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dc.contributor.authorSameie, Omid
dc.contributor.authorCreasey, Peter
dc.contributor.authorYu, Hai-Bo
dc.contributor.authorSales, Laura V
dc.contributor.authorVogelsberger, Mark
dc.contributor.authorZavala, Jesús
dc.date.accessioned2020-04-29T17:46:48Z
dc.date.available2020-04-29T17:46:48Z
dc.date.issued2018-06
dc.date.submitted2018-01
dc.identifier.issn1365-2966
dc.identifier.urihttps://hdl.handle.net/1721.1/124930
dc.description.abstractWe employ isolated N-body simulations to study the response of self-interacting dark matter (SIDM) haloes in the presence of the baryonic potentials. Dark matter self-interactions lead to kinematic thermalization in the inner halo, resulting in a tight correlation between the dark matter and baryon distributions. A deep baryonic potential shortens the phase of SIDM core expansion and triggers core contraction. This effect can be further enhanced by a large selfscattering cross-section. We find the final SIDM density profile is sensitive to the baryonic concentration and the strength of dark matter self-interactions. Assuming a spherical initial halo, we also study evolution of the SIDM halo shape together with the density profile. The halo shape at later epochs deviates from spherical symmetry due to the influence of the non-spherical disc potential, and its significance depends on the baryonic contribution to the total gravitational potential, relative to the dark matter one. In addition, we construct a multicomponent model for the MilkyWay, including an SIDM halo, a stellar disc, and a bulge, and show it is consistent with observations from stellar kinematics and streams. ©2018 The Author(s). Published by Oxford University Press on behalf of The Royal Astronomical Society.en_US
dc.description.sponsorshipNASA MUREP Institutional Research Opportunity (grant no. NNX15AP99A )en_US
dc.description.sponsorshipHubble Space Telescope (grant no. HST-AR-14582)en_US
dc.description.sponsorshipU. S. Department of Energy (grant no. de-sc0008541)en_US
dc.description.sponsorshipHellman Fellows Funden_US
dc.description.sponsorshipMIT RSC awarden_US
dc.description.sponsorshipNASA ATP (grant NNX17AG29G)en_US
dc.description.sponsorshipGrant of Excellence Iceland Research Fund (grant no. 173929-051)en_US
dc.language.isoen
dc.publisherOxford University Press (OUP)en_US
dc.relation.isversionof10.1093/MNRAS/STY1516en_US
dc.rightsCreative Commons Attribution-Noncommercial-Share Alikeen_US
dc.rights.urihttp://creativecommons.org/licenses/by-nc-sa/4.0/en_US
dc.sourcearXiven_US
dc.titleThe impact of baryonic discs on the shapes and profiles of self-interacting dark matter haloesen_US
dc.typeArticleen_US
dc.identifier.citationSameie, Omid et. al., "The impact of baryonic discs on the shapes and profiles of self-interacting dark matter haloes." Monthly Notices of the Royal Astronomical Society 479, 1 (June 2018): 359–67 doi. 10.1093/MNRAS/STY1516 ©2018 Authorsen_US
dc.contributor.departmentMassachusetts Institute of Technology. Department of Physicsen_US
dc.contributor.departmentMIT Kavli Institute for Astrophysics and Space Researchen_US
dc.relation.journalMonthly Notices of the Royal Astronomical Societyen_US
dc.eprint.versionAuthor's final manuscripten_US
dc.type.urihttp://purl.org/eprint/type/JournalArticleen_US
eprint.statushttp://purl.org/eprint/status/PeerRevieweden_US
dc.date.updated2019-06-07T18:50:17Z
dspace.date.submission2019-06-07T18:50:20Z
mit.journal.volume479en_US
mit.journal.issue1en_US


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