The evolution of the mass-size relation for early-type galaxies from z~1 to the present: Dependence on environment, mass range and detailed morphology

We study the dependence of the galaxy size evolution on morphology, stellar mass and largescale environment for a sample of 298 group and 384 field quiescent early-type galaxies from the COSMOS survey, selected from z1 to the present, and with masses log(M/M) 10.5. From a detailed morphological anal...

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Autores: Huertas-Company, M., Mei, S., Shankar, F., Delaye, L., Raichoor, A., Covone, G., Finoguenov, A., Kneib, J. P., Le F'evre, O., Povic, M.
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2013
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/408319
Acceso en línea:http://hdl.handle.net/10261/408319
Access Level:acceso abierto
Palabra clave:Cd-galaxies: evolution
Galaxies: elliptical and lenticular
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spelling The evolution of the mass-size relation for early-type galaxies from z~1 to the present: Dependence on environment, mass range and detailed morphologyHuertas-Company, M.Mei, S.Shankar, F.Delaye, L.Raichoor, A.Covone, G.Finoguenov, A.Kneib, J. P.Le F'evre, O.Povic, M.Cd-galaxies: evolutionGalaxies: elliptical and lenticularWe study the dependence of the galaxy size evolution on morphology, stellar mass and largescale environment for a sample of 298 group and 384 field quiescent early-type galaxies from the COSMOS survey, selected from z1 to the present, and with masses log(M/M) 10.5. From a detailed morphological analysis we infer that 80 per cent of passive galaxies with mass log(M/M) 10.5 have an early-type morphology and that this fraction does not evolve over the last 6 Gyr. However, the relative abundance of lenticular and elliptical galaxies depends on stellarmass. Elliptical galaxies dominate only at the very high mass end - log(M/M) 11 - while S0 galaxies dominate at lower stellar masses - 10.5 log(M/M) 11. The galaxy size growth depends on galaxy mass range and early-type galaxy morphology, e.g. elliptical galaxies evolve differently than lenticular galaxies. At the low-mass end - 10.5 log(M/M) 11 - ellipticals do not show strong size growth from z 1 to the present (10 to 30 per cent depending on the morphological classification). On the other end, massive ellipticals - log(M/M) 11.2 - approximately doubled their size. Interestingly, lenticular galaxies display different behaviour: they appear more compact on average and they do show a size growth of 60 per cent since z = 1 independent of stellar mass range. We compare our results with state-of-the art semi-analytic models. While major and minor mergers can account for most of the galaxy size growth, we find that with present data and the theoretical uncertainties in the modelling we cannot state clear evidence favouring either merger or mass-loss via quasar and/or stellar winds as the primary mechanism driving the evolution. The galaxy mass-size relation and size growth do not depend on environment in the halo mass range explored in this work (field to group mass log(Mh/M) 14), i.e. group and field galaxies follow the same trends. At low redshift, where we examine both Sloan Digital Sky Survey and COSMOS groups, this result is at variance with predictions from some current hierarchical models that show a clear dependence of size growth on halo mass for massive ellipticals (log(M/M) 11.2). In future work, we will analyse in detail if this result is specific of the observations and model used in this work. Brightest Cluster Galaxies (BCG) and satellite galaxies lie on the same mass-size relation, at variance with predictions from hierarchical models, which predict that BCGs should have larger sizes than satellites because they experience more mergers in groups over the halo mass range probed. 2012 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. © 2012 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.The authors thank Boris H¨auβler for his great help with GALAPAGOS and M.R. George for putting together the main catalogue used in this paper. We are also thankful to P. Capak, O. Ilbert as well as to K. Bundy and A. Leauthaud for interesting discussions. FS acknowledges support from a Marie Curie grant.Oxford University PressEuropean CommissionConsejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]2025202520132025info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionhttp://hdl.handle.net/10261/408319reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)http://dx.doi.org/10.1093/mnras/sts150Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/4083192026-05-22T06:33:51Z
dc.title.none.fl_str_mv The evolution of the mass-size relation for early-type galaxies from z~1 to the present: Dependence on environment, mass range and detailed morphology
title The evolution of the mass-size relation for early-type galaxies from z~1 to the present: Dependence on environment, mass range and detailed morphology
spellingShingle The evolution of the mass-size relation for early-type galaxies from z~1 to the present: Dependence on environment, mass range and detailed morphology
Huertas-Company, M.
Cd-galaxies: evolution
Galaxies: elliptical and lenticular
title_short The evolution of the mass-size relation for early-type galaxies from z~1 to the present: Dependence on environment, mass range and detailed morphology
title_full The evolution of the mass-size relation for early-type galaxies from z~1 to the present: Dependence on environment, mass range and detailed morphology
title_fullStr The evolution of the mass-size relation for early-type galaxies from z~1 to the present: Dependence on environment, mass range and detailed morphology
title_full_unstemmed The evolution of the mass-size relation for early-type galaxies from z~1 to the present: Dependence on environment, mass range and detailed morphology
title_sort The evolution of the mass-size relation for early-type galaxies from z~1 to the present: Dependence on environment, mass range and detailed morphology
dc.creator.none.fl_str_mv Huertas-Company, M.
Mei, S.
Shankar, F.
Delaye, L.
Raichoor, A.
Covone, G.
Finoguenov, A.
Kneib, J. P.
Le F'evre, O.
Povic, M.
author Huertas-Company, M.
author_facet Huertas-Company, M.
Mei, S.
Shankar, F.
Delaye, L.
Raichoor, A.
Covone, G.
Finoguenov, A.
Kneib, J. P.
Le F'evre, O.
Povic, M.
author_role author
author2 Mei, S.
Shankar, F.
Delaye, L.
Raichoor, A.
Covone, G.
Finoguenov, A.
Kneib, J. P.
Le F'evre, O.
Povic, M.
author2_role author
author
author
author
author
author
author
author
author
dc.contributor.none.fl_str_mv European Commission
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Cd-galaxies: evolution
Galaxies: elliptical and lenticular
topic Cd-galaxies: evolution
Galaxies: elliptical and lenticular
description We study the dependence of the galaxy size evolution on morphology, stellar mass and largescale environment for a sample of 298 group and 384 field quiescent early-type galaxies from the COSMOS survey, selected from z1 to the present, and with masses log(M/M) 10.5. From a detailed morphological analysis we infer that 80 per cent of passive galaxies with mass log(M/M) 10.5 have an early-type morphology and that this fraction does not evolve over the last 6 Gyr. However, the relative abundance of lenticular and elliptical galaxies depends on stellarmass. Elliptical galaxies dominate only at the very high mass end - log(M/M) 11 - while S0 galaxies dominate at lower stellar masses - 10.5 log(M/M) 11. The galaxy size growth depends on galaxy mass range and early-type galaxy morphology, e.g. elliptical galaxies evolve differently than lenticular galaxies. At the low-mass end - 10.5 log(M/M) 11 - ellipticals do not show strong size growth from z 1 to the present (10 to 30 per cent depending on the morphological classification). On the other end, massive ellipticals - log(M/M) 11.2 - approximately doubled their size. Interestingly, lenticular galaxies display different behaviour: they appear more compact on average and they do show a size growth of 60 per cent since z = 1 independent of stellar mass range. We compare our results with state-of-the art semi-analytic models. While major and minor mergers can account for most of the galaxy size growth, we find that with present data and the theoretical uncertainties in the modelling we cannot state clear evidence favouring either merger or mass-loss via quasar and/or stellar winds as the primary mechanism driving the evolution. The galaxy mass-size relation and size growth do not depend on environment in the halo mass range explored in this work (field to group mass log(Mh/M) 14), i.e. group and field galaxies follow the same trends. At low redshift, where we examine both Sloan Digital Sky Survey and COSMOS groups, this result is at variance with predictions from some current hierarchical models that show a clear dependence of size growth on halo mass for massive ellipticals (log(M/M) 11.2). In future work, we will analyse in detail if this result is specific of the observations and model used in this work. Brightest Cluster Galaxies (BCG) and satellite galaxies lie on the same mass-size relation, at variance with predictions from hierarchical models, which predict that BCGs should have larger sizes than satellites because they experience more mergers in groups over the halo mass range probed. 2012 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. © 2012 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.
publishDate 2013
dc.date.none.fl_str_mv 2013
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/10261/408319
url http://hdl.handle.net/10261/408319
dc.relation.none.fl_str_mv http://dx.doi.org/10.1093/mnras/sts150
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.publisher.none.fl_str_mv Oxford University Press
publisher.none.fl_str_mv Oxford University Press
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
collection DIGITAL.CSIC. Repositorio Institucional del CSIC
repository.name.fl_str_mv
repository.mail.fl_str_mv
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