Dark matter response to galaxy assembly history

Autores
Artale, María Celeste; Pedrosa, Susana Elizabeth; Tissera, Patricia Beatriz; Cataldi, Pedro Anselmo; Di Cintio, Arianna
Año de publicación
2019
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Aims. It is well known that the presence of baryons affects the dark matter host haloes. Exploring the galaxy assembly history together with the dark matter haloes properties through time can provide a way to measure these effects. Methods. We study the properties of four Milky Way mass dark matter haloes from the Aquarius project during their assembly history, between z = 0 − 4. In this work, we use the SPH run from Scannapieco et al. (2009) and the dark matter only counterpart as case studies. To asses the robustness of our findings, we compare them with one of the haloes run using a moving-mesh technique and different sub-grid scheme. Results. Our results show that the cosmic evolution of the dark matter halo profiles depends on the assembly history of the baryons. We find that the dark matter profiles do not significantly change with time, hence they become stable, when the fraction of baryons accumulated in the central regions reaches 80 percent of its present mass within the virial radius. Furthermore, the mass accretion history shows that the haloes that assembled earlier are those that contain a larger amount of baryonic mass aforetime, which in turn allows the dark matter halo profiles to reach a stable configuration earlier. For the SPH haloes, we find that the specific angular momentum of the dark matter particles within the five percent of the virial radius at z = 0, remains approximately constant from the time at which 60 percent of the stellar mass is gathered. We explore different theoretical and empirical models for the contraction of the haloes through redshift. A model to better describe the contraction of the haloes through redshift evolution must depend on the stellar mass content in the inner regions.
Fil: Artale, María Celeste. Universidad de Innsbruck; Austria
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. Universidad Andrés Bello; Chile
Fil: Cataldi, Pedro Anselmo. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Física de Buenos Aires. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Física de Buenos Aires; Argentina
Fil: Di Cintio, Arianna. Universidad de La Laguna; España. Instituto de Astrofísica de Canarias; España
Materia
GALAXIES: HALOS
GALAXY: EVOLUTION
GALAXY: FORMATION
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:11336/151826
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/151826
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Dark matter response to galaxy assembly historyArtale, María CelestePedrosa, Susana ElizabethTissera, Patricia BeatrizCataldi, Pedro AnselmoDi Cintio, AriannaGALAXIES: HALOSGALAXY: EVOLUTIONGALAXY: FORMATIONhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Aims. It is well known that the presence of baryons affects the dark matter host haloes. Exploring the galaxy assembly history together with the dark matter haloes properties through time can provide a way to measure these effects. Methods. We study the properties of four Milky Way mass dark matter haloes from the Aquarius project during their assembly history, between z = 0 − 4. In this work, we use the SPH run from Scannapieco et al. (2009) and the dark matter only counterpart as case studies. To asses the robustness of our findings, we compare them with one of the haloes run using a moving-mesh technique and different sub-grid scheme. Results. Our results show that the cosmic evolution of the dark matter halo profiles depends on the assembly history of the baryons. We find that the dark matter profiles do not significantly change with time, hence they become stable, when the fraction of baryons accumulated in the central regions reaches 80 percent of its present mass within the virial radius. Furthermore, the mass accretion history shows that the haloes that assembled earlier are those that contain a larger amount of baryonic mass aforetime, which in turn allows the dark matter halo profiles to reach a stable configuration earlier. For the SPH haloes, we find that the specific angular momentum of the dark matter particles within the five percent of the virial radius at z = 0, remains approximately constant from the time at which 60 percent of the stellar mass is gathered. We explore different theoretical and empirical models for the contraction of the haloes through redshift. A model to better describe the contraction of the haloes through redshift evolution must depend on the stellar mass content in the inner regions.Fil: Artale, María Celeste. Universidad de Innsbruck; AustriaFil: 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; Argentina. Universidad Andrés Bello; ChileFil: Cataldi, Pedro Anselmo. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Física de Buenos Aires. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Física de Buenos Aires; ArgentinaFil: Di Cintio, Arianna. Universidad de La Laguna; España. Instituto de Astrofísica de Canarias; EspañaEDP Sciences2019-02info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/151826Artale, María Celeste; Pedrosa, Susana Elizabeth; Tissera, Patricia Beatriz; Cataldi, Pedro Anselmo; Di Cintio, Arianna; Dark matter response to galaxy assembly history; EDP Sciences; Astronomy and Astrophysics; 622; A197; 2-2019; 1-170004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201834096info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1901.02269v1info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2019/02/aa34096-18/aa34096-18.htmlinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-15T14:55:45Zoai:ri.conicet.gov.ar:11336/151826instacron: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 14:55:45.984CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Dark matter response to galaxy assembly history
title Dark matter response to galaxy assembly history
spellingShingle Dark matter response to galaxy assembly history
Artale, María Celeste
GALAXIES: HALOS
GALAXY: EVOLUTION
GALAXY: FORMATION
title_short Dark matter response to galaxy assembly history
title_full Dark matter response to galaxy assembly history
title_fullStr Dark matter response to galaxy assembly history
title_full_unstemmed Dark matter response to galaxy assembly history
title_sort Dark matter response to galaxy assembly history
dc.creator.none.fl_str_mv Artale, María Celeste
Pedrosa, Susana Elizabeth
Tissera, Patricia Beatriz
Cataldi, Pedro Anselmo
Di Cintio, Arianna
author Artale, María Celeste
author_facet Artale, María Celeste
Pedrosa, Susana Elizabeth
Tissera, Patricia Beatriz
Cataldi, Pedro Anselmo
Di Cintio, Arianna
author_role author
author2 Pedrosa, Susana Elizabeth
Tissera, Patricia Beatriz
Cataldi, Pedro Anselmo
Di Cintio, Arianna
author2_role author
author
author
author
dc.subject.none.fl_str_mv GALAXIES: HALOS
GALAXY: EVOLUTION
GALAXY: FORMATION
topic GALAXIES: HALOS
GALAXY: EVOLUTION
GALAXY: FORMATION
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Aims. It is well known that the presence of baryons affects the dark matter host haloes. Exploring the galaxy assembly history together with the dark matter haloes properties through time can provide a way to measure these effects. Methods. We study the properties of four Milky Way mass dark matter haloes from the Aquarius project during their assembly history, between z = 0 − 4. In this work, we use the SPH run from Scannapieco et al. (2009) and the dark matter only counterpart as case studies. To asses the robustness of our findings, we compare them with one of the haloes run using a moving-mesh technique and different sub-grid scheme. Results. Our results show that the cosmic evolution of the dark matter halo profiles depends on the assembly history of the baryons. We find that the dark matter profiles do not significantly change with time, hence they become stable, when the fraction of baryons accumulated in the central regions reaches 80 percent of its present mass within the virial radius. Furthermore, the mass accretion history shows that the haloes that assembled earlier are those that contain a larger amount of baryonic mass aforetime, which in turn allows the dark matter halo profiles to reach a stable configuration earlier. For the SPH haloes, we find that the specific angular momentum of the dark matter particles within the five percent of the virial radius at z = 0, remains approximately constant from the time at which 60 percent of the stellar mass is gathered. We explore different theoretical and empirical models for the contraction of the haloes through redshift. A model to better describe the contraction of the haloes through redshift evolution must depend on the stellar mass content in the inner regions.
Fil: Artale, María Celeste. Universidad de Innsbruck; Austria
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. Universidad Andrés Bello; Chile
Fil: Cataldi, Pedro Anselmo. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Física de Buenos Aires. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Física de Buenos Aires; Argentina
Fil: Di Cintio, Arianna. Universidad de La Laguna; España. Instituto de Astrofísica de Canarias; España
description Aims. It is well known that the presence of baryons affects the dark matter host haloes. Exploring the galaxy assembly history together with the dark matter haloes properties through time can provide a way to measure these effects. Methods. We study the properties of four Milky Way mass dark matter haloes from the Aquarius project during their assembly history, between z = 0 − 4. In this work, we use the SPH run from Scannapieco et al. (2009) and the dark matter only counterpart as case studies. To asses the robustness of our findings, we compare them with one of the haloes run using a moving-mesh technique and different sub-grid scheme. Results. Our results show that the cosmic evolution of the dark matter halo profiles depends on the assembly history of the baryons. We find that the dark matter profiles do not significantly change with time, hence they become stable, when the fraction of baryons accumulated in the central regions reaches 80 percent of its present mass within the virial radius. Furthermore, the mass accretion history shows that the haloes that assembled earlier are those that contain a larger amount of baryonic mass aforetime, which in turn allows the dark matter halo profiles to reach a stable configuration earlier. For the SPH haloes, we find that the specific angular momentum of the dark matter particles within the five percent of the virial radius at z = 0, remains approximately constant from the time at which 60 percent of the stellar mass is gathered. We explore different theoretical and empirical models for the contraction of the haloes through redshift. A model to better describe the contraction of the haloes through redshift evolution must depend on the stellar mass content in the inner regions.
publishDate 2019
dc.date.none.fl_str_mv 2019-02
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/11336/151826
Artale, María Celeste; Pedrosa, Susana Elizabeth; Tissera, Patricia Beatriz; Cataldi, Pedro Anselmo; Di Cintio, Arianna; Dark matter response to galaxy assembly history; EDP Sciences; Astronomy and Astrophysics; 622; A197; 2-2019; 1-17
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/151826
identifier_str_mv Artale, María Celeste; Pedrosa, Susana Elizabeth; Tissera, Patricia Beatriz; Cataldi, Pedro Anselmo; Di Cintio, Arianna; Dark matter response to galaxy assembly history; EDP Sciences; Astronomy and Astrophysics; 622; A197; 2-2019; 1-17
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/doi/10.1051/0004-6361/201834096
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1901.02269v1
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2019/02/aa34096-18/aa34096-18.html
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
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 13.22299

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