Simulating the spatial distribution and kinematics of globular clusters within galaxy clusters in illustris
- Autores
- Ramos Almendares, Felipe Alberto; Sales, Laura Virginia; Abadi, Mario Gabriel; Muriel, Hernan; Doppel, Jessica E.; Peng, Eric W.
- Año de publicación
- 2020
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- We study the assembly of globular clusters (GCs) in 9 galaxy clusters using the cosmological simulation Illustris. GCs are tagged to individual galaxies at their infall time. The tidal removal of GCs from their galaxies and the distribution of the GCs within the cluster is later followed self-consistently by the simulation. The method relies on the simple assumption of a single power-law relation between halo mass (Mvir) and mass in GCs (MGC) as found in observations. We find that the GCs specific frequency SN as a function of V-band magnitude naturally reproduces the observed ‘U’-shape due to the combination of the power law MGC–Mvir relation and the non-linear stellar mass (M∗)–halo mass relation from the simulation. Additional scatter in the SN values is traced back to galaxies with early infall times due to the evolution of the M∗–Mvir relation with redshift. GCs that have been tidally removed from their galaxies form the present-day intracluster component, from which about ∼60 per cent were brought in by galaxies that currently orbit within the cluster potential. The remaining ‘orphan’ GCs are contributed by satellite galaxies with a wide range of stellar masses that are fully tidally disrupted at z = 0. This intracluster component is a good dynamical tracer of the dark matter potential. As a consequence of the accreted nature of most intracluster GCs, their orbits are fairly radial with a predicted orbital anisotropy β ≥ 0.5. However, local tangential motions may appear as a consequence of localized substructure, providing a possible interpretation to the β < 0 values suggested in observations of M87.
Fil: Ramos Almendares, Felipe Alberto. 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: Sales, Laura Virginia. University of California; Estados Unidos. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina
Fil: Abadi, Mario Gabriel. 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: Muriel, Hernan. 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. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina
Fil: Doppel, Jessica E.. University of California; Estados Unidos
Fil: Peng, Eric W.. Peking University; China - Materia
-
GALAXIES: CLUSTERS: GENERAL
GALAXIES: HALOES
GALAXIES: STAR CLUSTERS: GENERAL - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-nd/2.5/ar/
- Repositorio
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/147862
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Simulating the spatial distribution and kinematics of globular clusters within galaxy clusters in illustrisRamos Almendares, Felipe AlbertoSales, Laura VirginiaAbadi, Mario GabrielMuriel, HernanDoppel, Jessica E.Peng, Eric W.GALAXIES: CLUSTERS: GENERALGALAXIES: HALOESGALAXIES: STAR CLUSTERS: GENERALhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We study the assembly of globular clusters (GCs) in 9 galaxy clusters using the cosmological simulation Illustris. GCs are tagged to individual galaxies at their infall time. The tidal removal of GCs from their galaxies and the distribution of the GCs within the cluster is later followed self-consistently by the simulation. The method relies on the simple assumption of a single power-law relation between halo mass (Mvir) and mass in GCs (MGC) as found in observations. We find that the GCs specific frequency SN as a function of V-band magnitude naturally reproduces the observed ‘U’-shape due to the combination of the power law MGC–Mvir relation and the non-linear stellar mass (M∗)–halo mass relation from the simulation. Additional scatter in the SN values is traced back to galaxies with early infall times due to the evolution of the M∗–Mvir relation with redshift. GCs that have been tidally removed from their galaxies form the present-day intracluster component, from which about ∼60 per cent were brought in by galaxies that currently orbit within the cluster potential. The remaining ‘orphan’ GCs are contributed by satellite galaxies with a wide range of stellar masses that are fully tidally disrupted at z = 0. This intracluster component is a good dynamical tracer of the dark matter potential. As a consequence of the accreted nature of most intracluster GCs, their orbits are fairly radial with a predicted orbital anisotropy β ≥ 0.5. However, local tangential motions may appear as a consequence of localized substructure, providing a possible interpretation to the β < 0 values suggested in observations of M87.Fil: Ramos Almendares, Felipe Alberto. 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: Sales, Laura Virginia. University of California; Estados Unidos. Consejo Nacional de Investigaciones Científicas y Técnicas; ArgentinaFil: Abadi, Mario Gabriel. 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: Muriel, Hernan. 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. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; ArgentinaFil: Doppel, Jessica E.. University of California; Estados UnidosFil: Peng, Eric W.. Peking University; ChinaOxford University Press2020-04info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/147862Ramos Almendares, Felipe Alberto; Sales, Laura Virginia; Abadi, Mario Gabriel; Muriel, Hernan; Doppel, Jessica E.; et al.; Simulating the spatial distribution and kinematics of globular clusters within galaxy clusters in illustris; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 493; 4; 4-2020; 5357-53680035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/493/4/5357/5758313info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/staa551info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-nd/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:37:20Zoai:ri.conicet.gov.ar:11336/147862instacron: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:34982025-09-29 09:37:20.403CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
dc.title.none.fl_str_mv |
Simulating the spatial distribution and kinematics of globular clusters within galaxy clusters in illustris |
title |
Simulating the spatial distribution and kinematics of globular clusters within galaxy clusters in illustris |
spellingShingle |
Simulating the spatial distribution and kinematics of globular clusters within galaxy clusters in illustris Ramos Almendares, Felipe Alberto GALAXIES: CLUSTERS: GENERAL GALAXIES: HALOES GALAXIES: STAR CLUSTERS: GENERAL |
title_short |
Simulating the spatial distribution and kinematics of globular clusters within galaxy clusters in illustris |
title_full |
Simulating the spatial distribution and kinematics of globular clusters within galaxy clusters in illustris |
title_fullStr |
Simulating the spatial distribution and kinematics of globular clusters within galaxy clusters in illustris |
title_full_unstemmed |
Simulating the spatial distribution and kinematics of globular clusters within galaxy clusters in illustris |
title_sort |
Simulating the spatial distribution and kinematics of globular clusters within galaxy clusters in illustris |
dc.creator.none.fl_str_mv |
Ramos Almendares, Felipe Alberto Sales, Laura Virginia Abadi, Mario Gabriel Muriel, Hernan Doppel, Jessica E. Peng, Eric W. |
author |
Ramos Almendares, Felipe Alberto |
author_facet |
Ramos Almendares, Felipe Alberto Sales, Laura Virginia Abadi, Mario Gabriel Muriel, Hernan Doppel, Jessica E. Peng, Eric W. |
author_role |
author |
author2 |
Sales, Laura Virginia Abadi, Mario Gabriel Muriel, Hernan Doppel, Jessica E. Peng, Eric W. |
author2_role |
author author author author author |
dc.subject.none.fl_str_mv |
GALAXIES: CLUSTERS: GENERAL GALAXIES: HALOES GALAXIES: STAR CLUSTERS: GENERAL |
topic |
GALAXIES: CLUSTERS: GENERAL GALAXIES: HALOES GALAXIES: STAR CLUSTERS: GENERAL |
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 study the assembly of globular clusters (GCs) in 9 galaxy clusters using the cosmological simulation Illustris. GCs are tagged to individual galaxies at their infall time. The tidal removal of GCs from their galaxies and the distribution of the GCs within the cluster is later followed self-consistently by the simulation. The method relies on the simple assumption of a single power-law relation between halo mass (Mvir) and mass in GCs (MGC) as found in observations. We find that the GCs specific frequency SN as a function of V-band magnitude naturally reproduces the observed ‘U’-shape due to the combination of the power law MGC–Mvir relation and the non-linear stellar mass (M∗)–halo mass relation from the simulation. Additional scatter in the SN values is traced back to galaxies with early infall times due to the evolution of the M∗–Mvir relation with redshift. GCs that have been tidally removed from their galaxies form the present-day intracluster component, from which about ∼60 per cent were brought in by galaxies that currently orbit within the cluster potential. The remaining ‘orphan’ GCs are contributed by satellite galaxies with a wide range of stellar masses that are fully tidally disrupted at z = 0. This intracluster component is a good dynamical tracer of the dark matter potential. As a consequence of the accreted nature of most intracluster GCs, their orbits are fairly radial with a predicted orbital anisotropy β ≥ 0.5. However, local tangential motions may appear as a consequence of localized substructure, providing a possible interpretation to the β < 0 values suggested in observations of M87. Fil: Ramos Almendares, Felipe Alberto. 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: Sales, Laura Virginia. University of California; Estados Unidos. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina Fil: Abadi, Mario Gabriel. 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: Muriel, Hernan. 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. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina Fil: Doppel, Jessica E.. University of California; Estados Unidos Fil: Peng, Eric W.. Peking University; China |
description |
We study the assembly of globular clusters (GCs) in 9 galaxy clusters using the cosmological simulation Illustris. GCs are tagged to individual galaxies at their infall time. The tidal removal of GCs from their galaxies and the distribution of the GCs within the cluster is later followed self-consistently by the simulation. The method relies on the simple assumption of a single power-law relation between halo mass (Mvir) and mass in GCs (MGC) as found in observations. We find that the GCs specific frequency SN as a function of V-band magnitude naturally reproduces the observed ‘U’-shape due to the combination of the power law MGC–Mvir relation and the non-linear stellar mass (M∗)–halo mass relation from the simulation. Additional scatter in the SN values is traced back to galaxies with early infall times due to the evolution of the M∗–Mvir relation with redshift. GCs that have been tidally removed from their galaxies form the present-day intracluster component, from which about ∼60 per cent were brought in by galaxies that currently orbit within the cluster potential. The remaining ‘orphan’ GCs are contributed by satellite galaxies with a wide range of stellar masses that are fully tidally disrupted at z = 0. This intracluster component is a good dynamical tracer of the dark matter potential. As a consequence of the accreted nature of most intracluster GCs, their orbits are fairly radial with a predicted orbital anisotropy β ≥ 0.5. However, local tangential motions may appear as a consequence of localized substructure, providing a possible interpretation to the β < 0 values suggested in observations of M87. |
publishDate |
2020 |
dc.date.none.fl_str_mv |
2020-04 |
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/11336/147862 Ramos Almendares, Felipe Alberto; Sales, Laura Virginia; Abadi, Mario Gabriel; Muriel, Hernan; Doppel, Jessica E.; et al.; Simulating the spatial distribution and kinematics of globular clusters within galaxy clusters in illustris; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 493; 4; 4-2020; 5357-5368 0035-8711 CONICET Digital CONICET |
url |
http://hdl.handle.net/11336/147862 |
identifier_str_mv |
Ramos Almendares, Felipe Alberto; Sales, Laura Virginia; Abadi, Mario Gabriel; Muriel, Hernan; Doppel, Jessica E.; et al.; Simulating the spatial distribution and kinematics of globular clusters within galaxy clusters in illustris; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 493; 4; 4-2020; 5357-5368 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/493/4/5357/5758313 info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/staa551 |
dc.rights.none.fl_str_mv |
info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by-nc-nd/2.5/ar/ |
eu_rights_str_mv |
openAccess |
rights_invalid_str_mv |
https://creativecommons.org/licenses/by-nc-nd/2.5/ar/ |
dc.format.none.fl_str_mv |
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 |
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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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1844613176191090688 |
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13.070432 |