to be a consequence of the orbital decay of M. galaxies in massive halos and the associated growth of the central object. As a result, to first order the amplitude of this gap is a good statistical proxy for the dynamical age of a system of galaxies. Fossil and non-fossil systems could therefore have different galaxy populations that should be reflected in their luminosity functions. Aims. In this work we study, for the first time, the dependence of the luminosity function parameters on Δm12 using data obtained by the fossil group origins (FOGO) project. Methods. We constructed a hybrid luminosity function for 102 groups and clusters at z ≤ 0.25 using both photometric data from the SDSS-DR7 and redshifts from the DR7 and the FOGO surveys. The latter consists of ∼1200 new redshifts in 34 fossil system candidates. We stacked all the individual luminosity functions, dividing them into bins of Δm12, and studied their best-fit Schechter parameters. We additionally computed a i°relativei± luminosity function, expressed as a function of the central galaxy luminosity, which boosts our capacity to detect differences . especially at the bright end. Results. We find trends as a function of Δm12 at both the bright and faint ends of the luminosity function. In particular, at the bright end, the larger the magnitude gap, the fainter the characteristic magnitude M. The characteristic luminosity in systems with negligible gaps is more than a factor three brighter than in fossil-like ones. Remarkably, we also find differences at the faint end. In this region, the larger the gap, the flatter the faint-end slope 1á. Conclusions. The differences found at the bright end support a dissipationless, dynamical friction-driven merging model for the growth of the central galaxy in group-and cluster-sized halos. The differences in the faint end cannot be explained by this mechanism. Other processes . such as enhanced tidal disruption due to early infall and/or prevalence of eccentric orbits . may play a role. However, a larger sample of systems with Δm12 > 1.5 is needed to establish the differences at the faint end. © 2015 ESO.We acknowledge the anonymous referee for the useful comments that helped us to improve the paper. This work has been partially funded by the MINECO (grant AIA2013-43188-P). This article is based on observations made with the Isaac Newton Telescope, Nordic Optical Telescope, and Telescopio Nazionale Galileo operated on the island of La Palma by the Isaac Newton Group, the Nordic Optical Telescope Scientific Association, and the Fundación Galileo Galilei of the INAF (Istituto Nazionale di Astrofísica), respectively, in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias. E.M.C. acknowledges financial support from Padua University by the grants 60A02-4807/12, 60A02-5857/13, 60A02-5833/14, and CPDA133894. M.G. acknowledges financial support from MIUR PRIN2010-2011. J.M.A. acknowledges support from the European Research Council Starting Grant (SEDmorph; P.I. V. Wild). E.D. gratefully acknowledges the support of the Alfred P. Sloan Foundation. E.D. and A.K. are supported by NASA Grant No NNX13AE97G. J.I.P. and J.M.V. acknowledge financial support from the Spanish MINECO under grant AYA2010-21887-C04-01 and from Junta de Andalucía Excellence Project PEX2011-FQM7058. Funding for the Sloan Digital Sky Survey (SDSS) and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, and the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium (ARC) for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, The University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, The Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington.EDP SciencesMinisterio de Economía y Competitividad (España)European Research CouncilAlfred P. Sloan FoundationNASAJunta de AndalucíaConsejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]2025202520152025info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionhttp://hdl.handle.net/10261/386402reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/MINECO//AYA2013-43188-Pinfo:eu-repo/grantAgreement/MICINN//AYA2010-21887-C04-01http://dx.doi.org/10.1051/0004-6361/201425506Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/3864022026-05-22T06:33:51Z
score 15,81155

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