Angular momentum evolution for galaxies in a Λ-CDM scenario

Autores
Pedrosa, Susana Elizabeth; Tissera, Patricia Beatriz
Año de publicación
2015
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Context. Galaxy formation in the current cosmological paradigm is a verycomplex process in which inflows, outflows, interactions, and mergersare common events. These processes can redistribute the angular momentumcontent of baryons. Recent observational results suggest that discformed conserving angular momentum while elliptical galaxies, althoughthey lose angular momentum, determine a correlation between the specificangular momentum of the galaxy and the stellar mass. These observationsprovide stringent constraints for galaxy formation models in ahierarchical clustering scenario.
Aims: We aim to analyse thespecific angular momentum content of the disc and bulge components as afunction of virial mass, stellar mass, and redshift. We also estimatethe size of the simulated galaxies and compare them with observations.
Methods: We use cosmological hydrodynamical simulations thatinclude an effective, physically motivated supernova feedback which isable to regulate the star formation in haloes of different masses. Weanalyse the morphology and formation history of a sample of galaxies ina cosmological simulation by performing a bulge-disc decomposition ofthe analysed systems and their progenitors. We estimate the angularmomentum content of the stellar and gaseous discs, stellar bulges, andtotal baryons.
Results: In agreement with recent observationalfindings, our simulated galaxies have disc and spheroid components whosespecific angular momentum content determine correlations with thestellar and dark matter masses with the same slope, although thespheroidal components are offset by a fixed fraction. The averageangular momentum efficiency for the simulated discs is η ~ 1, whilefor bulges it is η ~ 0.10-0.20. For the simulated sample, thecorrelations found for the specific angular momentum content as afunction of virial mass or stellar mass are found not to evolvesignificantly with redshift (up to z ~ 2). Both dynamical componentsseem to move along the correlations as they evolve. The total specificangular momentum of galaxies occupy different positions filling the gapbetween pure rotational-dominated and dispersion-dominated systems. Thescaling relations derived from the simulated galaxies determine asimilar relation with the virial radius, which is in agreement withrecent observations.
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. Universidad Andres Bello; Chile. 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
GALAXY FORMATION
GALAXY EVOLUTION
COSMOLOGY DARK MATTER
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/18115
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/18115
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Angular momentum evolution for galaxies in a Λ-CDM scenarioPedrosa, Susana ElizabethTissera, Patricia BeatrizGALAXY FORMATIONGALAXY EVOLUTIONCOSMOLOGY DARK MATTERhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. Galaxy formation in the current cosmological paradigm is a verycomplex process in which inflows, outflows, interactions, and mergersare common events. These processes can redistribute the angular momentumcontent of baryons. Recent observational results suggest that discformed conserving angular momentum while elliptical galaxies, althoughthey lose angular momentum, determine a correlation between the specificangular momentum of the galaxy and the stellar mass. These observationsprovide stringent constraints for galaxy formation models in ahierarchical clustering scenario. <br /> Aims: We aim to analyse thespecific angular momentum content of the disc and bulge components as afunction of virial mass, stellar mass, and redshift. We also estimatethe size of the simulated galaxies and compare them with observations.<br /> Methods: We use cosmological hydrodynamical simulations thatinclude an effective, physically motivated supernova feedback which isable to regulate the star formation in haloes of different masses. Weanalyse the morphology and formation history of a sample of galaxies ina cosmological simulation by performing a bulge-disc decomposition ofthe analysed systems and their progenitors. We estimate the angularmomentum content of the stellar and gaseous discs, stellar bulges, andtotal baryons. <br /> Results: In agreement with recent observationalfindings, our simulated galaxies have disc and spheroid components whosespecific angular momentum content determine correlations with thestellar and dark matter masses with the same slope, although thespheroidal components are offset by a fixed fraction. The averageangular momentum efficiency for the simulated discs is η ~ 1, whilefor bulges it is η ~ 0.10-0.20. For the simulated sample, thecorrelations found for the specific angular momentum content as afunction of virial mass or stellar mass are found not to evolvesignificantly with redshift (up to z ~ 2). Both dynamical componentsseem to move along the correlations as they evolve. The total specificangular momentum of galaxies occupy different positions filling the gapbetween pure rotational-dominated and dispersion-dominated systems. Thescaling relations derived from the simulated galaxies determine asimilar relation with the virial radius, which is in agreement withrecent observations.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. Universidad Andres Bello; Chile. 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 Sciences2015-12info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/18115Pedrosa, Susana Elizabeth; Tissera, Patricia Beatriz; Angular momentum evolution for galaxies in a Λ-CDM scenario; EDP Sciences; Astronomy & Astrophysics. Supplement Series (print); 584; A43; 12-2015; 1-80365-0138CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201526440info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1508.07220info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2015/12/aa26440-15/aa26440-15.htmlinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-03T09:52:06Zoai:ri.conicet.gov.ar:11336/18115instacron: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 09:52:06.637CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Angular momentum evolution for galaxies in a Λ-CDM scenario
title Angular momentum evolution for galaxies in a Λ-CDM scenario
spellingShingle Angular momentum evolution for galaxies in a Λ-CDM scenario
Pedrosa, Susana Elizabeth
GALAXY FORMATION
GALAXY EVOLUTION
COSMOLOGY DARK MATTER
title_short Angular momentum evolution for galaxies in a Λ-CDM scenario
title_full Angular momentum evolution for galaxies in a Λ-CDM scenario
title_fullStr Angular momentum evolution for galaxies in a Λ-CDM scenario
title_full_unstemmed Angular momentum evolution for galaxies in a Λ-CDM scenario
title_sort Angular momentum evolution for galaxies in a Λ-CDM scenario
dc.creator.none.fl_str_mv Pedrosa, Susana Elizabeth
Tissera, Patricia Beatriz
author Pedrosa, Susana Elizabeth
author_facet Pedrosa, Susana Elizabeth
Tissera, Patricia Beatriz
author_role author
author2 Tissera, Patricia Beatriz
author2_role author
dc.subject.none.fl_str_mv GALAXY FORMATION
GALAXY EVOLUTION
COSMOLOGY DARK MATTER
topic GALAXY FORMATION
GALAXY EVOLUTION
COSMOLOGY DARK MATTER
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. Galaxy formation in the current cosmological paradigm is a verycomplex process in which inflows, outflows, interactions, and mergersare common events. These processes can redistribute the angular momentumcontent of baryons. Recent observational results suggest that discformed conserving angular momentum while elliptical galaxies, althoughthey lose angular momentum, determine a correlation between the specificangular momentum of the galaxy and the stellar mass. These observationsprovide stringent constraints for galaxy formation models in ahierarchical clustering scenario. <br /> Aims: We aim to analyse thespecific angular momentum content of the disc and bulge components as afunction of virial mass, stellar mass, and redshift. We also estimatethe size of the simulated galaxies and compare them with observations.<br /> Methods: We use cosmological hydrodynamical simulations thatinclude an effective, physically motivated supernova feedback which isable to regulate the star formation in haloes of different masses. Weanalyse the morphology and formation history of a sample of galaxies ina cosmological simulation by performing a bulge-disc decomposition ofthe analysed systems and their progenitors. We estimate the angularmomentum content of the stellar and gaseous discs, stellar bulges, andtotal baryons. <br /> Results: In agreement with recent observationalfindings, our simulated galaxies have disc and spheroid components whosespecific angular momentum content determine correlations with thestellar and dark matter masses with the same slope, although thespheroidal components are offset by a fixed fraction. The averageangular momentum efficiency for the simulated discs is η ~ 1, whilefor bulges it is η ~ 0.10-0.20. For the simulated sample, thecorrelations found for the specific angular momentum content as afunction of virial mass or stellar mass are found not to evolvesignificantly with redshift (up to z ~ 2). Both dynamical componentsseem to move along the correlations as they evolve. The total specificangular momentum of galaxies occupy different positions filling the gapbetween pure rotational-dominated and dispersion-dominated systems. Thescaling relations derived from the simulated galaxies determine asimilar relation with the virial radius, which is in agreement withrecent observations.
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. Universidad Andres Bello; Chile. 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. Galaxy formation in the current cosmological paradigm is a verycomplex process in which inflows, outflows, interactions, and mergersare common events. These processes can redistribute the angular momentumcontent of baryons. Recent observational results suggest that discformed conserving angular momentum while elliptical galaxies, althoughthey lose angular momentum, determine a correlation between the specificangular momentum of the galaxy and the stellar mass. These observationsprovide stringent constraints for galaxy formation models in ahierarchical clustering scenario. <br /> Aims: We aim to analyse thespecific angular momentum content of the disc and bulge components as afunction of virial mass, stellar mass, and redshift. We also estimatethe size of the simulated galaxies and compare them with observations.<br /> Methods: We use cosmological hydrodynamical simulations thatinclude an effective, physically motivated supernova feedback which isable to regulate the star formation in haloes of different masses. Weanalyse the morphology and formation history of a sample of galaxies ina cosmological simulation by performing a bulge-disc decomposition ofthe analysed systems and their progenitors. We estimate the angularmomentum content of the stellar and gaseous discs, stellar bulges, andtotal baryons. <br /> Results: In agreement with recent observationalfindings, our simulated galaxies have disc and spheroid components whosespecific angular momentum content determine correlations with thestellar and dark matter masses with the same slope, although thespheroidal components are offset by a fixed fraction. The averageangular momentum efficiency for the simulated discs is η ~ 1, whilefor bulges it is η ~ 0.10-0.20. For the simulated sample, thecorrelations found for the specific angular momentum content as afunction of virial mass or stellar mass are found not to evolvesignificantly with redshift (up to z ~ 2). Both dynamical componentsseem to move along the correlations as they evolve. The total specificangular momentum of galaxies occupy different positions filling the gapbetween pure rotational-dominated and dispersion-dominated systems. Thescaling relations derived from the simulated galaxies determine asimilar relation with the virial radius, which is in agreement withrecent observations.
publishDate 2015
dc.date.none.fl_str_mv 2015-12
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/11336/18115
Pedrosa, Susana Elizabeth; Tissera, Patricia Beatriz; Angular momentum evolution for galaxies in a Λ-CDM scenario; EDP Sciences; Astronomy & Astrophysics. Supplement Series (print); 584; A43; 12-2015; 1-8
0365-0138
CONICET Digital
CONICET
url http://hdl.handle.net/11336/18115
identifier_str_mv Pedrosa, Susana Elizabeth; Tissera, Patricia Beatriz; Angular momentum evolution for galaxies in a Λ-CDM scenario; EDP Sciences; Astronomy & Astrophysics. Supplement Series (print); 584; A43; 12-2015; 1-8
0365-0138
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201526440
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1508.07220
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2015/12/aa26440-15/aa26440-15.html
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
application/pdf
application/pdf
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
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 13.13397

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