The impact of baryonic discs on the shapes and profiles of self-interacting dark matter haloes
We 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...
| Autori principali: | , , , , , |
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| Natura: | Articolo |
| Lingua: | English |
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Oxford University Press (OUP)
2020
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| Accesso online: | https://hdl.handle.net/1721.1/124930 |
| _version_ | 1826216406609297408 |
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| author | Sameie, Omid Creasey, Peter Yu, Hai-Bo Sales, Laura V Vogelsberger, Mark Zavala, Jesús |
| author2 | Massachusetts Institute of Technology. Department of Physics |
| author_facet | Massachusetts Institute of Technology. Department of Physics Sameie, Omid Creasey, Peter Yu, Hai-Bo Sales, Laura V Vogelsberger, Mark Zavala, Jesús |
| author_sort | Sameie, Omid |
| collection | MIT |
| description | We 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. |
| first_indexed | 2024-09-23T16:46:49Z |
| format | Article |
| id | mit-1721.1/124930 |
| institution | Massachusetts Institute of Technology |
| language | English |
| last_indexed | 2024-09-23T16:46:49Z |
| publishDate | 2020 |
| publisher | Oxford University Press (OUP) |
| record_format | dspace |
| spelling | mit-1721.1/1249302022-10-03T08:16:00Z The impact of baryonic discs on the shapes and profiles of self-interacting dark matter haloes Sameie, Omid Creasey, Peter Yu, Hai-Bo Sales, Laura V Vogelsberger, Mark Zavala, Jesús Massachusetts Institute of Technology. Department of Physics MIT Kavli Institute for Astrophysics and Space Research We 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. NASA MUREP Institutional Research Opportunity (grant no. NNX15AP99A ) Hubble Space Telescope (grant no. HST-AR-14582) U. S. Department of Energy (grant no. de-sc0008541) Hellman Fellows Fund MIT RSC award NASA ATP (grant NNX17AG29G) Grant of Excellence Iceland Research Fund (grant no. 173929-051) 2020-04-29T17:46:48Z 2020-04-29T17:46:48Z 2018-06 2018-01 2019-06-07T18:50:17Z Article http://purl.org/eprint/type/JournalArticle 1365-2966 https://hdl.handle.net/1721.1/124930 Sameie, 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 Authors en 10.1093/MNRAS/STY1516 Monthly Notices of the Royal Astronomical Society Creative Commons Attribution-Noncommercial-Share Alike http://creativecommons.org/licenses/by-nc-sa/4.0/ application/pdf Oxford University Press (OUP) arXiv |
| spellingShingle | Sameie, Omid Creasey, Peter Yu, Hai-Bo Sales, Laura V Vogelsberger, Mark Zavala, Jesús The impact of baryonic discs on the shapes and profiles of self-interacting dark matter haloes |
| title | The impact of baryonic discs on the shapes and profiles of self-interacting dark matter haloes |
| title_full | The impact of baryonic discs on the shapes and profiles of self-interacting dark matter haloes |
| title_fullStr | The impact of baryonic discs on the shapes and profiles of self-interacting dark matter haloes |
| title_full_unstemmed | The impact of baryonic discs on the shapes and profiles of self-interacting dark matter haloes |
| title_short | The impact of baryonic discs on the shapes and profiles of self-interacting dark matter haloes |
| title_sort | impact of baryonic discs on the shapes and profiles of self interacting dark matter haloes |
| url | https://hdl.handle.net/1721.1/124930 |
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