The evolution of galaxy metallicity scaling relations in cosmological hydrodynamical simulations

Autores
de Rossi, Maria Emilia; Theuns, T.; Font, A. S.; Mccarthy, I. G.
Año de publicación
2015
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
The evolution of the metal content of galaxies and its relations to other global properties [such as total stellar mass (M*), circular velocity, star formation rate (SFR), halo mass, etc.] provides important constraints on models of galaxy formation. Here we examine the evolution of metallicity scaling relations of simulated galaxies in the Galaxies-Intergalactic Medium Interaction Calculation suite of cosmological simulations. We make comparisons to observations of the correlation of gas-phase abundances with M* (the mass-metallicity relation, MZR), as well as with both M* and SFR or gas mass fraction (the so-called 3D fundamental metallicity relations, FMRs). The simulated galaxies follow the observed local MZR and FMRs over an order of magnitude in M*, but overpredict the metallicity of massive galaxies (log M* > 10.5), plausibly due to inefficient feedback in this regime. We discuss the origin of the MZR and FMRs in the context of galactic outflows and gas accretion. We examine the evolution of mass-metallicity relations defined using different elements that probe the three enrichment channels (SNII, SNIa, and AGB stars). Relations based on elements produced mainly by SNII evolve weakly, whereas those based on elements produced preferentially in SNIa/AGB exhibit stronger evolution, due to the longer timescales associated with these channels. Finally, we compare the relations of central and satellite galaxies, finding systematically higher metallicities for satellites, as observed. We show this is due to the removal of the metal poor gas reservoir that normally surrounds galaxies and acts to dilute their gas-phase metallicity (via cooling/accretion onto the disk), but is lost due to ram pressure stripping for satellites.
Fil: de Rossi, Maria Emilia. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Theuns, T.. University Of Durham. Dep.of Physics; Reino Unido
Fil: Font, A. S.. John Moores University; Reino Unido
Fil: Mccarthy, I. G.. John Moores University; Reino Unido
Materia
COSMOLOGY: THEORY
GALAXIES: EVOLUTION
GALAXIES: ABUNDANCES
GALAXIES: HALOES
GALAXIES: HIGH-REDSHIFT
GALAXIES: STAR FORMATION
METHOD: NUMERICAL SIMULATIONS
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/17710
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/17710
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling The evolution of galaxy metallicity scaling relations in cosmological hydrodynamical simulationsde Rossi, Maria EmiliaTheuns, T.Font, A. S.Mccarthy, I. G.COSMOLOGY: THEORYGALAXIES: EVOLUTIONGALAXIES: ABUNDANCESGALAXIES: HALOESGALAXIES: HIGH-REDSHIFTGALAXIES: STAR FORMATIONMETHOD: NUMERICAL SIMULATIONShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1The evolution of the metal content of galaxies and its relations to other global properties [such as total stellar mass (M*), circular velocity, star formation rate (SFR), halo mass, etc.] provides important constraints on models of galaxy formation. Here we examine the evolution of metallicity scaling relations of simulated galaxies in the Galaxies-Intergalactic Medium Interaction Calculation suite of cosmological simulations. We make comparisons to observations of the correlation of gas-phase abundances with M* (the mass-metallicity relation, MZR), as well as with both M* and SFR or gas mass fraction (the so-called 3D fundamental metallicity relations, FMRs). The simulated galaxies follow the observed local MZR and FMRs over an order of magnitude in M*, but overpredict the metallicity of massive galaxies (log M* > 10.5), plausibly due to inefficient feedback in this regime. We discuss the origin of the MZR and FMRs in the context of galactic outflows and gas accretion. We examine the evolution of mass-metallicity relations defined using different elements that probe the three enrichment channels (SNII, SNIa, and AGB stars). Relations based on elements produced mainly by SNII evolve weakly, whereas those based on elements produced preferentially in SNIa/AGB exhibit stronger evolution, due to the longer timescales associated with these channels. Finally, we compare the relations of central and satellite galaxies, finding systematically higher metallicities for satellites, as observed. We show this is due to the removal of the metal poor gas reservoir that normally surrounds galaxies and acts to dilute their gas-phase metallicity (via cooling/accretion onto the disk), but is lost due to ram pressure stripping for satellites.Fil: de Rossi, Maria Emilia. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Theuns, T.. University Of Durham. Dep.of Physics; Reino UnidoFil: Font, A. S.. John Moores University; Reino UnidoFil: Mccarthy, I. G.. John Moores University; Reino UnidoOxford University Press2015-07-03info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/zipapplication/pdfhttp://hdl.handle.net/11336/17710de Rossi, Maria Emilia; Theuns, T.; Font, A. S.; Mccarthy, I. G.; The evolution of galaxy metallicity scaling relations in cosmological hydrodynamical simulations; Oxford University Press; Monthly Notices Of The Royal Astronomical Society; 452; 1; 3-7-2015; 486-5010035-8711enginfo:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stv1287info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-abstract/452/1/486/1749726/The-evolution-of-galaxy-metallicity-scaling?redirectedFrom=fulltextinfo:eu-repo/semantics/altIdentifier/arxiv/https://arxiv.org/abs/1506.02772info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-15T15:13:16Zoai:ri.conicet.gov.ar:11336/17710instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-10-15 15:13:16.267CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv The evolution of galaxy metallicity scaling relations in cosmological hydrodynamical simulations
title The evolution of galaxy metallicity scaling relations in cosmological hydrodynamical simulations
spellingShingle The evolution of galaxy metallicity scaling relations in cosmological hydrodynamical simulations
de Rossi, Maria Emilia
COSMOLOGY: THEORY
GALAXIES: EVOLUTION
GALAXIES: ABUNDANCES
GALAXIES: HALOES
GALAXIES: HIGH-REDSHIFT
GALAXIES: STAR FORMATION
METHOD: NUMERICAL SIMULATIONS
title_short The evolution of galaxy metallicity scaling relations in cosmological hydrodynamical simulations
title_full The evolution of galaxy metallicity scaling relations in cosmological hydrodynamical simulations
title_fullStr The evolution of galaxy metallicity scaling relations in cosmological hydrodynamical simulations
title_full_unstemmed The evolution of galaxy metallicity scaling relations in cosmological hydrodynamical simulations
title_sort The evolution of galaxy metallicity scaling relations in cosmological hydrodynamical simulations
dc.creator.none.fl_str_mv de Rossi, Maria Emilia
Theuns, T.
Font, A. S.
Mccarthy, I. G.
author de Rossi, Maria Emilia
author_facet de Rossi, Maria Emilia
Theuns, T.
Font, A. S.
Mccarthy, I. G.
author_role author
author2 Theuns, T.
Font, A. S.
Mccarthy, I. G.
author2_role author
author
author
dc.subject.none.fl_str_mv COSMOLOGY: THEORY
GALAXIES: EVOLUTION
GALAXIES: ABUNDANCES
GALAXIES: HALOES
GALAXIES: HIGH-REDSHIFT
GALAXIES: STAR FORMATION
METHOD: NUMERICAL SIMULATIONS
topic COSMOLOGY: THEORY
GALAXIES: EVOLUTION
GALAXIES: ABUNDANCES
GALAXIES: HALOES
GALAXIES: HIGH-REDSHIFT
GALAXIES: STAR FORMATION
METHOD: NUMERICAL SIMULATIONS
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv The evolution of the metal content of galaxies and its relations to other global properties [such as total stellar mass (M*), circular velocity, star formation rate (SFR), halo mass, etc.] provides important constraints on models of galaxy formation. Here we examine the evolution of metallicity scaling relations of simulated galaxies in the Galaxies-Intergalactic Medium Interaction Calculation suite of cosmological simulations. We make comparisons to observations of the correlation of gas-phase abundances with M* (the mass-metallicity relation, MZR), as well as with both M* and SFR or gas mass fraction (the so-called 3D fundamental metallicity relations, FMRs). The simulated galaxies follow the observed local MZR and FMRs over an order of magnitude in M*, but overpredict the metallicity of massive galaxies (log M* > 10.5), plausibly due to inefficient feedback in this regime. We discuss the origin of the MZR and FMRs in the context of galactic outflows and gas accretion. We examine the evolution of mass-metallicity relations defined using different elements that probe the three enrichment channels (SNII, SNIa, and AGB stars). Relations based on elements produced mainly by SNII evolve weakly, whereas those based on elements produced preferentially in SNIa/AGB exhibit stronger evolution, due to the longer timescales associated with these channels. Finally, we compare the relations of central and satellite galaxies, finding systematically higher metallicities for satellites, as observed. We show this is due to the removal of the metal poor gas reservoir that normally surrounds galaxies and acts to dilute their gas-phase metallicity (via cooling/accretion onto the disk), but is lost due to ram pressure stripping for satellites.
Fil: de Rossi, Maria Emilia. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Theuns, T.. University Of Durham. Dep.of Physics; Reino Unido
Fil: Font, A. S.. John Moores University; Reino Unido
Fil: Mccarthy, I. G.. John Moores University; Reino Unido
description The evolution of the metal content of galaxies and its relations to other global properties [such as total stellar mass (M*), circular velocity, star formation rate (SFR), halo mass, etc.] provides important constraints on models of galaxy formation. Here we examine the evolution of metallicity scaling relations of simulated galaxies in the Galaxies-Intergalactic Medium Interaction Calculation suite of cosmological simulations. We make comparisons to observations of the correlation of gas-phase abundances with M* (the mass-metallicity relation, MZR), as well as with both M* and SFR or gas mass fraction (the so-called 3D fundamental metallicity relations, FMRs). The simulated galaxies follow the observed local MZR and FMRs over an order of magnitude in M*, but overpredict the metallicity of massive galaxies (log M* > 10.5), plausibly due to inefficient feedback in this regime. We discuss the origin of the MZR and FMRs in the context of galactic outflows and gas accretion. We examine the evolution of mass-metallicity relations defined using different elements that probe the three enrichment channels (SNII, SNIa, and AGB stars). Relations based on elements produced mainly by SNII evolve weakly, whereas those based on elements produced preferentially in SNIa/AGB exhibit stronger evolution, due to the longer timescales associated with these channels. Finally, we compare the relations of central and satellite galaxies, finding systematically higher metallicities for satellites, as observed. We show this is due to the removal of the metal poor gas reservoir that normally surrounds galaxies and acts to dilute their gas-phase metallicity (via cooling/accretion onto the disk), but is lost due to ram pressure stripping for satellites.
publishDate 2015
dc.date.none.fl_str_mv 2015-07-03
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/11336/17710
de Rossi, Maria Emilia; Theuns, T.; Font, A. S.; Mccarthy, I. G.; The evolution of galaxy metallicity scaling relations in cosmological hydrodynamical simulations; Oxford University Press; Monthly Notices Of The Royal Astronomical Society; 452; 1; 3-7-2015; 486-501
0035-8711
url http://hdl.handle.net/11336/17710
identifier_str_mv de Rossi, Maria Emilia; Theuns, T.; Font, A. S.; Mccarthy, I. G.; The evolution of galaxy metallicity scaling relations in cosmological hydrodynamical simulations; Oxford University Press; Monthly Notices Of The Royal Astronomical Society; 452; 1; 3-7-2015; 486-501
0035-8711
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stv1287
info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-abstract/452/1/486/1749726/The-evolution-of-galaxy-metallicity-scaling?redirectedFrom=fulltext
info:eu-repo/semantics/altIdentifier/arxiv/https://arxiv.org/abs/1506.02772
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/zip
application/pdf
dc.publisher.none.fl_str_mv Oxford University Press
publisher.none.fl_str_mv Oxford University Press
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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score 13.22299

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