Dust evolution in galaxy cluster simulations

Autores
Gjergo, Eda; Granato, Gian Luigi; Murante, Giuseppe; Ragone Figueroa, Cinthia Judith; Tornatore, Luca; Borgani, Stefano
Año de publicación
2018
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We implement a state-of-the-art treatment of the processes affecting the production and Interstellar Medium (ISM) evolution of carbonaceous and silicate dust grains within SPH simulations. We trace the dust grain size distribution by means of a two-size approximation. We test our method on zoom-in simulations of four massive (M200 ≥ 3 × 1014M⊙) galaxy clusters. We predict that during the early stages of assembly of the cluster at z ≳ 3, where the star formation activity is at its maximum in our simulations, the proto-cluster regions are rich in dusty gas. Compared to the case in which only dust production in stellar ejecta is active, if we include processes occurring in the cold ISM, the dust content is enhanced by a factor 2-3. However, the dust properties in this stage turn out to be significantly different from those observationally derived for the average Milky Way dust, and commonly adopted in calculations of dust reprocessing.We show that these differences may have a strong impact on the predicted spectral energy distributions. At low redshift in star-forming regions our model reproduces reasonably well the trend of dust abundances over metallicity as observed in local galaxies. However we underproduce by a factor of 2-3 the total dust content of clusters estimated observationally at low redshift, z ≲ 0.5 using IRAS, Planck, and Herschel satellites data. This discrepancy does not subsist by assuming a lower sputtering efficiency, which erodes dust grains in the hot intracluster medium.
Fil: Gjergo, Eda. Università degli Studi di Trieste; Italia. Osservatorio Astronómico di Trieste; Italia
Fil: Granato, Gian Luigi. Osservatorio Astronómico di Trieste; Italia. Istituto Nazionale di Astrofisica; Italia. 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: Murante, Giuseppe. Osservatorio Astronómico di Trieste; Italia. 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. Istituto Nazionale di Astrofisica; Italia
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. Osservatorio Astronómico di Trieste; Italia
Fil: Tornatore, Luca. Istituto Nazionale di Astrofisica; Italia. Osservatorio Astronómico di Trieste; Italia
Fil: Borgani, Stefano. Osservatorio Astronómico di Trieste; Italia. Istituto Nazionale di Astrofisica; Italia. Università degli Studi di Trieste; Italia
Materia
GALAXIES: CLUSTERS: GENERAL
GALAXIES: CLUSTERS: INTRACLUSTER MEDIUM
GALAXIES: EVOLUTION
ISM: EVOLUTION
METHODS: NUMERICAL
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:11336/86948
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/86948
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Dust evolution in galaxy cluster simulationsGjergo, EdaGranato, Gian LuigiMurante, GiuseppeRagone Figueroa, Cinthia JudithTornatore, LucaBorgani, StefanoGALAXIES: CLUSTERS: GENERALGALAXIES: CLUSTERS: INTRACLUSTER MEDIUMGALAXIES: EVOLUTIONISM: EVOLUTIONMETHODS: NUMERICALhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We implement a state-of-the-art treatment of the processes affecting the production and Interstellar Medium (ISM) evolution of carbonaceous and silicate dust grains within SPH simulations. We trace the dust grain size distribution by means of a two-size approximation. We test our method on zoom-in simulations of four massive (M200 ≥ 3 × 1014M⊙) galaxy clusters. We predict that during the early stages of assembly of the cluster at z ≳ 3, where the star formation activity is at its maximum in our simulations, the proto-cluster regions are rich in dusty gas. Compared to the case in which only dust production in stellar ejecta is active, if we include processes occurring in the cold ISM, the dust content is enhanced by a factor 2-3. However, the dust properties in this stage turn out to be significantly different from those observationally derived for the average Milky Way dust, and commonly adopted in calculations of dust reprocessing.We show that these differences may have a strong impact on the predicted spectral energy distributions. At low redshift in star-forming regions our model reproduces reasonably well the trend of dust abundances over metallicity as observed in local galaxies. However we underproduce by a factor of 2-3 the total dust content of clusters estimated observationally at low redshift, z ≲ 0.5 using IRAS, Planck, and Herschel satellites data. This discrepancy does not subsist by assuming a lower sputtering efficiency, which erodes dust grains in the hot intracluster medium.Fil: Gjergo, Eda. Università degli Studi di Trieste; Italia. Osservatorio Astronómico di Trieste; ItaliaFil: Granato, Gian Luigi. Osservatorio Astronómico di Trieste; Italia. Istituto Nazionale di Astrofisica; Italia. 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: Murante, Giuseppe. Osservatorio Astronómico di Trieste; Italia. 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. Istituto Nazionale di Astrofisica; ItaliaFil: 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. Osservatorio Astronómico di Trieste; ItaliaFil: Tornatore, Luca. Istituto Nazionale di Astrofisica; Italia. Osservatorio Astronómico di Trieste; ItaliaFil: Borgani, Stefano. Osservatorio Astronómico di Trieste; Italia. Istituto Nazionale di Astrofisica; Italia. Università degli Studi di Trieste; ItaliaWiley Blackwell Publishing, Inc2018-09info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/86948Gjergo, Eda; Granato, Gian Luigi; Murante, Giuseppe; Ragone Figueroa, Cinthia Judith; Tornatore, Luca; et al.; Dust evolution in galaxy cluster simulations; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 479; 2; 9-2018; 2588-26060035-87111365-2966CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/479/2/2588/5037930info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/sty1564info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:34:03Zoai:ri.conicet.gov.ar:11336/86948instacron: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 09:34:03.593CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Dust evolution in galaxy cluster simulations
title Dust evolution in galaxy cluster simulations
spellingShingle Dust evolution in galaxy cluster simulations
Gjergo, Eda
GALAXIES: CLUSTERS: GENERAL
GALAXIES: CLUSTERS: INTRACLUSTER MEDIUM
GALAXIES: EVOLUTION
ISM: EVOLUTION
METHODS: NUMERICAL
title_short Dust evolution in galaxy cluster simulations
title_full Dust evolution in galaxy cluster simulations
title_fullStr Dust evolution in galaxy cluster simulations
title_full_unstemmed Dust evolution in galaxy cluster simulations
title_sort Dust evolution in galaxy cluster simulations
dc.creator.none.fl_str_mv Gjergo, Eda
Granato, Gian Luigi
Murante, Giuseppe
Ragone Figueroa, Cinthia Judith
Tornatore, Luca
Borgani, Stefano
author Gjergo, Eda
author_facet Gjergo, Eda
Granato, Gian Luigi
Murante, Giuseppe
Ragone Figueroa, Cinthia Judith
Tornatore, Luca
Borgani, Stefano
author_role author
author2 Granato, Gian Luigi
Murante, Giuseppe
Ragone Figueroa, Cinthia Judith
Tornatore, Luca
Borgani, Stefano
author2_role author
author
author
author
author
dc.subject.none.fl_str_mv GALAXIES: CLUSTERS: GENERAL
GALAXIES: CLUSTERS: INTRACLUSTER MEDIUM
GALAXIES: EVOLUTION
ISM: EVOLUTION
METHODS: NUMERICAL
topic GALAXIES: CLUSTERS: GENERAL
GALAXIES: CLUSTERS: INTRACLUSTER MEDIUM
GALAXIES: EVOLUTION
ISM: EVOLUTION
METHODS: NUMERICAL
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 implement a state-of-the-art treatment of the processes affecting the production and Interstellar Medium (ISM) evolution of carbonaceous and silicate dust grains within SPH simulations. We trace the dust grain size distribution by means of a two-size approximation. We test our method on zoom-in simulations of four massive (M200 ≥ 3 × 1014M⊙) galaxy clusters. We predict that during the early stages of assembly of the cluster at z ≳ 3, where the star formation activity is at its maximum in our simulations, the proto-cluster regions are rich in dusty gas. Compared to the case in which only dust production in stellar ejecta is active, if we include processes occurring in the cold ISM, the dust content is enhanced by a factor 2-3. However, the dust properties in this stage turn out to be significantly different from those observationally derived for the average Milky Way dust, and commonly adopted in calculations of dust reprocessing.We show that these differences may have a strong impact on the predicted spectral energy distributions. At low redshift in star-forming regions our model reproduces reasonably well the trend of dust abundances over metallicity as observed in local galaxies. However we underproduce by a factor of 2-3 the total dust content of clusters estimated observationally at low redshift, z ≲ 0.5 using IRAS, Planck, and Herschel satellites data. This discrepancy does not subsist by assuming a lower sputtering efficiency, which erodes dust grains in the hot intracluster medium.
Fil: Gjergo, Eda. Università degli Studi di Trieste; Italia. Osservatorio Astronómico di Trieste; Italia
Fil: Granato, Gian Luigi. Osservatorio Astronómico di Trieste; Italia. Istituto Nazionale di Astrofisica; Italia. 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: Murante, Giuseppe. Osservatorio Astronómico di Trieste; Italia. 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. Istituto Nazionale di Astrofisica; Italia
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. Osservatorio Astronómico di Trieste; Italia
Fil: Tornatore, Luca. Istituto Nazionale di Astrofisica; Italia. Osservatorio Astronómico di Trieste; Italia
Fil: Borgani, Stefano. Osservatorio Astronómico di Trieste; Italia. Istituto Nazionale di Astrofisica; Italia. Università degli Studi di Trieste; Italia
description We implement a state-of-the-art treatment of the processes affecting the production and Interstellar Medium (ISM) evolution of carbonaceous and silicate dust grains within SPH simulations. We trace the dust grain size distribution by means of a two-size approximation. We test our method on zoom-in simulations of four massive (M200 ≥ 3 × 1014M⊙) galaxy clusters. We predict that during the early stages of assembly of the cluster at z ≳ 3, where the star formation activity is at its maximum in our simulations, the proto-cluster regions are rich in dusty gas. Compared to the case in which only dust production in stellar ejecta is active, if we include processes occurring in the cold ISM, the dust content is enhanced by a factor 2-3. However, the dust properties in this stage turn out to be significantly different from those observationally derived for the average Milky Way dust, and commonly adopted in calculations of dust reprocessing.We show that these differences may have a strong impact on the predicted spectral energy distributions. At low redshift in star-forming regions our model reproduces reasonably well the trend of dust abundances over metallicity as observed in local galaxies. However we underproduce by a factor of 2-3 the total dust content of clusters estimated observationally at low redshift, z ≲ 0.5 using IRAS, Planck, and Herschel satellites data. This discrepancy does not subsist by assuming a lower sputtering efficiency, which erodes dust grains in the hot intracluster medium.
publishDate 2018
dc.date.none.fl_str_mv 2018-09
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/11336/86948
Gjergo, Eda; Granato, Gian Luigi; Murante, Giuseppe; Ragone Figueroa, Cinthia Judith; Tornatore, Luca; et al.; Dust evolution in galaxy cluster simulations; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 479; 2; 9-2018; 2588-2606
0035-8711
1365-2966
CONICET Digital
CONICET
url http://hdl.handle.net/11336/86948
identifier_str_mv Gjergo, Eda; Granato, Gian Luigi; Murante, Giuseppe; Ragone Figueroa, Cinthia Judith; Tornatore, Luca; et al.; Dust evolution in galaxy cluster simulations; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 479; 2; 9-2018; 2588-2606
0035-8711
1365-2966
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/479/2/2588/5037930
info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/sty1564
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
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 13.070432

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