The impact of baryons on dark matter haloes

Autores
Pedrosa, Susana Elizabeth; Tissera, Patricia Beatriz; Scannapieco, Cecilia
Año de publicación
2009
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We analyse the dark matter (DM) distribution in an ≈1012 M halo extracted from a simulation consistent with the concordance cosmology, where the physics regulating the transformation of gas into stars was allowed to change producing galaxies with different morphologies. Although the DM profiles get more concentrated as baryons are collected at the centre of the haloes compared to a pure dynamical run, the total baryonic mass alone is not enough to fully predict the reaction of the DM profile. We also note that baryons affect the DM distribution even outside the central regions. Those systems where the transformation of gas into stars is regulated by supernova (SN) feedback, so that significant disc structures are able to form, are found to have more concentrated DM profiles than a galaxy which has efficiently transformed most of its baryons into stars at early times. The accretion of satellites is found to be associated with an expansion of the DM profiles, triggered by angular momentum transfer from the incoming satellites. As the impact of SN feedback increases, the satellites get less massive and are even strongly disrupted before getting close to the main structure causing less angular momentum transfer. Our findings suggest that the response of the DM halo is driven by the history of assembly of baryons into a galaxy along their merger tree.
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: Scannapieco, Cecilia. Gobierno de la Republica Federal de Alemania. Max Planck Institut Fur Astrophysik; Alemania. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina
Materia
GALAXIES HALOES
GALAXIES STRUCTURE
DARK MATTER
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:11336/21846
Acceder
id CONICETDig_461d85288bba7d6f4d05651b0249d383
oai_identifier_str oai:ri.conicet.gov.ar:11336/21846
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling The impact of baryons on dark matter haloesPedrosa, Susana ElizabethTissera, Patricia BeatrizScannapieco, CeciliaGALAXIES HALOESGALAXIES STRUCTUREDARK MATTERhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We analyse the dark matter (DM) distribution in an ≈1012 M halo extracted from a simulation consistent with the concordance cosmology, where the physics regulating the transformation of gas into stars was allowed to change producing galaxies with different morphologies. Although the DM profiles get more concentrated as baryons are collected at the centre of the haloes compared to a pure dynamical run, the total baryonic mass alone is not enough to fully predict the reaction of the DM profile. We also note that baryons affect the DM distribution even outside the central regions. Those systems where the transformation of gas into stars is regulated by supernova (SN) feedback, so that significant disc structures are able to form, are found to have more concentrated DM profiles than a galaxy which has efficiently transformed most of its baryons into stars at early times. The accretion of satellites is found to be associated with an expansion of the DM profiles, triggered by angular momentum transfer from the incoming satellites. As the impact of SN feedback increases, the satellites get less massive and are even strongly disrupted before getting close to the main structure causing less angular momentum transfer. Our findings suggest that the response of the DM halo is driven by the history of assembly of baryons into a galaxy along their merger tree.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: Scannapieco, Cecilia. Gobierno de la Republica Federal de Alemania. Max Planck Institut Fur Astrophysik; Alemania. Consejo Nacional de Investigaciones Científicas y Técnicas; ArgentinaOxford University Press2009-05info: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/11336/21846Pedrosa, Susana Elizabeth; Tissera, Patricia Beatriz; Scannapieco, Cecilia; The impact of baryons on dark matter haloes; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 395; 1; 5-2009; L57-L610035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1111/j.1745-3933.2009.00641.xinfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnrasl/article-lookup/doi/10.1111/j.1745-3933.2009.00641.xinfo:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/0902.2100info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-03T10:07:23Zoai:ri.conicet.gov.ar:11336/21846instacron: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 10:07:23.488CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv The impact of baryons on dark matter haloes
title The impact of baryons on dark matter haloes
spellingShingle The impact of baryons on dark matter haloes
Pedrosa, Susana Elizabeth
GALAXIES HALOES
GALAXIES STRUCTURE
DARK MATTER
title_short The impact of baryons on dark matter haloes
title_full The impact of baryons on dark matter haloes
title_fullStr The impact of baryons on dark matter haloes
title_full_unstemmed The impact of baryons on dark matter haloes
title_sort The impact of baryons on dark matter haloes
dc.creator.none.fl_str_mv Pedrosa, Susana Elizabeth
Tissera, Patricia Beatriz
Scannapieco, Cecilia
author Pedrosa, Susana Elizabeth
author_facet Pedrosa, Susana Elizabeth
Tissera, Patricia Beatriz
Scannapieco, Cecilia
author_role author
author2 Tissera, Patricia Beatriz
Scannapieco, Cecilia
author2_role author
author
dc.subject.none.fl_str_mv GALAXIES HALOES
GALAXIES STRUCTURE
DARK MATTER
topic GALAXIES HALOES
GALAXIES STRUCTURE
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 We analyse the dark matter (DM) distribution in an ≈1012 M halo extracted from a simulation consistent with the concordance cosmology, where the physics regulating the transformation of gas into stars was allowed to change producing galaxies with different morphologies. Although the DM profiles get more concentrated as baryons are collected at the centre of the haloes compared to a pure dynamical run, the total baryonic mass alone is not enough to fully predict the reaction of the DM profile. We also note that baryons affect the DM distribution even outside the central regions. Those systems where the transformation of gas into stars is regulated by supernova (SN) feedback, so that significant disc structures are able to form, are found to have more concentrated DM profiles than a galaxy which has efficiently transformed most of its baryons into stars at early times. The accretion of satellites is found to be associated with an expansion of the DM profiles, triggered by angular momentum transfer from the incoming satellites. As the impact of SN feedback increases, the satellites get less massive and are even strongly disrupted before getting close to the main structure causing less angular momentum transfer. Our findings suggest that the response of the DM halo is driven by the history of assembly of baryons into a galaxy along their merger tree.
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: Scannapieco, Cecilia. Gobierno de la Republica Federal de Alemania. Max Planck Institut Fur Astrophysik; Alemania. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina
description We analyse the dark matter (DM) distribution in an ≈1012 M halo extracted from a simulation consistent with the concordance cosmology, where the physics regulating the transformation of gas into stars was allowed to change producing galaxies with different morphologies. Although the DM profiles get more concentrated as baryons are collected at the centre of the haloes compared to a pure dynamical run, the total baryonic mass alone is not enough to fully predict the reaction of the DM profile. We also note that baryons affect the DM distribution even outside the central regions. Those systems where the transformation of gas into stars is regulated by supernova (SN) feedback, so that significant disc structures are able to form, are found to have more concentrated DM profiles than a galaxy which has efficiently transformed most of its baryons into stars at early times. The accretion of satellites is found to be associated with an expansion of the DM profiles, triggered by angular momentum transfer from the incoming satellites. As the impact of SN feedback increases, the satellites get less massive and are even strongly disrupted before getting close to the main structure causing less angular momentum transfer. Our findings suggest that the response of the DM halo is driven by the history of assembly of baryons into a galaxy along their merger tree.
publishDate 2009
dc.date.none.fl_str_mv 2009-05
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/11336/21846
Pedrosa, Susana Elizabeth; Tissera, Patricia Beatriz; Scannapieco, Cecilia; The impact of baryons on dark matter haloes; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 395; 1; 5-2009; L57-L61
0035-8711
CONICET Digital
CONICET
url http://hdl.handle.net/11336/21846
identifier_str_mv Pedrosa, Susana Elizabeth; Tissera, Patricia Beatriz; Scannapieco, Cecilia; The impact of baryons on dark matter haloes; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 395; 1; 5-2009; L57-L61
0035-8711
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1111/j.1745-3933.2009.00641.x
info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnrasl/article-lookup/doi/10.1111/j.1745-3933.2009.00641.x
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/0902.2100
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
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
_version_ 1842270001628708864
score 13.13397

Publicaciones similares