A holistic review of a galactic interaction

Our situation as occupants of the Milky Way (MW) Galaxy, bombarded by the Sagittarius dwarf galaxy, provides an intimate view of physical processes that can lead to the dynamical heating of a galactic disc. While this evolution is instigated by Sagittarius, it is also driven by the intertwined influ...

Descripción completa

Detalles Bibliográficos
Autores: Grion Filho, Douglas, Johnston, Kathryn V., Poggio, Eloisa, Laporte, Chervin F. P., Drimmel, Ronald, D'Onghia, Elena
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2021
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/253860
Acceso en línea:http://hdl.handle.net/10261/253860
Access Level:acceso abierto
Palabra clave:Galaxy: disc
Galaxy: evolution
Galaxy: kinematics
Galaxy: structure
Local group
id ES_027afbe2bdf356ba44d08dbf2a37435f
oai_identifier_str oai:digital.csic.es:10261/253860
network_acronym_str ES
network_name_str España
repository_id_str
spelling A holistic review of a galactic interactionGrion Filho, DouglasJohnston, Kathryn V.Poggio, EloisaLaporte, Chervin F. P.Drimmel, RonaldD'Onghia, ElenaGalaxy: discGalaxy: evolutionGalaxy: kinematicsGalaxy: structureLocal groupOur situation as occupants of the Milky Way (MW) Galaxy, bombarded by the Sagittarius dwarf galaxy, provides an intimate view of physical processes that can lead to the dynamical heating of a galactic disc. While this evolution is instigated by Sagittarius, it is also driven by the intertwined influences of the dark matter halo and the disc itself. We analyse an N-body simulation following a Sagittarius-like galaxy interacting with a MW-like host to disentangle these different influences during the stages of a minor merger. The accelerations in the disc plane from each component are calculated for each snapshot in the simulation, and then decomposed into Fourier series on annuli. The analysis maps quantify and compare the scales of the individual contributions over space and through time: (i) accelerations due to the satellite are only important around disc passages; (ii) the influence around these passages is enhanced and extended by the distortion of the dark matter halo; (iii) the interaction drives disc asymmetries within and perpendicular to the plane and the self-gravity of these distortions increase in importance with time eventually leading to the formation of a bar. These results have interesting implications for identifying different influences within our own Galaxy. Currently, Sagittarius is close enough to a plane crossing to search for localized signatures of its effect at intermediate radii, the distortion of the MW's dark matter halo should leave its imprint in the outer disc and the disc's own self-consistent response is sculpting the intermediate and inner disc.KVJ and DGF were supported by NSF grant AST-1715582. CL acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement no. 852839). This work was supported in part by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan.Oxford University PressRoyal Astronomical SocietyEuropean CommissionMinistry of Education, Culture, Sports, Science and Technology (Japan)Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]2021202120212021info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_dcae04bcPublisher's versioninfo:eu-repo/semantics/publishedVersionhttp://hdl.handle.net/10261/253860reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/EC/H2020/852839http://doi.org/10.1093/mnras/stab2398Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/2538602026-05-22T06:33:51Z
dc.title.none.fl_str_mv A holistic review of a galactic interaction
title A holistic review of a galactic interaction
spellingShingle A holistic review of a galactic interaction
Grion Filho, Douglas
Galaxy: disc
Galaxy: evolution
Galaxy: kinematics
Galaxy: structure
Local group
title_short A holistic review of a galactic interaction
title_full A holistic review of a galactic interaction
title_fullStr A holistic review of a galactic interaction
title_full_unstemmed A holistic review of a galactic interaction
title_sort A holistic review of a galactic interaction
dc.creator.none.fl_str_mv Grion Filho, Douglas
Johnston, Kathryn V.
Poggio, Eloisa
Laporte, Chervin F. P.
Drimmel, Ronald
D'Onghia, Elena
author Grion Filho, Douglas
author_facet Grion Filho, Douglas
Johnston, Kathryn V.
Poggio, Eloisa
Laporte, Chervin F. P.
Drimmel, Ronald
D'Onghia, Elena
author_role author
author2 Johnston, Kathryn V.
Poggio, Eloisa
Laporte, Chervin F. P.
Drimmel, Ronald
D'Onghia, Elena
author2_role author
author
author
author
author
dc.contributor.none.fl_str_mv European Commission
Ministry of Education, Culture, Sports, Science and Technology (Japan)
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Galaxy: disc
Galaxy: evolution
Galaxy: kinematics
Galaxy: structure
Local group
topic Galaxy: disc
Galaxy: evolution
Galaxy: kinematics
Galaxy: structure
Local group
description Our situation as occupants of the Milky Way (MW) Galaxy, bombarded by the Sagittarius dwarf galaxy, provides an intimate view of physical processes that can lead to the dynamical heating of a galactic disc. While this evolution is instigated by Sagittarius, it is also driven by the intertwined influences of the dark matter halo and the disc itself. We analyse an N-body simulation following a Sagittarius-like galaxy interacting with a MW-like host to disentangle these different influences during the stages of a minor merger. The accelerations in the disc plane from each component are calculated for each snapshot in the simulation, and then decomposed into Fourier series on annuli. The analysis maps quantify and compare the scales of the individual contributions over space and through time: (i) accelerations due to the satellite are only important around disc passages; (ii) the influence around these passages is enhanced and extended by the distortion of the dark matter halo; (iii) the interaction drives disc asymmetries within and perpendicular to the plane and the self-gravity of these distortions increase in importance with time eventually leading to the formation of a bar. These results have interesting implications for identifying different influences within our own Galaxy. Currently, Sagittarius is close enough to a plane crossing to search for localized signatures of its effect at intermediate radii, the distortion of the MW's dark matter halo should leave its imprint in the outer disc and the disc's own self-consistent response is sculpting the intermediate and inner disc.
publishDate 2021
dc.date.none.fl_str_mv 2021
2021
2021
2021
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_dcae04bc
Publisher's version
info:eu-repo/semantics/publishedVersion
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/253860
url http://hdl.handle.net/10261/253860
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
http://doi.org/10.1093/mnras/stab2398
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.publisher.none.fl_str_mv Oxford University Press
Royal Astronomical Society
publisher.none.fl_str_mv Oxford University Press
Royal Astronomical Society
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
_version_ 1869402658145566720
score 15.811543

Similares en LA Referencia