Galaxy evolution in modified gravity simulations: using galaxy properties to constrain our gravitational model

Autores
Pallero, Diego; Gómez, Facundo A.; Padilla, Nelson David; Jaffé, Y. L.; Baugh, Carlton M.; Li, Baojiu; Hernández Aguayo, César; Arnold, Christian
Año de publicación
2024
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We present a quantitative analysis of the properties of galaxies and structures evolving in universes dominated by different modified gravitational models, including two variants of the f(R)-gravity (F) and two of the Dvali-Gabdadze-Poratti (N) braneworld model, which respectively feature the chameleon and Vainshtein screening mechanisms. Using the Simulation HYdrodynamics BeyONd Einstein (SHYBONE) cosmological hydrodynamical full-physics simulations suite, we study the departures in the properties of galaxies residing in different environments with respect to the standard model (GR). Using two different criteria to compare, we find that structures formed within modified gravity tend to show a denser gas density profile than their GR counterparts. Within the different modified gravity models, N1 and F5 gravity models show greater departures from the standard model, with gas density profiles ρIGM≥30 per cent denser in the outskirts for the N1 model, and in the inner parts for the F5 model. Additionally, we find that haloes evolving in MG universes show, in general, larger quenched fractions than GR, reaching up to 20 per cent larger quenching fractions in F5 regardless of the stellar mass of the galaxy. Concerning the other models, F6, N1, and N5 show slightly larger quenched fractions, but no strong differences can be found. These results directly impact the colour distribution of galaxies, making them in MG models redder and older than their GR counterparts. Like GR, once the environment starts to play a role, galaxies rapidly get quenched, and the differences between models vanish.
Fil: Pallero, Diego. Universidad Técnica Federico Santa María; Chile
Fil: Gómez, Facundo A.. Universidad de La Serena; Chile
Fil: Padilla, Nelson David. 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: Jaffé, Y. L.. Universidad Técnica Federico Santa María; Chile. Universidad de Valparaíso; Chile
Fil: Baugh, Carlton M.. University of Durham; Reino Unido
Fil: Li, Baojiu. University of Durham; Reino Unido
Fil: Hernández Aguayo, César. Max-Planck-Institut für Astrophysik ; Alemania
Fil: Arnold, Christian. University of Durham; Reino Unido
Materia
Astrophysics
Galaxies
Cosmology
Modified gravity
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/282057
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/282057
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Galaxy evolution in modified gravity simulations: using galaxy properties to constrain our gravitational modelPallero, DiegoGómez, Facundo A.Padilla, Nelson DavidJaffé, Y. L.Baugh, Carlton M.Li, BaojiuHernández Aguayo, CésarArnold, ChristianAstrophysicsGalaxiesCosmologyModified gravityhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We present a quantitative analysis of the properties of galaxies and structures evolving in universes dominated by different modified gravitational models, including two variants of the f(R)-gravity (F) and two of the Dvali-Gabdadze-Poratti (N) braneworld model, which respectively feature the chameleon and Vainshtein screening mechanisms. Using the Simulation HYdrodynamics BeyONd Einstein (SHYBONE) cosmological hydrodynamical full-physics simulations suite, we study the departures in the properties of galaxies residing in different environments with respect to the standard model (GR). Using two different criteria to compare, we find that structures formed within modified gravity tend to show a denser gas density profile than their GR counterparts. Within the different modified gravity models, N1 and F5 gravity models show greater departures from the standard model, with gas density profiles ρIGM≥30 per cent denser in the outskirts for the N1 model, and in the inner parts for the F5 model. Additionally, we find that haloes evolving in MG universes show, in general, larger quenched fractions than GR, reaching up to 20 per cent larger quenching fractions in F5 regardless of the stellar mass of the galaxy. Concerning the other models, F6, N1, and N5 show slightly larger quenched fractions, but no strong differences can be found. These results directly impact the colour distribution of galaxies, making them in MG models redder and older than their GR counterparts. Like GR, once the environment starts to play a role, galaxies rapidly get quenched, and the differences between models vanish.Fil: Pallero, Diego. Universidad Técnica Federico Santa María; ChileFil: Gómez, Facundo A.. Universidad de La Serena; ChileFil: Padilla, Nelson David. 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: Jaffé, Y. L.. Universidad Técnica Federico Santa María; Chile. Universidad de Valparaíso; ChileFil: Baugh, Carlton M.. University of Durham; Reino UnidoFil: Li, Baojiu. University of Durham; Reino UnidoFil: Hernández Aguayo, César. Max-Planck-Institut für Astrophysik ; AlemaniaFil: Arnold, Christian. University of Durham; Reino UnidoWiley Blackwell Publishing, Inc2024-09info: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/11336/282057Pallero, Diego; Gómez, Facundo A.; Padilla, Nelson David; Jaffé, Y. L.; Baugh, Carlton M.; et al.; Galaxy evolution in modified gravity simulations: using galaxy properties to constrain our gravitational model; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 533; 3; 9-2024; 3344-33640035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/533/3/3344/7742177info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stae2002info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2026-03-11T11:37:57Zoai:ri.conicet.gov.ar:11336/282057instacron: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:34982026-03-11 11:37:58.171CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Galaxy evolution in modified gravity simulations: using galaxy properties to constrain our gravitational model
title Galaxy evolution in modified gravity simulations: using galaxy properties to constrain our gravitational model
spellingShingle Galaxy evolution in modified gravity simulations: using galaxy properties to constrain our gravitational model
Pallero, Diego
Astrophysics
Galaxies
Cosmology
Modified gravity
title_short Galaxy evolution in modified gravity simulations: using galaxy properties to constrain our gravitational model
title_full Galaxy evolution in modified gravity simulations: using galaxy properties to constrain our gravitational model
title_fullStr Galaxy evolution in modified gravity simulations: using galaxy properties to constrain our gravitational model
title_full_unstemmed Galaxy evolution in modified gravity simulations: using galaxy properties to constrain our gravitational model
title_sort Galaxy evolution in modified gravity simulations: using galaxy properties to constrain our gravitational model
dc.creator.none.fl_str_mv Pallero, Diego
Gómez, Facundo A.
Padilla, Nelson David
Jaffé, Y. L.
Baugh, Carlton M.
Li, Baojiu
Hernández Aguayo, César
Arnold, Christian
author Pallero, Diego
author_facet Pallero, Diego
Gómez, Facundo A.
Padilla, Nelson David
Jaffé, Y. L.
Baugh, Carlton M.
Li, Baojiu
Hernández Aguayo, César
Arnold, Christian
author_role author
author2 Gómez, Facundo A.
Padilla, Nelson David
Jaffé, Y. L.
Baugh, Carlton M.
Li, Baojiu
Hernández Aguayo, César
Arnold, Christian
author2_role author
author
author
author
author
author
author
dc.subject.none.fl_str_mv Astrophysics
Galaxies
Cosmology
Modified gravity
topic Astrophysics
Galaxies
Cosmology
Modified gravity
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 quantitative analysis of the properties of galaxies and structures evolving in universes dominated by different modified gravitational models, including two variants of the f(R)-gravity (F) and two of the Dvali-Gabdadze-Poratti (N) braneworld model, which respectively feature the chameleon and Vainshtein screening mechanisms. Using the Simulation HYdrodynamics BeyONd Einstein (SHYBONE) cosmological hydrodynamical full-physics simulations suite, we study the departures in the properties of galaxies residing in different environments with respect to the standard model (GR). Using two different criteria to compare, we find that structures formed within modified gravity tend to show a denser gas density profile than their GR counterparts. Within the different modified gravity models, N1 and F5 gravity models show greater departures from the standard model, with gas density profiles ρIGM≥30 per cent denser in the outskirts for the N1 model, and in the inner parts for the F5 model. Additionally, we find that haloes evolving in MG universes show, in general, larger quenched fractions than GR, reaching up to 20 per cent larger quenching fractions in F5 regardless of the stellar mass of the galaxy. Concerning the other models, F6, N1, and N5 show slightly larger quenched fractions, but no strong differences can be found. These results directly impact the colour distribution of galaxies, making them in MG models redder and older than their GR counterparts. Like GR, once the environment starts to play a role, galaxies rapidly get quenched, and the differences between models vanish.
Fil: Pallero, Diego. Universidad Técnica Federico Santa María; Chile
Fil: Gómez, Facundo A.. Universidad de La Serena; Chile
Fil: Padilla, Nelson David. 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: Jaffé, Y. L.. Universidad Técnica Federico Santa María; Chile. Universidad de Valparaíso; Chile
Fil: Baugh, Carlton M.. University of Durham; Reino Unido
Fil: Li, Baojiu. University of Durham; Reino Unido
Fil: Hernández Aguayo, César. Max-Planck-Institut für Astrophysik ; Alemania
Fil: Arnold, Christian. University of Durham; Reino Unido
description We present a quantitative analysis of the properties of galaxies and structures evolving in universes dominated by different modified gravitational models, including two variants of the f(R)-gravity (F) and two of the Dvali-Gabdadze-Poratti (N) braneworld model, which respectively feature the chameleon and Vainshtein screening mechanisms. Using the Simulation HYdrodynamics BeyONd Einstein (SHYBONE) cosmological hydrodynamical full-physics simulations suite, we study the departures in the properties of galaxies residing in different environments with respect to the standard model (GR). Using two different criteria to compare, we find that structures formed within modified gravity tend to show a denser gas density profile than their GR counterparts. Within the different modified gravity models, N1 and F5 gravity models show greater departures from the standard model, with gas density profiles ρIGM≥30 per cent denser in the outskirts for the N1 model, and in the inner parts for the F5 model. Additionally, we find that haloes evolving in MG universes show, in general, larger quenched fractions than GR, reaching up to 20 per cent larger quenching fractions in F5 regardless of the stellar mass of the galaxy. Concerning the other models, F6, N1, and N5 show slightly larger quenched fractions, but no strong differences can be found. These results directly impact the colour distribution of galaxies, making them in MG models redder and older than their GR counterparts. Like GR, once the environment starts to play a role, galaxies rapidly get quenched, and the differences between models vanish.
publishDate 2024
dc.date.none.fl_str_mv 2024-09
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/11336/282057
Pallero, Diego; Gómez, Facundo A.; Padilla, Nelson David; Jaffé, Y. L.; Baugh, Carlton M.; et al.; Galaxy evolution in modified gravity simulations: using galaxy properties to constrain our gravitational model; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 533; 3; 9-2024; 3344-3364
0035-8711
CONICET Digital
CONICET
url http://hdl.handle.net/11336/282057
identifier_str_mv Pallero, Diego; Gómez, Facundo A.; Padilla, Nelson David; Jaffé, Y. L.; Baugh, Carlton M.; et al.; Galaxy evolution in modified gravity simulations: using galaxy properties to constrain our gravitational model; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 533; 3; 9-2024; 3344-3364
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/533/3/3344/7742177
info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stae2002
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by/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 12.977003

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