On the dynamical origin of the ICM metallicity evolution
- Autores
- Cora, Sofia Alejandra; Tornatore, Luca; Tozzi, Paolo; Dolag, Klaus
- Año de publicación
- 2008
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- We present a study on the origin of the metallicity evolution of the intra-cluster medium (ICM) by applying a semi-analytic model of galaxy formation to N-body/smoothed particle hydrodynamic (SPH) non-radiative numerical simulations of clusters of galaxies. The semi-analytic model includes gas cooling, star formation, supernovae feedback and metal enrichment, and is linked to the diffuse gas of the underlying simulations so that the chemical properties of gas particles are dynamically and consistently generated from stars in the galaxies. This hybrid model lets us have information on the spatial distribution of metals in the ICM. The results obtained for a set of clusters with virial masses of ∼1.5 × 1015 h−1 M contribute to the theoretical interpretation of recent observational X-ray data, which indicate a decrease of the average iron content of the intra-cluster gas with increasing redshift. We find that this evolution arises mainly as a result of a progressive increase of the iron abundance within ∼0.15 Rvir. The clusters have been considerably enriched by z ∼ 1 with very low contribution from recent star formation. Low entropy gas that has been enriched at high redshift sinks to the cluster centre contributing to the evolution of the metallicity profiles.
Fil: Cora, Sofia Alejandra. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Tornatore, Luca. Istituto Nazionale Di Astrofisica; Italia
Fil: Tozzi, Paolo. Istituto Nazionale Di Astrofisica; Italia
Fil: Dolag, Klaus. Max-Planck-Institut fur Astrophysik; Alemania - Materia
-
Numerical methods
Galaxies
Cosmology
X-ray galaxies
Clusters of galaxies - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
.jpg)
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/43219
Ver los metadatos del registro completo
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On the dynamical origin of the ICM metallicity evolutionCora, Sofia AlejandraTornatore, LucaTozzi, PaoloDolag, KlausNumerical methodsGalaxiesCosmologyX-ray galaxiesClusters of galaxieshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We present a study on the origin of the metallicity evolution of the intra-cluster medium (ICM) by applying a semi-analytic model of galaxy formation to N-body/smoothed particle hydrodynamic (SPH) non-radiative numerical simulations of clusters of galaxies. The semi-analytic model includes gas cooling, star formation, supernovae feedback and metal enrichment, and is linked to the diffuse gas of the underlying simulations so that the chemical properties of gas particles are dynamically and consistently generated from stars in the galaxies. This hybrid model lets us have information on the spatial distribution of metals in the ICM. The results obtained for a set of clusters with virial masses of ∼1.5 × 1015 h−1 M contribute to the theoretical interpretation of recent observational X-ray data, which indicate a decrease of the average iron content of the intra-cluster gas with increasing redshift. We find that this evolution arises mainly as a result of a progressive increase of the iron abundance within ∼0.15 Rvir. The clusters have been considerably enriched by z ∼ 1 with very low contribution from recent star formation. Low entropy gas that has been enriched at high redshift sinks to the cluster centre contributing to the evolution of the metallicity profiles.Fil: Cora, Sofia Alejandra. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaFil: Tornatore, Luca. Istituto Nazionale Di Astrofisica; ItaliaFil: Tozzi, Paolo. Istituto Nazionale Di Astrofisica; ItaliaFil: Dolag, Klaus. Max-Planck-Institut fur Astrophysik; AlemaniaWiley Blackwell Publishing, Inc2008-12info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/43219Cora, Sofia Alejandra; Tornatore, Luca ; Tozzi, Paolo ; Dolag, Klaus ; On the dynamical origin of the ICM metallicity evolution; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 306; 12-2008; 96-1040035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2008.13068.xinfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/386/1/96/977131info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:31:33Zoai:ri.conicet.gov.ar:11336/43219instacron: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 10:31:33.745CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| dc.title.none.fl_str_mv |
On the dynamical origin of the ICM metallicity evolution |
| title |
On the dynamical origin of the ICM metallicity evolution |
| spellingShingle |
On the dynamical origin of the ICM metallicity evolution Cora, Sofia Alejandra Numerical methods Galaxies Cosmology X-ray galaxies Clusters of galaxies |
| title_short |
On the dynamical origin of the ICM metallicity evolution |
| title_full |
On the dynamical origin of the ICM metallicity evolution |
| title_fullStr |
On the dynamical origin of the ICM metallicity evolution |
| title_full_unstemmed |
On the dynamical origin of the ICM metallicity evolution |
| title_sort |
On the dynamical origin of the ICM metallicity evolution |
| dc.creator.none.fl_str_mv |
Cora, Sofia Alejandra Tornatore, Luca Tozzi, Paolo Dolag, Klaus |
| author |
Cora, Sofia Alejandra |
| author_facet |
Cora, Sofia Alejandra Tornatore, Luca Tozzi, Paolo Dolag, Klaus |
| author_role |
author |
| author2 |
Tornatore, Luca Tozzi, Paolo Dolag, Klaus |
| author2_role |
author author author |
| dc.subject.none.fl_str_mv |
Numerical methods Galaxies Cosmology X-ray galaxies Clusters of galaxies |
| topic |
Numerical methods Galaxies Cosmology X-ray galaxies Clusters of galaxies |
| 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 present a study on the origin of the metallicity evolution of the intra-cluster medium (ICM) by applying a semi-analytic model of galaxy formation to N-body/smoothed particle hydrodynamic (SPH) non-radiative numerical simulations of clusters of galaxies. The semi-analytic model includes gas cooling, star formation, supernovae feedback and metal enrichment, and is linked to the diffuse gas of the underlying simulations so that the chemical properties of gas particles are dynamically and consistently generated from stars in the galaxies. This hybrid model lets us have information on the spatial distribution of metals in the ICM. The results obtained for a set of clusters with virial masses of ∼1.5 × 1015 h−1 M contribute to the theoretical interpretation of recent observational X-ray data, which indicate a decrease of the average iron content of the intra-cluster gas with increasing redshift. We find that this evolution arises mainly as a result of a progressive increase of the iron abundance within ∼0.15 Rvir. The clusters have been considerably enriched by z ∼ 1 with very low contribution from recent star formation. Low entropy gas that has been enriched at high redshift sinks to the cluster centre contributing to the evolution of the metallicity profiles. Fil: Cora, Sofia Alejandra. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina Fil: Tornatore, Luca. Istituto Nazionale Di Astrofisica; Italia Fil: Tozzi, Paolo. Istituto Nazionale Di Astrofisica; Italia Fil: Dolag, Klaus. Max-Planck-Institut fur Astrophysik; Alemania |
| description |
We present a study on the origin of the metallicity evolution of the intra-cluster medium (ICM) by applying a semi-analytic model of galaxy formation to N-body/smoothed particle hydrodynamic (SPH) non-radiative numerical simulations of clusters of galaxies. The semi-analytic model includes gas cooling, star formation, supernovae feedback and metal enrichment, and is linked to the diffuse gas of the underlying simulations so that the chemical properties of gas particles are dynamically and consistently generated from stars in the galaxies. This hybrid model lets us have information on the spatial distribution of metals in the ICM. The results obtained for a set of clusters with virial masses of ∼1.5 × 1015 h−1 M contribute to the theoretical interpretation of recent observational X-ray data, which indicate a decrease of the average iron content of the intra-cluster gas with increasing redshift. We find that this evolution arises mainly as a result of a progressive increase of the iron abundance within ∼0.15 Rvir. The clusters have been considerably enriched by z ∼ 1 with very low contribution from recent star formation. Low entropy gas that has been enriched at high redshift sinks to the cluster centre contributing to the evolution of the metallicity profiles. |
| publishDate |
2008 |
| dc.date.none.fl_str_mv |
2008-12 |
| 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/11336/43219 Cora, Sofia Alejandra; Tornatore, Luca ; Tozzi, Paolo ; Dolag, Klaus ; On the dynamical origin of the ICM metallicity evolution; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 306; 12-2008; 96-104 0035-8711 CONICET Digital CONICET |
| url |
http://hdl.handle.net/11336/43219 |
| identifier_str_mv |
Cora, Sofia Alejandra; Tornatore, Luca ; Tozzi, Paolo ; Dolag, Klaus ; On the dynamical origin of the ICM metallicity evolution; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 306; 12-2008; 96-104 0035-8711 CONICET Digital CONICET |
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eng |
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eng |
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info:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2008.13068.x info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/386/1/96/977131 |
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openAccess |
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application/pdf application/pdf |
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Wiley Blackwell Publishing, Inc |
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Wiley Blackwell Publishing, Inc |
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