The relation between halo shape, velocity dispersion and formation time

Autores
Ragone Figueroa, Cinthia Judith; Plionis, M.; Merchan, Manuel Enrique; Gottlöber, S.; Yepes, G.
Año de publicación
2010
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We use dark matter haloes identified in the MareNostrum Universe and galaxy groups identified in the Sloan Data Release 7 galaxy catalogue, to study the relation between halo shape and halo dynamics, parametrizing out the mass of the systems. A strong shape-dynamics, independent of mass, correlation is present in the simulation data, which we find it to be due to different halo formation times. Early formation time haloes are, at the present epoch, more spherical and have higher velocity dispersions than late forming-timehaloes. The halo shape-dynamics correlation, albeit weaker, survives the projection in 2D (ie., among projected shape and 1-D velocity dispersion). A similar shape-dynamics  correlation, independent of mass, is also found in the SDSS DR7 groups of galaxies and in order to investigate its cause we have tested and used, as a proxy of the group formation time, a concentration parameter. We have found, as in the case of the simulated haloes, that less concentrated groups, corresponding to late formation times, have lower velocity dispersions and higher elongations than groups with higher values of concentration,corresponding to early formation times.
Fil: Ragone Figueroa, Cinthia Judith. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina
Fil: Plionis, M.. Instituto Nacional de Astrofísica Óptica y Electrónica; México
Fil: Merchan, Manuel Enrique. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina
Fil: Gottlöber, S.. No especifíca;
Fil: Yepes, G.. Universidad Autónoma de Madrid; España
Materia
GALAXIES: CLUSTERS: GENERAL
GALAXIES: HALOES
COSMOLOGY: DARK MATTER
METHODS: N-BODY 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:11336/277184
Acceder
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network_name_str CONICET Digital (CONICET)
spelling The relation between halo shape, velocity dispersion and formation timeRagone Figueroa, Cinthia JudithPlionis, M.Merchan, Manuel EnriqueGottlöber, S.Yepes, G.GALAXIES: CLUSTERS: GENERALGALAXIES: HALOESCOSMOLOGY: DARK MATTERMETHODS: N-BODY SIMULATIONShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We use dark matter haloes identified in the MareNostrum Universe and galaxy groups identified in the Sloan Data Release 7 galaxy catalogue, to study the relation between halo shape and halo dynamics, parametrizing out the mass of the systems. A strong shape-dynamics, independent of mass, correlation is present in the simulation data, which we find it to be due to different halo formation times. Early formation time haloes are, at the present epoch, more spherical and have higher velocity dispersions than late forming-timehaloes. The halo shape-dynamics correlation, albeit weaker, survives the projection in 2D (ie., among projected shape and 1-D velocity dispersion). A similar shape-dynamics  correlation, independent of mass, is also found in the SDSS DR7 groups of galaxies and in order to investigate its cause we have tested and used, as a proxy of the group formation time, a concentration parameter. We have found, as in the case of the simulated haloes, that less concentrated groups, corresponding to late formation times, have lower velocity dispersions and higher elongations than groups with higher values of concentration,corresponding to early formation times.Fil: Ragone Figueroa, Cinthia Judith. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; ArgentinaFil: Plionis, M.. Instituto Nacional de Astrofísica Óptica y Electrónica; MéxicoFil: Merchan, Manuel Enrique. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; ArgentinaFil: Gottlöber, S.. No especifíca;Fil: Yepes, G.. Universidad Autónoma de Madrid; EspañaWiley Blackwell Publishing, Inc2010-09info: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/11336/277184Ragone Figueroa, Cinthia Judith; Plionis, M.; Merchan, Manuel Enrique; Gottlöber, S.; Yepes, G.; The relation between halo shape, velocity dispersion and formation time; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 407; 1; 9-2010; 581-5890035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/407/1/581/986146info:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2010.16935.xinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-12-23T13:42:00Zoai:ri.conicet.gov.ar:11336/277184instacron: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:34982025-12-23 13:42:00.902CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv The relation between halo shape, velocity dispersion and formation time
title The relation between halo shape, velocity dispersion and formation time
spellingShingle The relation between halo shape, velocity dispersion and formation time
Ragone Figueroa, Cinthia Judith
GALAXIES: CLUSTERS: GENERAL
GALAXIES: HALOES
COSMOLOGY: DARK MATTER
METHODS: N-BODY SIMULATIONS
title_short The relation between halo shape, velocity dispersion and formation time
title_full The relation between halo shape, velocity dispersion and formation time
title_fullStr The relation between halo shape, velocity dispersion and formation time
title_full_unstemmed The relation between halo shape, velocity dispersion and formation time
title_sort The relation between halo shape, velocity dispersion and formation time
dc.creator.none.fl_str_mv Ragone Figueroa, Cinthia Judith
Plionis, M.
Merchan, Manuel Enrique
Gottlöber, S.
Yepes, G.
author Ragone Figueroa, Cinthia Judith
author_facet Ragone Figueroa, Cinthia Judith
Plionis, M.
Merchan, Manuel Enrique
Gottlöber, S.
Yepes, G.
author_role author
author2 Plionis, M.
Merchan, Manuel Enrique
Gottlöber, S.
Yepes, G.
author2_role author
author
author
author
dc.subject.none.fl_str_mv GALAXIES: CLUSTERS: GENERAL
GALAXIES: HALOES
COSMOLOGY: DARK MATTER
METHODS: N-BODY SIMULATIONS
topic GALAXIES: CLUSTERS: GENERAL
GALAXIES: HALOES
COSMOLOGY: DARK MATTER
METHODS: N-BODY 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 We use dark matter haloes identified in the MareNostrum Universe and galaxy groups identified in the Sloan Data Release 7 galaxy catalogue, to study the relation between halo shape and halo dynamics, parametrizing out the mass of the systems. A strong shape-dynamics, independent of mass, correlation is present in the simulation data, which we find it to be due to different halo formation times. Early formation time haloes are, at the present epoch, more spherical and have higher velocity dispersions than late forming-timehaloes. The halo shape-dynamics correlation, albeit weaker, survives the projection in 2D (ie., among projected shape and 1-D velocity dispersion). A similar shape-dynamics  correlation, independent of mass, is also found in the SDSS DR7 groups of galaxies and in order to investigate its cause we have tested and used, as a proxy of the group formation time, a concentration parameter. We have found, as in the case of the simulated haloes, that less concentrated groups, corresponding to late formation times, have lower velocity dispersions and higher elongations than groups with higher values of concentration,corresponding to early formation times.
Fil: Ragone Figueroa, Cinthia Judith. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina
Fil: Plionis, M.. Instituto Nacional de Astrofísica Óptica y Electrónica; México
Fil: Merchan, Manuel Enrique. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina
Fil: Gottlöber, S.. No especifíca;
Fil: Yepes, G.. Universidad Autónoma de Madrid; España
description We use dark matter haloes identified in the MareNostrum Universe and galaxy groups identified in the Sloan Data Release 7 galaxy catalogue, to study the relation between halo shape and halo dynamics, parametrizing out the mass of the systems. A strong shape-dynamics, independent of mass, correlation is present in the simulation data, which we find it to be due to different halo formation times. Early formation time haloes are, at the present epoch, more spherical and have higher velocity dispersions than late forming-timehaloes. The halo shape-dynamics correlation, albeit weaker, survives the projection in 2D (ie., among projected shape and 1-D velocity dispersion). A similar shape-dynamics  correlation, independent of mass, is also found in the SDSS DR7 groups of galaxies and in order to investigate its cause we have tested and used, as a proxy of the group formation time, a concentration parameter. We have found, as in the case of the simulated haloes, that less concentrated groups, corresponding to late formation times, have lower velocity dispersions and higher elongations than groups with higher values of concentration,corresponding to early formation times.
publishDate 2010
dc.date.none.fl_str_mv 2010-09
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/11336/277184
Ragone Figueroa, Cinthia Judith; Plionis, M.; Merchan, Manuel Enrique; Gottlöber, S.; Yepes, G.; The relation between halo shape, velocity dispersion and formation time; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 407; 1; 9-2010; 581-589
0035-8711
CONICET Digital
CONICET
url http://hdl.handle.net/11336/277184
identifier_str_mv Ragone Figueroa, Cinthia Judith; Plionis, M.; Merchan, Manuel Enrique; Gottlöber, S.; Yepes, G.; The relation between halo shape, velocity dispersion and formation time; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 407; 1; 9-2010; 581-589
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/url/https://academic.oup.com/mnras/article/407/1/581/986146
info:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2010.16935.x
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 Wiley Blackwell Publishing, Inc
publisher.none.fl_str_mv Wiley Blackwell Publishing, Inc
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 12.441415

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