Shapes of Milky-Way-Mass Galaxies with Self-Interacting Dark Matter
Abstract
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.
Additional Information
Attribution 4.0 International (CC BY 4.0). RES acknowledges support from NASA grant 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 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. ASG 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 National Science Foundation 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 National Science Foundation grant number OCI-1053575. DATA AVAILABILITY. The simulations used for this study are currently proprietary to members of the FIRE collaboration. Please contact the authors if interested.Attached Files
Submitted - 2104.14069.pdf
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Additional details
- Eprint ID
- 113640
- Resolver ID
- CaltechAUTHORS:20220228-183235199
- 19-ATP19-0068
- NASA
- HST-AR-15809
- NASA
- NAS5-26555
- NASA
- AST-1752913
- NSF
- AST-1910346
- NSF
- NNX17AG29G
- NASA
- HST-AR-15006
- NASA
- HST-AR-15809
- NASA
- HST-GO-15658
- NASA
- HST-GO-15901
- NASA
- HST-GO-15902
- NASA
- 80NSSC18K1097
- NASA
- 80NSSC20K0513
- NASA
- HST-GO-14734
- NASA
- HST-AR-15057
- NASA
- HST-AR-15809
- NASA
- HST-GO-15902
- NASA
- Scialog Award
- Heising-Simons Foundation
- Hellman Fellowship
- Harlan J. Smith McDonald Observatory
- OAC-1818253
- NSF
- OCI-1053575
- NSF
- Created
-
2022-03-01Created from EPrint's datestamp field
- Updated
-
2023-06-02Created from EPrint's last_modified field
- Caltech groups
- Astronomy Department, TAPIR