Lopsided galaxies in a cosmological context: a new galaxy-halo connection

Disc galaxies commonly show asymmetric features in their morphology, such as warps and lopsidedness. These features can provide key information regarding the recent evolution of a given disc galaxy. In the nearby Universe, up to ∼30 per cent of late-type galaxies display a global non-axisymmetric lo...

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Autores: Varela-Lavin, Silvio, Gómez, Facundo A., Tissera, Patricia, Besla, Gurtina, Garavito Camargo, Nicolás, Marinacci, Federico, Laporte, Chervin F. P.
Tipo de documento: artigo
Estado:Versão publicada
Data de publicação:2023
País:España
Recursos:Consejo Superior de Investigaciones Científicas (CSIC)
Repositório:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/337632
Acesso em linha:http://hdl.handle.net/10261/337632
Access Level:Acceso aberto
Palavra-chave:Galaxies: evolution
Galaxies: formation
Galaxies: haloes
Galaxies: interactions
Galaxies: spiral
Galaxies: structure
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spelling Lopsided galaxies in a cosmological context: a new galaxy-halo connectionVarela-Lavin, SilvioGómez, Facundo A.Tissera, PatriciaBesla, GurtinaGaravito Camargo, NicolásMarinacci, FedericoLaporte, Chervin F. P.Galaxies: evolutionGalaxies: formationGalaxies: haloesGalaxies: interactionsGalaxies: spiralGalaxies: structureDisc galaxies commonly show asymmetric features in their morphology, such as warps and lopsidedness. These features can provide key information regarding the recent evolution of a given disc galaxy. In the nearby Universe, up to ∼30 per cent of late-type galaxies display a global non-axisymmetric lopsided mass distribution. However, the origin of this perturbation is not well understood. In this work, we study the origin of lopsided perturbations in simulated disc galaxies extracted from the TNG50 simulation of the IllustrisTNG project. We statistically explore different excitation mechanisms for this perturbation, such as direct satellite tidal interactions and distortions of the underlying dark matter distributions. We also characterize the main physical conditions that lead to lopsided perturbations. 50 per cent of our sample galaxy have lopsided modes m = 1 greater than ∼0.12. We find a strong correlation between internal galaxy properties, such as central stellar surface density and disc radial extension with the strength of lopsided modes. The majority of lopsided galaxies have lower central surface densities and more extended discs than symmetric galaxies. As a result, such lopsided galaxies are less self-gravitationally cohesive, and their outer disc region is more susceptible to different types of external perturbations. However, we do not find strong evidence that tidal interactions with satellite galaxies are the main driving agent of lopsided modes. Lopsided galaxies tend to live in asymmetric dark matter haloes with high spin, indicating strong galaxy–halo connections in late-type lopsided galaxies.SV-L acknowledges financial support from Agencia Nacional de Investigacion y Desarrollo (ANID)/‘Beca de Doctorado Nacional’/21221776. FAG and SV-L acknowledge financial support from CONICYT through the project FONDECYT Regular No. 1211370. FAG and SV-L acknowledge funding from the Max Planck Society through a Partner Group grant. PBT acknowledges partial support from Fondecyt 1200703/2020 (ANID), Nucleus Millennium ERIS ANID NCN2021-017. FAG, PBT, and SV-L acknowledge support from ANID BASAL project FB210003. CFPL acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement no. 852839).Peer reviewedOxford University PressAgencia Nacional de Investigación y Desarrollo (Chile)Fondo Nacional de Desarrollo Científico y Tecnológico (Chile)Comisión Nacional de Investigación Científica y Tecnológica (Chile)Max Planck SocietyEuropean CommissionEuropean Research Council202320232023info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionapplication/pdfhttp://hdl.handle.net/10261/337632reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/EC/H2020/852839The data used in this work are accessible via the IllustrisTNG public data base: https://www.tng-project.org/data/https://doi.org/10.1093/mnras/stad1724Noinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/3376322026-05-22T06:33:51Z
dc.title.none.fl_str_mv Lopsided galaxies in a cosmological context: a new galaxy-halo connection
title Lopsided galaxies in a cosmological context: a new galaxy-halo connection
spellingShingle Lopsided galaxies in a cosmological context: a new galaxy-halo connection
Varela-Lavin, Silvio
Galaxies: evolution
Galaxies: formation
Galaxies: haloes
Galaxies: interactions
Galaxies: spiral
Galaxies: structure
title_short Lopsided galaxies in a cosmological context: a new galaxy-halo connection
title_full Lopsided galaxies in a cosmological context: a new galaxy-halo connection
title_fullStr Lopsided galaxies in a cosmological context: a new galaxy-halo connection
title_full_unstemmed Lopsided galaxies in a cosmological context: a new galaxy-halo connection
title_sort Lopsided galaxies in a cosmological context: a new galaxy-halo connection
dc.creator.none.fl_str_mv Varela-Lavin, Silvio
Gómez, Facundo A.
Tissera, Patricia
Besla, Gurtina
Garavito Camargo, Nicolás
Marinacci, Federico
Laporte, Chervin F. P.
author Varela-Lavin, Silvio
author_facet Varela-Lavin, Silvio
Gómez, Facundo A.
Tissera, Patricia
Besla, Gurtina
Garavito Camargo, Nicolás
Marinacci, Federico
Laporte, Chervin F. P.
author_role author
author2 Gómez, Facundo A.
Tissera, Patricia
Besla, Gurtina
Garavito Camargo, Nicolás
Marinacci, Federico
Laporte, Chervin F. P.
author2_role author
author
author
author
author
author
dc.contributor.none.fl_str_mv Agencia Nacional de Investigación y Desarrollo (Chile)
Fondo Nacional de Desarrollo Científico y Tecnológico (Chile)
Comisión Nacional de Investigación Científica y Tecnológica (Chile)
Max Planck Society
European Commission
European Research Council
dc.subject.none.fl_str_mv Galaxies: evolution
Galaxies: formation
Galaxies: haloes
Galaxies: interactions
Galaxies: spiral
Galaxies: structure
topic Galaxies: evolution
Galaxies: formation
Galaxies: haloes
Galaxies: interactions
Galaxies: spiral
Galaxies: structure
description Disc galaxies commonly show asymmetric features in their morphology, such as warps and lopsidedness. These features can provide key information regarding the recent evolution of a given disc galaxy. In the nearby Universe, up to ∼30 per cent of late-type galaxies display a global non-axisymmetric lopsided mass distribution. However, the origin of this perturbation is not well understood. In this work, we study the origin of lopsided perturbations in simulated disc galaxies extracted from the TNG50 simulation of the IllustrisTNG project. We statistically explore different excitation mechanisms for this perturbation, such as direct satellite tidal interactions and distortions of the underlying dark matter distributions. We also characterize the main physical conditions that lead to lopsided perturbations. 50 per cent of our sample galaxy have lopsided modes m = 1 greater than ∼0.12. We find a strong correlation between internal galaxy properties, such as central stellar surface density and disc radial extension with the strength of lopsided modes. The majority of lopsided galaxies have lower central surface densities and more extended discs than symmetric galaxies. As a result, such lopsided galaxies are less self-gravitationally cohesive, and their outer disc region is more susceptible to different types of external perturbations. However, we do not find strong evidence that tidal interactions with satellite galaxies are the main driving agent of lopsided modes. Lopsided galaxies tend to live in asymmetric dark matter haloes with high spin, indicating strong galaxy–halo connections in late-type lopsided galaxies.
publishDate 2023
dc.date.none.fl_str_mv 2023
2023
2023
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
Publisher's version
info:eu-repo/semantics/publishedVersion
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/337632
url http://hdl.handle.net/10261/337632
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv #PLACEHOLDER_PARENT_METADATA_VALUE#
info:eu-repo/grantAgreement/EC/H2020/852839
The data used in this work are accessible via the IllustrisTNG public data base: https://www.tng-project.org/data/
https://doi.org/10.1093/mnras/stad1724
No
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv 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:DIGITAL.CSIC. Repositorio Institucional del CSIC
instname:Consejo Superior de Investigaciones Científicas (CSIC)
instname_str Consejo Superior de Investigaciones Científicas (CSIC)
reponame_str DIGITAL.CSIC. Repositorio Institucional del CSIC
collection DIGITAL.CSIC. Repositorio Institucional del CSIC
repository.name.fl_str_mv
repository.mail.fl_str_mv
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