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
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/202960
Ver los metadatos del registro completo
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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 Técnicas2025-09-29T10:11:47Zoai: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:34982025-09-29 10:11:47.846CONICET 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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1844614020200398848 |
score |
13.070432 |