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Shapes of Milky-Way-mass galaxies with self-interacting dark matter

Vargya, Drona and Sanderson, Robyn and Sameie, Omid and Boylan-Kolchin, Michael and Hopkins, Philip F. and Wetzel, Andrew and Graus, Andrew (2022) Shapes of Milky-Way-mass galaxies with self-interacting dark matter. Monthly Notices of the Royal Astronomical Society, 516 (2). pp. 2389-2405. ISSN 0035-8711. doi:10.1093/mnras/stac2069.

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Self-interacting dark matter (SIDM) models offer one way to reconcile inconsistencies between observations and predictions from collisionless cold dark matter (CDM) models on dwarf-galaxy scales. In order to incorporate the effects of both baryonic and SIDM interactions, we study a suite of cosmological-baryonic simulations of Milky-Way (MW)-mass galaxies from the Feedback in Realistic Environments (FIRE-2) project where we vary the SIDM self-interaction cross-section σ/m. We compare the shape of the main dark matter (DM) halo at redshift z = 0 predicted by SIDM simulations (at σ/m = 0.1, 1, and 10 cm² g⁻¹) with CDM simulations using the same initial conditions. In the presence of baryonic feedback effects, we find that SIDM models do not produce the large differences in the inner structure of MW-mass galaxies predicted by SIDM-only models. However, we do find that the radius where the shape of the total mass distribution begins to differ from that of the stellar mass distribution is dependent on σ/m. This transition could potentially be used to set limits on the SIDM cross-section in the MW.

Item Type:Article
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URLURL TypeDescription ItemDiscussion Paper
Sanderson, Robyn0000-0003-3939-3297
Sameie, Omid0000-0003-4394-6085
Boylan-Kolchin, Michael0000-0002-9604-343X
Hopkins, Philip F.0000-0003-3729-1684
Wetzel, Andrew0000-0003-0603-8942
Additional Information:RS acknowledges support from National Aeronautics and Space Administration (NASA) grants 19-ATP19-0068 and HST-AR-15809 from the Space Telescope Science Institute (STScI), which is operated by AURA, Inc., under NASA contract NAS5-26555. MBK acknowledges support from National Science Foundation (NSF) CAREER award AST-1752913, NSF grant AST-1910346, NASA grant NNX17AG29G, and HST-AR-15006, HST-AR-15809, HST-GO-15658, HST-GO-15901, and HST-GO-15902 from STScI. AW received support from NASA through ATP grants 80NSSC18K1097 and 80NSSC20K0513; HST grants GO-14734, AR-15057, AR-15809, and GO-15902 from STScI; a Scialog Award from the Heising-Simons Foundation; and a Hellman Fellowship. AG is supported by the Harlan J. Smith postdoctoral fellowship. This research is part of the Frontera computing project at the Texas Advanced Computing Center (TACC). Frontera is made possible by NSF award OAC-1818253. Simulations in this project were run using Early Science Allocation 1923870, and analysed using computing resources supported by the Scientific Computing Core at the Flatiron Institute. This work used additional computational resources of the University of Texas at Austin and TACC, the NASA Advanced Supercomputing (NAS) Division and the NASA Center for Climate Simulation (NCCS), and the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by NSF grant number OCI-1053575.
Group:Astronomy Department, TAPIR
Funding AgencyGrant Number
Heising-Simons FoundationUNSPECIFIED
Hellman FellowshipUNSPECIFIED
Harlan J. Smith Postdoctoral FellowshipUNSPECIFIED
Issue or Number:2
Record Number:CaltechAUTHORS:20220926-576716400.13
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:117146
Deposited By: Melissa Ray
Deposited On:30 Sep 2022 16:49
Last Modified:30 Sep 2022 16:49

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