Disc heating: Comparing the Milky Way with cosmological simulations

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dc.contributor.author House, E. L.
dc.contributor.author Brook, C. B.
dc.contributor.author Gibson, B. K.
dc.contributor.author Sánchez-Blázquez, Patricia
dc.contributor.author Courty, S.
dc.contributor.author Few, C. G.
dc.contributor.author Governato, F.
dc.contributor.author Kawata, D.
dc.contributor.author Roškar, R.
dc.contributor.author Steinmetz, M.
dc.contributor.author Stinson, G. S.
dc.contributor.author Teyssier, R.
dc.contributor.other UAM. Departamento de Física Teórica es_ES
dc.date.accessioned 2015-07-23T08:59:50Z
dc.date.available 2015-07-23T08:59:50Z
dc.date.issued 2011-08-01
dc.identifier.citation Monthly Notices of the Royal Astronomical Society 415.3(2011): 2652-2664 en_US
dc.identifier.issn 0035-8711 (print) es_ES
dc.identifier.issn 1365-2966 (online) es_ES
dc.identifier.uri http://hdl.handle.net/10486/667531
dc.description This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2011 RAS © The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. en_US
dc.description.abstract We present an analysis of a suite of simulations run with different particle- and grid-based cosmological hydrodynamical codes and compare them with observational data of the Milky Way. This is the first study to make comparisons of properties of galaxies simulated with particle- and grid-based codes. Our analysis indicates that there is broad agreement between these different modelling techniques. We study the velocity dispersion-age relation for disc stars at z= 0 and find that four of the simulations are more consistent with observations by Holmberg, Nordstroem & Andersen in which the stellar disc appears to undergo continual/secular heating. Two other simulations are in better agreement with the Quillen & Garnett observations that suggest 'saturation' in the heating profile for young stars in the disc. None of the simulations has thin discs as old as that of the Milky Way. We also analyse the kinematics of disc stars at the time of their birth for different epochs in the galaxies' evolution and find that in some simulations old stars are born cold within the disc and are subsequently heated, while other simulations possess old stellar populations which are born relatively hot. The models which are in better agreement with observations of the Milky Way's stellar disc undergo significantly lower minor-merger/assembly activity after the last major merger, that is, once the disc has formed. All of the simulations are significantly 'hotter' than the Milky Way disc; on top of the effects of mergers, we find a 'floor' in the dispersion that is related to the underlying treatment of the heating and cooling of the interstellar medium, and the low density threshold which such codes use for star formation. This finding has important implications for all studies of disc heating that use hydrodynamical codes en_US
dc.description.sponsorship ELH acknowledges the support of the UK’s Science & Technology Facilities Council through its PhD studentship programme (ST/F006764/1). BKG and CBB acknowledge the support of the UK’s Science & Technology Facilities Council (ST/F002432/1). PS-B acknowledges the support of a Marie Curie European Reintegration grant within the Sixth European Community Framework Programme. FG acknowledges the support from the HST GO-1125, NSF AST-0607819 and NASA ATP NNX08AG84G grants. RT would like to thank the granted access to the HPC resources of CINES and CCRT under the allocations 2009-SAP2191 and 2010-GEN2192 made by GENCI.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 en_US
dc.format.extent 13 pag. en
dc.format.mimetype application/pdf en
dc.language.iso eng en
dc.publisher The American Astronomical Society en_US
dc.publisher Oxford University Press en_US
dc.relation.ispartof Monthly Notices of the Royal Astronomical Society en_US
dc.rights © 2011 The Authors Monthly Notices of the Royal Astronomical Society en_US
dc.rights © 2011 RAS en_US
dc.subject.other Galaxies: evolution en_US
dc.subject.other Galaxies: formation en_US
dc.subject.other Galaxy: disc en_US
dc.title Disc heating: Comparing the Milky Way with cosmological simulations en_US
dc.type article en
dc.subject.eciencia Física es_ES
dc.relation.publisherversion http://dx.doi.org/10.1111/j.1365-2966.2011.18891.x es_ES
dc.identifier.doi 10.1111/j.1365-2966.2011.18891.x es_ES
dc.identifier.publicationfirstpage 2652 es_ES
dc.identifier.publicationissue 3 es_ES
dc.identifier.publicationlastpage 2664 es_ES
dc.identifier.publicationvolume 415 es_ES
dc.relation.projectID info:eu-repo/grantAgreement/EC/FP7/222919 es_ES
dc.type.version info:eu-repo/semantics/publishedVersion en
dc.rights.accessRights openAccess en
dc.authorUAM Sánchez Blázquez, Patricia (264444)

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