Revealing the properties of void galaxies and their assembly using the eagle simulation

Autores
Rosas Guevara, Yetli; Tissera, Patricia Beatriz; Lagos, Claudia del P; Paillas, Enrique; Padilla, Nelson David
Año de publicación
2022
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We explore the properties of central galaxies living in voids using the EAGLE cosmological hydrodynamic simulations. Based on the minimum void-centric distance, we define four galaxy samples: inner void, outer void, wall, and skeleton. We find that inner void galaxies with host halo masses <1012M⊙<1012M⊙ have lower stellar mass and stellar mass fractions than those in denser environments, and the fraction of galaxies with star formation (SF) activity and atomic hydrogen (H I) gas decreases with increasing void-centric distance, in agreement with observations. To mitigate the influence of stellar (halo) mass, we compare inner void galaxies to subsamples of fixed stellar (halo) mass. Compared to denser environments, inner void galaxies with M∗=10[9.0−9.5]M⊙M∗=10[9.0−9.5]M⊙ have comparable SF activity and H I gas fractions, but the lowest quenched galaxy fraction. Inner void galaxies with M∗=10[9.5−10.5]M⊙M∗=10[9.5−10.5]M⊙ have the lowest H I gas fraction, the highest quenched fraction and the lowest gas metallicities. On the other hand, inner void galaxies with M∗>1010.5M⊙M∗>1010.5M⊙ have comparable SF activity and H I gas fractions to their analogues in denser environments. They retain the highest metallicity gas that might be linked to physical processes that act with lower efficiency in underdense regions such as AGN (active galaxy nucleus) feedback. Furthermore, inner void galaxies have the lowest fraction of positive gas-phase metallicity gradients, which are typically associated with external processes or feedback events, suggesting they have more quiet merger histories than galaxies in denser environments. Our findings shed light on how galaxies are influenced by their large-scale environment.
Fil: Rosas Guevara, Yetli. Pontificia Universidad Católica de Chile; Chile
Fil: Tissera, Patricia Beatriz. 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. Pontificia Universidad Católica de Chile; Chile
Fil: Lagos, Claudia del P. Pontificia Universidad Católica de Chile; Chile
Fil: Paillas, Enrique. Pontificia Universidad Católica de Chile; 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
Materia
Galaxies
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:11336/202960
Acceder
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network_name_str CONICET Digital (CONICET)
spelling Revealing the properties of void galaxies and their assembly using the eagle simulationRosas Guevara, YetliTissera, Patricia BeatrizLagos, Claudia del PPaillas, EnriquePadilla, Nelson DavidGalaxiesSimulationshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We explore the properties of central galaxies living in voids using the EAGLE cosmological hydrodynamic simulations. Based on the minimum void-centric distance, we define four galaxy samples: inner void, outer void, wall, and skeleton. We find that inner void galaxies with host halo masses <1012M⊙<1012M⊙ have lower stellar mass and stellar mass fractions than those in denser environments, and the fraction of galaxies with star formation (SF) activity and atomic hydrogen (H I) gas decreases with increasing void-centric distance, in agreement with observations. To mitigate the influence of stellar (halo) mass, we compare inner void galaxies to subsamples of fixed stellar (halo) mass. Compared to denser environments, inner void galaxies with M∗=10[9.0−9.5]M⊙M∗=10[9.0−9.5]M⊙ have comparable SF activity and H I gas fractions, but the lowest quenched galaxy fraction. Inner void galaxies with M∗=10[9.5−10.5]M⊙M∗=10[9.5−10.5]M⊙ have the lowest H I gas fraction, the highest quenched fraction and the lowest gas metallicities. On the other hand, inner void galaxies with M∗>1010.5M⊙M∗>1010.5M⊙ have comparable SF activity and H I gas fractions to their analogues in denser environments. They retain the highest metallicity gas that might be linked to physical processes that act with lower efficiency in underdense regions such as AGN (active galaxy nucleus) feedback. Furthermore, inner void galaxies have the lowest fraction of positive gas-phase metallicity gradients, which are typically associated with external processes or feedback events, suggesting they have more quiet merger histories than galaxies in denser environments. Our findings shed light on how galaxies are influenced by their large-scale environment.Fil: Rosas Guevara, Yetli. Pontificia Universidad Católica de Chile; ChileFil: Tissera, Patricia Beatriz. 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. Pontificia Universidad Católica de Chile; ChileFil: Lagos, Claudia del P. Pontificia Universidad Católica de Chile; ChileFil: Paillas, Enrique. Pontificia Universidad Católica de Chile; 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; ArgentinaOxford University Press2022-11info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/202960Rosas Guevara, Yetli; Tissera, Patricia Beatriz; Lagos, Claudia del P; Paillas, Enrique; Padilla, Nelson David; Revealing the properties of void galaxies and their assembly using the eagle simulation; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 517; 1; 11-2022; 712-7310035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/517/1/712/6696385info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stac2583info:eu-repo/semantics/altIdentifier/arxiv/https://arxiv.org/abs/2204.04565info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-15T15:08:54Zoai:ri.conicet.gov.ar:11336/202960instacron: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:34982025-10-15 15:08:55.053CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Revealing the properties of void galaxies and their assembly using the eagle simulation
title Revealing the properties of void galaxies and their assembly using the eagle simulation
spellingShingle Revealing the properties of void galaxies and their assembly using the eagle simulation
Rosas Guevara, Yetli
Galaxies
Simulations
title_short Revealing the properties of void galaxies and their assembly using the eagle simulation
title_full Revealing the properties of void galaxies and their assembly using the eagle simulation
title_fullStr Revealing the properties of void galaxies and their assembly using the eagle simulation
title_full_unstemmed Revealing the properties of void galaxies and their assembly using the eagle simulation
title_sort Revealing the properties of void galaxies and their assembly using the eagle simulation
dc.creator.none.fl_str_mv Rosas Guevara, Yetli
Tissera, Patricia Beatriz
Lagos, Claudia del P
Paillas, Enrique
Padilla, Nelson David
author Rosas Guevara, Yetli
author_facet Rosas Guevara, Yetli
Tissera, Patricia Beatriz
Lagos, Claudia del P
Paillas, Enrique
Padilla, Nelson David
author_role author
author2 Tissera, Patricia Beatriz
Lagos, Claudia del P
Paillas, Enrique
Padilla, Nelson David
author2_role author
author
author
author
dc.subject.none.fl_str_mv Galaxies
Simulations
topic Galaxies
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 explore the properties of central galaxies living in voids using the EAGLE cosmological hydrodynamic simulations. Based on the minimum void-centric distance, we define four galaxy samples: inner void, outer void, wall, and skeleton. We find that inner void galaxies with host halo masses <1012M⊙<1012M⊙ have lower stellar mass and stellar mass fractions than those in denser environments, and the fraction of galaxies with star formation (SF) activity and atomic hydrogen (H I) gas decreases with increasing void-centric distance, in agreement with observations. To mitigate the influence of stellar (halo) mass, we compare inner void galaxies to subsamples of fixed stellar (halo) mass. Compared to denser environments, inner void galaxies with M∗=10[9.0−9.5]M⊙M∗=10[9.0−9.5]M⊙ have comparable SF activity and H I gas fractions, but the lowest quenched galaxy fraction. Inner void galaxies with M∗=10[9.5−10.5]M⊙M∗=10[9.5−10.5]M⊙ have the lowest H I gas fraction, the highest quenched fraction and the lowest gas metallicities. On the other hand, inner void galaxies with M∗>1010.5M⊙M∗>1010.5M⊙ have comparable SF activity and H I gas fractions to their analogues in denser environments. They retain the highest metallicity gas that might be linked to physical processes that act with lower efficiency in underdense regions such as AGN (active galaxy nucleus) feedback. Furthermore, inner void galaxies have the lowest fraction of positive gas-phase metallicity gradients, which are typically associated with external processes or feedback events, suggesting they have more quiet merger histories than galaxies in denser environments. Our findings shed light on how galaxies are influenced by their large-scale environment.
Fil: Rosas Guevara, Yetli. Pontificia Universidad Católica de Chile; Chile
Fil: Tissera, Patricia Beatriz. 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. Pontificia Universidad Católica de Chile; Chile
Fil: Lagos, Claudia del P. Pontificia Universidad Católica de Chile; Chile
Fil: Paillas, Enrique. Pontificia Universidad Católica de Chile; 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
description We explore the properties of central galaxies living in voids using the EAGLE cosmological hydrodynamic simulations. Based on the minimum void-centric distance, we define four galaxy samples: inner void, outer void, wall, and skeleton. We find that inner void galaxies with host halo masses <1012M⊙<1012M⊙ have lower stellar mass and stellar mass fractions than those in denser environments, and the fraction of galaxies with star formation (SF) activity and atomic hydrogen (H I) gas decreases with increasing void-centric distance, in agreement with observations. To mitigate the influence of stellar (halo) mass, we compare inner void galaxies to subsamples of fixed stellar (halo) mass. Compared to denser environments, inner void galaxies with M∗=10[9.0−9.5]M⊙M∗=10[9.0−9.5]M⊙ have comparable SF activity and H I gas fractions, but the lowest quenched galaxy fraction. Inner void galaxies with M∗=10[9.5−10.5]M⊙M∗=10[9.5−10.5]M⊙ have the lowest H I gas fraction, the highest quenched fraction and the lowest gas metallicities. On the other hand, inner void galaxies with M∗>1010.5M⊙M∗>1010.5M⊙ have comparable SF activity and H I gas fractions to their analogues in denser environments. They retain the highest metallicity gas that might be linked to physical processes that act with lower efficiency in underdense regions such as AGN (active galaxy nucleus) feedback. Furthermore, inner void galaxies have the lowest fraction of positive gas-phase metallicity gradients, which are typically associated with external processes or feedback events, suggesting they have more quiet merger histories than galaxies in denser environments. Our findings shed light on how galaxies are influenced by their large-scale environment.
publishDate 2022
dc.date.none.fl_str_mv 2022-11
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/11336/202960
Rosas Guevara, Yetli; Tissera, Patricia Beatriz; Lagos, Claudia del P; Paillas, Enrique; Padilla, Nelson David; Revealing the properties of void galaxies and their assembly using the eagle simulation; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 517; 1; 11-2022; 712-731
0035-8711
CONICET Digital
CONICET
url http://hdl.handle.net/11336/202960
identifier_str_mv Rosas Guevara, Yetli; Tissera, Patricia Beatriz; Lagos, Claudia del P; Paillas, Enrique; Padilla, Nelson David; Revealing the properties of void galaxies and their assembly using the eagle simulation; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 517; 1; 11-2022; 712-731
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/517/1/712/6696385
info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stac2583
info:eu-repo/semantics/altIdentifier/arxiv/https://arxiv.org/abs/2204.04565
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
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
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 13.22299

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