Elliptical galaxies from mergers of discs

[EN]We analyse N-body galaxy merger experiments involving disc galaxies. Mergers of disc–bulge–halo models are compared to those of bulgeless, disc–halo models to quantify the effects of the central bulge on merger dynamics and the structure of the remnant. Our models explore galaxy mass ratios 1:1...

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Detalhes bibliográficos
Autores: González-García, A. César, Balcells, Marc
Formato: artículo
Fecha de publicación:2005
País:España
Recursos:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/75051
Acesso em linha:http://hdl.handle.net/10261/75051
Access Level:acceso abierto
Palavra-chave:Galaxies: elliptical and lenticular, cD
Galaxies: interactions
Galaxies: kinematics and dynamics
Galaxies: structure
Incipit
Institute of Heritage Sciences
Instituto de Ciencias del Patrimonio
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repository_id_str
spelling Elliptical galaxies from mergers of discsGonzález-García, A. CésarBalcells, MarcGalaxies: elliptical and lenticular, cDGalaxies: interactionsGalaxies: kinematics and dynamicsGalaxies: structureIncipitInstitute of Heritage SciencesInstituto de Ciencias del Patrimonio[EN]We analyse N-body galaxy merger experiments involving disc galaxies. Mergers of disc–bulge–halo models are compared to those of bulgeless, disc–halo models to quantify the effects of the central bulge on merger dynamics and the structure of the remnant. Our models explore galaxy mass ratios 1:1 through 3:1, and use higher bulge mass fractions than previous studies. A full comparison of the structural and dynamical properties with our observations is carried out. The presence of central bulges results in longer tidal tails, oblate final intrinsic shapes, surface brightness profiles with a higher Sérsic index, steeper rotation curves and oblate-rotator internal dynamics. Mergers of bulgeless galaxies do not generate long-lasting tidal tails, and their strong triaxiality seems inconsistent with observations; these remnants show shells, which we do not find in models including central bulges. Giant ellipticals with boxy isophotes and anisotropic dynamics cannot be produced by the mergers modelled here; they could be the result of mergers between lower luminosity ellipticals, themselves plausibly formed in disc-disc mergers.Peer reviewedRoyal Astronomical Society201320132005info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501http://hdl.handle.net/10261/75051reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglésinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/750512026-05-22T06:33:51Z
dc.title.none.fl_str_mv Elliptical galaxies from mergers of discs
title Elliptical galaxies from mergers of discs
spellingShingle Elliptical galaxies from mergers of discs
González-García, A. César
Galaxies: elliptical and lenticular, cD
Galaxies: interactions
Galaxies: kinematics and dynamics
Galaxies: structure
Incipit
Institute of Heritage Sciences
Instituto de Ciencias del Patrimonio
title_short Elliptical galaxies from mergers of discs
title_full Elliptical galaxies from mergers of discs
title_fullStr Elliptical galaxies from mergers of discs
title_full_unstemmed Elliptical galaxies from mergers of discs
title_sort Elliptical galaxies from mergers of discs
dc.creator.none.fl_str_mv González-García, A. César
Balcells, Marc
author González-García, A. César
author_facet González-García, A. César
Balcells, Marc
author_role author
author2 Balcells, Marc
author2_role author
dc.subject.none.fl_str_mv Galaxies: elliptical and lenticular, cD
Galaxies: interactions
Galaxies: kinematics and dynamics
Galaxies: structure
Incipit
Institute of Heritage Sciences
Instituto de Ciencias del Patrimonio
topic Galaxies: elliptical and lenticular, cD
Galaxies: interactions
Galaxies: kinematics and dynamics
Galaxies: structure
Incipit
Institute of Heritage Sciences
Instituto de Ciencias del Patrimonio
description [EN]We analyse N-body galaxy merger experiments involving disc galaxies. Mergers of disc–bulge–halo models are compared to those of bulgeless, disc–halo models to quantify the effects of the central bulge on merger dynamics and the structure of the remnant. Our models explore galaxy mass ratios 1:1 through 3:1, and use higher bulge mass fractions than previous studies. A full comparison of the structural and dynamical properties with our observations is carried out. The presence of central bulges results in longer tidal tails, oblate final intrinsic shapes, surface brightness profiles with a higher Sérsic index, steeper rotation curves and oblate-rotator internal dynamics. Mergers of bulgeless galaxies do not generate long-lasting tidal tails, and their strong triaxiality seems inconsistent with observations; these remnants show shells, which we do not find in models including central bulges. Giant ellipticals with boxy isophotes and anisotropic dynamics cannot be produced by the mergers modelled here; they could be the result of mergers between lower luminosity ellipticals, themselves plausibly formed in disc-disc mergers.
publishDate 2005
dc.date.none.fl_str_mv 2005
2013
2013
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
format article
dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/75051
url http://hdl.handle.net/10261/75051
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.publisher.none.fl_str_mv Royal Astronomical Society
publisher.none.fl_str_mv 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_ 1869415757390020608
score 15,812429

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