Thin disc, thick disc and halo in a simulated galaxy

This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©2012 RAS © 2012 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

Detalles Bibliográficos
Autores: Brook, C. B., Stinson, G. S., Gibson, B. K., Kawata, D., House, E. L., Miranda, M. S., Pilkington, K., Roškar, R., Wadsley, J., Quinn, T. R., Macciò, A. V.
Tipo de recurso: artículo
Fecha de publicación:2012
País:España
Institución:Universidad Autónoma de Madrid
Repositorio:Biblos-e Archivo. Repositorio Institucional de la UAM
Idioma:inglés
OAI Identifier:oai:repositorio.uam.es:10486/667209
Acceso en línea:http://hdl.handle.net/10486/667209
https://dx.doi.org/10.1111/j.1365-2966.2012.21738.x
Access Level:acceso abierto
Palabra clave:Galaxy:disc
Galaxy: evolution
Galaxy: formation
Galaxies: evolution
Galaxies: formation
Física
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repository_id_str
spelling Thin disc, thick disc and halo in a simulated galaxyBrook, C. B.Stinson, G. S.Gibson, B. K.Kawata, D.House, E. L.Miranda, M. S.Pilkington, K.Roškar, R.Wadsley, J.Quinn, T. R.Macciò, A. V.Galaxy:discGalaxy: evolutionGalaxy: formationGalaxies: evolutionGalaxies: formationFísicaThis article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©2012 RAS © 2012 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.Within a cosmological hydrodynamical simulation, we form a disc galaxy with sub-components which can be assigned to a thin stellar disc, thick disc and a low-mass stellar halo via a chemical decomposition. The thin- and thick-disc populations so selected are distinct in their ages, kinematics and metallicities. Thin-disc stars are young (<6.6 Gyr), possess low velocity dispersion (σ U, V, W = 41, 31, 25 kms -1), high [Fe/H] and low [O/Fe]. Conversely, the thick-disc stars are old (6.6 < age < 9.8Gyr), lag the thin disc by ∼21 kms -1, possess higher velocity dispersion (σ U, V, W = 49, 44, 35 kms -1) and have relatively low [Fe/H] and high [O/Fe]. The halo component comprises less than 4 per cent of stars in the 'solar annulus' of the simulation, has low metallicity, a velocity ellipsoid defined by σ U, V, W = 62, 46, 45 kms -1 and is formed primarily in situ during an early merger epoch. Gas-rich mergers during this epoch play a major role in fuelling the formation of the old-disc stars (the thick disc). We demonstrate that this is consistent with studies which show that cold accretion is the main source of a disc galaxy's baryons. Our simulation initially forms a relatively short (scalelength ∼1.7kpc at z = 1) and kinematically hot disc, primarily from gas accreted during the galaxy's merger epoch. Far from being a competing formation scenario, we show that migration is crucial for reconciling the short, hot, discs which form at high redshift in Λ cold dark matter, with the properties of the thick disc at z = 0. The thick disc, as defined by its abundances, maintains its relatively short scalelength at z = 0 (2.31kpc) compared with the total disc scalelength of 2.73kpc. The inside-out nature of disc growth is imprinted in the evolution of abundances such that the metal-poor α-young population has a larger scalelength (4.07kpc) than the more chemically evolved metal-rich α-young population (2.74kpc)BKG and CBB acknowledge the support of the UK’s Science & Technology Facilities Council (ST/F002432/1 & ST/H00260X/1). BKG and KP acknowledge the generous visitor support provided by Saint Mary’s University and Monash University. TRQ was supported by NSF Grant AST- 0908499. We thank the DEISA consortium, co-funded through EU FP6 project RI-031513 and the FP7 project RI-222919, for support within the DEISA Extreme Computing Initiative, the UK’s National Cosmology Supercomputer (COSMOS) and the University of Central Lancashire’s High Performance Computing Facility. CBB and AVM acknowledge funding by Sonderforschungsbereich SFB 881 ‘The Milky Way System’(sub-project A1) of the German Research Foundation (DFG)Oxford University PressRoyal Astronomical SocietyDepartamento de Física TeóricaFacultad de Ciencias20122012-10-11research articlehttp://purl.org/coar/resource_type/c_2df8fbb1VoRhttp://purl.org/coar/version/c_970fb48d4fbd8a85info:eu-repo/semantics/articleapplication/pdfhttp://hdl.handle.net/10486/667209https://dx.doi.org/10.1111/j.1365-2966.2012.21738.xreponame:Biblos-e Archivo. Repositorio Institucional de la UAMinstname:Universidad Autónoma de MadridInglésengopen accesshttp://purl.org/coar/access_right/c_abf2info:eu-repo/semantics/openAccessoai:repositorio.uam.es:10486/6672092026-06-23T12:46:27Z
dc.title.none.fl_str_mv Thin disc, thick disc and halo in a simulated galaxy
title Thin disc, thick disc and halo in a simulated galaxy
spellingShingle Thin disc, thick disc and halo in a simulated galaxy
Brook, C. B.
Galaxy:disc
Galaxy: evolution
Galaxy: formation
Galaxies: evolution
Galaxies: formation
Física
title_short Thin disc, thick disc and halo in a simulated galaxy
title_full Thin disc, thick disc and halo in a simulated galaxy
title_fullStr Thin disc, thick disc and halo in a simulated galaxy
title_full_unstemmed Thin disc, thick disc and halo in a simulated galaxy
title_sort Thin disc, thick disc and halo in a simulated galaxy
dc.creator.none.fl_str_mv Brook, C. B.
Stinson, G. S.
Gibson, B. K.
Kawata, D.
House, E. L.
Miranda, M. S.
Pilkington, K.
Roškar, R.
Wadsley, J.
Quinn, T. R.
Macciò, A. V.
author Brook, C. B.
author_facet Brook, C. B.
Stinson, G. S.
Gibson, B. K.
Kawata, D.
House, E. L.
Miranda, M. S.
Pilkington, K.
Roškar, R.
Wadsley, J.
Quinn, T. R.
Macciò, A. V.
author_role author
author2 Stinson, G. S.
Gibson, B. K.
Kawata, D.
House, E. L.
Miranda, M. S.
Pilkington, K.
Roškar, R.
Wadsley, J.
Quinn, T. R.
Macciò, A. V.
author2_role author
author
author
author
author
author
author
author
author
author
dc.contributor.none.fl_str_mv Departamento de Física Teórica
Facultad de Ciencias
dc.subject.none.fl_str_mv Galaxy:disc
Galaxy: evolution
Galaxy: formation
Galaxies: evolution
Galaxies: formation
Física
topic Galaxy:disc
Galaxy: evolution
Galaxy: formation
Galaxies: evolution
Galaxies: formation
Física
description This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©2012 RAS © 2012 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
publishDate 2012
dc.date.none.fl_str_mv 2012
2012-10-11
dc.type.none.fl_str_mv research article
http://purl.org/coar/resource_type/c_2df8fbb1
VoR
http://purl.org/coar/version/c_970fb48d4fbd8a85
dc.type.openaire.fl_str_mv info:eu-repo/semantics/article
format article
dc.identifier.none.fl_str_mv http://hdl.handle.net/10486/667209
https://dx.doi.org/10.1111/j.1365-2966.2012.21738.x
url http://hdl.handle.net/10486/667209
https://dx.doi.org/10.1111/j.1365-2966.2012.21738.x
dc.language.none.fl_str_mv Inglés
eng
language_invalid_str_mv Inglés
language eng
dc.rights.none.fl_str_mv open access
http://purl.org/coar/access_right/c_abf2
dc.rights.openaire.fl_str_mv info:eu-repo/semantics/openAccess
rights_invalid_str_mv open access
http://purl.org/coar/access_right/c_abf2
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv application/pdf
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:Biblos-e Archivo. Repositorio Institucional de la UAM
instname:Universidad Autónoma de Madrid
instname_str Universidad Autónoma de Madrid
reponame_str Biblos-e Archivo. Repositorio Institucional de la UAM
collection Biblos-e Archivo. Repositorio Institucional de la UAM
repository.name.fl_str_mv
repository.mail.fl_str_mv
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score 15,300724

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