Morphology of galaxies with quiescent recent assembly history in a Λ-CDM universe

Autores
Pedrosa, Susana Elizabeth; Tissera, Patricia Beatriz; de Rossi, Maria Emilia
Año de publicación
2014
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Context. The standard disc formation scenario postulates that the disc forms as the gas cools and flows into the centre of the dark matter halo, conserving the specific angular momentum. Major mergers have been shown to be able to destroy or highly perturb the disc components. More recently, the alignment of the material that is accreted to form the galaxy has been pointed out as a key ingredient to determine galaxy morphology. However, in a hierarchical scenario galaxy formation is a complex process that combines these processes and others in a non-linear way so that the origin of galaxy morphology remains to be fully understood. Aims: We aim at exploring the differences in the formation histories of galaxies with a variety of morphologies, but quite recent merger histories, to identify which mechanisms are playing a major role. We analyse when minor mergers can be considered relevant to determine galaxy morphology. We also study the specific angular momentum content of the disc and central spheroidal components separately. Methods: We used cosmological hydrodynamical simulations that include an effective, physically motivated supernova feedback that is able to regulate the star formation in haloes of different masses. We analysed the morphology and formation history of a sample of 15 galaxies of a cosmological simulation. We performed a spheroid-disc decomposition of the selected galaxies and their progenitor systems. The angular momentum orientation of the merging systems as well as their relative masses were estimated to analyse the role played by orientation and by minor mergers in the determination of the morphology. Results: We found the discs to be formed by conserving the specific angular momentum in accordance with the classical disc formation model. The specific angular momentum of the stellar central spheroid correlates with the dark matter halo angular momentum and determines a power law. Our results suggest that gas accretion to rebuild the disc component is a necessary but not sufficient ingredient for a disc-dominated galaxy in a hierarchical clustering scenario. The survival of the discs is tightly linked to their subsequent history of accretion, as previously reported. Minor mergers play an important role. It is more likely that they will destroy the disc and feed the central spheroid if their angular momentum is misaligned with respect to that of the main galaxy. Conversely, if they are aligned, they can contribute to the disc formation.
Fil: Pedrosa, Susana Elizabeth. 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: Tissera, Patricia Beatriz. 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: 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
Materia
GALAXIES FORMATION
GALAXIES EVOLUTION
GALAXIES STRUCTURE
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:11336/21401

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network_name_str CONICET Digital (CONICET)
spelling Morphology of galaxies with quiescent recent assembly history in a Λ-CDM universePedrosa, Susana ElizabethTissera, Patricia Beatrizde Rossi, Maria EmiliaGALAXIES FORMATIONGALAXIES EVOLUTIONGALAXIES STRUCTUREhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. The standard disc formation scenario postulates that the disc forms as the gas cools and flows into the centre of the dark matter halo, conserving the specific angular momentum. Major mergers have been shown to be able to destroy or highly perturb the disc components. More recently, the alignment of the material that is accreted to form the galaxy has been pointed out as a key ingredient to determine galaxy morphology. However, in a hierarchical scenario galaxy formation is a complex process that combines these processes and others in a non-linear way so that the origin of galaxy morphology remains to be fully understood. Aims: We aim at exploring the differences in the formation histories of galaxies with a variety of morphologies, but quite recent merger histories, to identify which mechanisms are playing a major role. We analyse when minor mergers can be considered relevant to determine galaxy morphology. We also study the specific angular momentum content of the disc and central spheroidal components separately. Methods: We used cosmological hydrodynamical simulations that include an effective, physically motivated supernova feedback that is able to regulate the star formation in haloes of different masses. We analysed the morphology and formation history of a sample of 15 galaxies of a cosmological simulation. We performed a spheroid-disc decomposition of the selected galaxies and their progenitor systems. The angular momentum orientation of the merging systems as well as their relative masses were estimated to analyse the role played by orientation and by minor mergers in the determination of the morphology. Results: We found the discs to be formed by conserving the specific angular momentum in accordance with the classical disc formation model. The specific angular momentum of the stellar central spheroid correlates with the dark matter halo angular momentum and determines a power law. Our results suggest that gas accretion to rebuild the disc component is a necessary but not sufficient ingredient for a disc-dominated galaxy in a hierarchical clustering scenario. The survival of the discs is tightly linked to their subsequent history of accretion, as previously reported. Minor mergers play an important role. It is more likely that they will destroy the disc and feed the central spheroid if their angular momentum is misaligned with respect to that of the main galaxy. Conversely, if they are aligned, they can contribute to the disc formation.Fil: Pedrosa, Susana Elizabeth. 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: Tissera, Patricia Beatriz. 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: 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; ArgentinaEDP Sciences2014-07info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/21401Pedrosa, Susana Elizabeth; Tissera, Patricia Beatriz; de Rossi, Maria Emilia; Morphology of galaxies with quiescent recent assembly history in a Λ-CDM universe; EDP Sciences; Astronomy and Astrophysics; 567; A47; 7-2014; 1-90004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2014/07/aa23079-13/aa23079-13.htmlinfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201323079info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1405.5836info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-03T10:01:25Zoai:ri.conicet.gov.ar:11336/21401instacron: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:34982025-09-03 10:01:25.739CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Morphology of galaxies with quiescent recent assembly history in a Λ-CDM universe
title Morphology of galaxies with quiescent recent assembly history in a Λ-CDM universe
spellingShingle Morphology of galaxies with quiescent recent assembly history in a Λ-CDM universe
Pedrosa, Susana Elizabeth
GALAXIES FORMATION
GALAXIES EVOLUTION
GALAXIES STRUCTURE
title_short Morphology of galaxies with quiescent recent assembly history in a Λ-CDM universe
title_full Morphology of galaxies with quiescent recent assembly history in a Λ-CDM universe
title_fullStr Morphology of galaxies with quiescent recent assembly history in a Λ-CDM universe
title_full_unstemmed Morphology of galaxies with quiescent recent assembly history in a Λ-CDM universe
title_sort Morphology of galaxies with quiescent recent assembly history in a Λ-CDM universe
dc.creator.none.fl_str_mv Pedrosa, Susana Elizabeth
Tissera, Patricia Beatriz
de Rossi, Maria Emilia
author Pedrosa, Susana Elizabeth
author_facet Pedrosa, Susana Elizabeth
Tissera, Patricia Beatriz
de Rossi, Maria Emilia
author_role author
author2 Tissera, Patricia Beatriz
de Rossi, Maria Emilia
author2_role author
author
dc.subject.none.fl_str_mv GALAXIES FORMATION
GALAXIES EVOLUTION
GALAXIES STRUCTURE
topic GALAXIES FORMATION
GALAXIES EVOLUTION
GALAXIES STRUCTURE
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Context. The standard disc formation scenario postulates that the disc forms as the gas cools and flows into the centre of the dark matter halo, conserving the specific angular momentum. Major mergers have been shown to be able to destroy or highly perturb the disc components. More recently, the alignment of the material that is accreted to form the galaxy has been pointed out as a key ingredient to determine galaxy morphology. However, in a hierarchical scenario galaxy formation is a complex process that combines these processes and others in a non-linear way so that the origin of galaxy morphology remains to be fully understood. Aims: We aim at exploring the differences in the formation histories of galaxies with a variety of morphologies, but quite recent merger histories, to identify which mechanisms are playing a major role. We analyse when minor mergers can be considered relevant to determine galaxy morphology. We also study the specific angular momentum content of the disc and central spheroidal components separately. Methods: We used cosmological hydrodynamical simulations that include an effective, physically motivated supernova feedback that is able to regulate the star formation in haloes of different masses. We analysed the morphology and formation history of a sample of 15 galaxies of a cosmological simulation. We performed a spheroid-disc decomposition of the selected galaxies and their progenitor systems. The angular momentum orientation of the merging systems as well as their relative masses were estimated to analyse the role played by orientation and by minor mergers in the determination of the morphology. Results: We found the discs to be formed by conserving the specific angular momentum in accordance with the classical disc formation model. The specific angular momentum of the stellar central spheroid correlates with the dark matter halo angular momentum and determines a power law. Our results suggest that gas accretion to rebuild the disc component is a necessary but not sufficient ingredient for a disc-dominated galaxy in a hierarchical clustering scenario. The survival of the discs is tightly linked to their subsequent history of accretion, as previously reported. Minor mergers play an important role. It is more likely that they will destroy the disc and feed the central spheroid if their angular momentum is misaligned with respect to that of the main galaxy. Conversely, if they are aligned, they can contribute to the disc formation.
Fil: Pedrosa, Susana Elizabeth. 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: Tissera, Patricia Beatriz. 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: 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
description Context. The standard disc formation scenario postulates that the disc forms as the gas cools and flows into the centre of the dark matter halo, conserving the specific angular momentum. Major mergers have been shown to be able to destroy or highly perturb the disc components. More recently, the alignment of the material that is accreted to form the galaxy has been pointed out as a key ingredient to determine galaxy morphology. However, in a hierarchical scenario galaxy formation is a complex process that combines these processes and others in a non-linear way so that the origin of galaxy morphology remains to be fully understood. Aims: We aim at exploring the differences in the formation histories of galaxies with a variety of morphologies, but quite recent merger histories, to identify which mechanisms are playing a major role. We analyse when minor mergers can be considered relevant to determine galaxy morphology. We also study the specific angular momentum content of the disc and central spheroidal components separately. Methods: We used cosmological hydrodynamical simulations that include an effective, physically motivated supernova feedback that is able to regulate the star formation in haloes of different masses. We analysed the morphology and formation history of a sample of 15 galaxies of a cosmological simulation. We performed a spheroid-disc decomposition of the selected galaxies and their progenitor systems. The angular momentum orientation of the merging systems as well as their relative masses were estimated to analyse the role played by orientation and by minor mergers in the determination of the morphology. Results: We found the discs to be formed by conserving the specific angular momentum in accordance with the classical disc formation model. The specific angular momentum of the stellar central spheroid correlates with the dark matter halo angular momentum and determines a power law. Our results suggest that gas accretion to rebuild the disc component is a necessary but not sufficient ingredient for a disc-dominated galaxy in a hierarchical clustering scenario. The survival of the discs is tightly linked to their subsequent history of accretion, as previously reported. Minor mergers play an important role. It is more likely that they will destroy the disc and feed the central spheroid if their angular momentum is misaligned with respect to that of the main galaxy. Conversely, if they are aligned, they can contribute to the disc formation.
publishDate 2014
dc.date.none.fl_str_mv 2014-07
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/11336/21401
Pedrosa, Susana Elizabeth; Tissera, Patricia Beatriz; de Rossi, Maria Emilia; Morphology of galaxies with quiescent recent assembly history in a Λ-CDM universe; EDP Sciences; Astronomy and Astrophysics; 567; A47; 7-2014; 1-9
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/21401
identifier_str_mv Pedrosa, Susana Elizabeth; Tissera, Patricia Beatriz; de Rossi, Maria Emilia; Morphology of galaxies with quiescent recent assembly history in a Λ-CDM universe; EDP Sciences; Astronomy and Astrophysics; 567; A47; 7-2014; 1-9
0004-6361
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2014/07/aa23079-13/aa23079-13.html
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201323079
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1405.5836
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/pdf
application/pdf
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
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reponame_str CONICET Digital (CONICET)
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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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