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Title: The impact of baryonic discs on the shapes and profiles of self-interacting dark matter haloes

Abstract

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 self-scattering 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 Milky Way, including an SIDM halo, a stellar disc, and a bulge, and show it is consistent with observations from stellar kinematics and streams.

Authors:
 [1];  [1];  [1];  [1];  [2];  [3]
  1. Univ. of California, Riverside, CA (United States)
  2. Massachusetts Inst. of Technology (MIT), Cambridge, MA (United States)
  3. Univ. of Iceland, Reykjavik (Iceland)
Publication Date:
Research Org.:
Univ. of California, Riverside, CA (United States)
Sponsoring Org.:
USDOE Office of Science (SC)
OSTI Identifier:
1540623
Grant/Contract Number:  
SC0008541
Resource Type:
Accepted Manuscript
Journal Name:
Monthly Notices of the Royal Astronomical Society
Additional Journal Information:
Journal Volume: 479; Journal Issue: 1; Journal ID: ISSN 0035-8711
Publisher:
Royal Astronomical Society
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; Astronomy & Astrophysics

Citation Formats

Sameie, Omid, Creasey, Peter, Yu, Hai-Bo, Sales, Laura V., Vogelsberger, Mark, and Zavala, Jesús. The impact of baryonic discs on the shapes and profiles of self-interacting dark matter haloes. United States: N. p., 2018. Web. doi:10.1093/mnras/sty1516.
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. United States. doi:10.1093/mnras/sty1516.
Sameie, Omid, Creasey, Peter, Yu, Hai-Bo, Sales, Laura V., Vogelsberger, Mark, and Zavala, Jesús. Mon . "The impact of baryonic discs on the shapes and profiles of self-interacting dark matter haloes". United States. doi:10.1093/mnras/sty1516. https://www.osti.gov/servlets/purl/1540623.
@article{osti_1540623,
title = {The impact of baryonic discs on the shapes and profiles of self-interacting dark matter haloes},
author = {Sameie, Omid and Creasey, Peter and Yu, Hai-Bo and Sales, Laura V. and Vogelsberger, Mark and Zavala, Jesús},
abstractNote = {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 self-scattering 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 Milky Way, including an SIDM halo, a stellar disc, and a bulge, and show it is consistent with observations from stellar kinematics and streams.},
doi = {10.1093/mnras/sty1516},
journal = {Monthly Notices of the Royal Astronomical Society},
number = 1,
volume = 479,
place = {United States},
year = {2018},
month = {6}
}

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Cited by: 9 works
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