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Dissipative Dark Matter on FIRE: I. Structural and kinematic properties of dwarf galaxies

Shen, Xuejian and Hopkins, Philip F. and Necib, Lina and Jiang, Fangzhou and Boylan-Kolchin, Michael and Wetzel, Andrew (2021) Dissipative Dark Matter on FIRE: I. Structural and kinematic properties of dwarf galaxies. . (Unpublished)

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We present the first set of cosmological baryonic zoom-in simulations of galaxies including dissipative self-interacting dark matter (dSIDM). These simulations utilize the Feedback In Realistic Environments (FIRE-2) galaxy formation physics, but allow the dark matter to have dissipative self-interactions analogous to Standard Model forces, parameterized by the self-interaction cross-section per unit mass, (σ/m), and the dimensionless degree of dissipation, 0 < f_(diss) < 1. We survey this parameter space, including constant and velocity-dependent cross-sections, and focus on structural and kinematic properties of dwarf galaxies with M_(halo) ≃ 10¹⁰⁻¹¹M⊙ and M* ~ 10⁵⁻⁸ M⊙. Central density profiles of simulated dwarfs become cuspy when (σ/m)_(eff) ≳ 0.1cm²g⁻¹ (and f_(diss) = 0.5 as fiducial). The power-law slopes asymptote to α ≈ −1.5 in low-mass dwarfs independent of cross-section, which arises from a dark matter “cooling flow”. Through comparisons with dark matter only simulations, we find the profile in this regime is insensitive to the inclusion of baryons. However, when (σ/m)_(eff) ≪ 0.1cm²g⁻¹, baryonic effects can produce cored density profiles comparable to non-dissipative cold dark matter (CDM) runs but at smaller radii. Simulated galaxies with (σ/m) ≳ 10cm²g⁻¹ develop significant coherent rotation of dark matter, accompanied by halo deformation, but this is unlike the well-defined thin “dark disks” often attributed to baryon-like dSIDM. The density profiles in this high cross-section model exhibit lower normalizations given the onset of halo deformation. For our surveyed dSIDM parameters, halo masses and galaxy stellar masses do not show appreciable difference from CDM, but dark matter kinematics and halo concentrations/shapes can differ.

Item Type:Report or Paper (Discussion Paper)
Related URLs:
URLURL TypeDescription Paper
Shen, Xuejian0000-0002-6196-823X
Hopkins, Philip F.0000-0003-3729-1684
Necib, Lina0000-0003-2806-1414
Boylan-Kolchin, Michael0000-0002-9604-343X
Wetzel, Andrew0000-0003-0603-8942
Additional Information:© 2021 The Authors. Support for PFH was provided by NSF Research Grants 1911233 & 20009234, NSF CAREER grant 1455342, NASA grants 80NSSC18K0562, HST-AR-15800.001-A. Numerical calculations were run on the Caltech compute cluster “Wheeler”, allocations FTA-Hopkins/AST20016 supported by the NSF and TACC, and NASA HEC SMD-16-7592. LN is supported by the DOE under Award Number DESC0011632, the Sherman Fairchild fellowship, the University of California Presidential fellowship, and the fellowship of theoretical astrophysics at Carnegie Observatories. FJ is supported by the Troesh scholarship. 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, HST-GO-15902, HST-AR-16159, and HST-GO-16226 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS5-26555. 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.
Group:Astronomy Department, TAPIR, Walter Burke Institute for Theoretical Physics
Funding AgencyGrant Number
Department of Energy (DOE)DE-SC0011632
Sherman Fairchild FoundationUNSPECIFIED
University of CaliforniaUNSPECIFIED
Carnegie ObservatoriesUNSPECIFIED
Troesh ScholarshipUNSPECIFIED
NASA Hubble FellowshipGO-14734
NASA Hubble FellowshipAR-15057
NASA Hubble FellowshipGO-15902
Heising-Simons FoundationUNSPECIFIED
Hellman FellowshipUNSPECIFIED
Subject Keywords:methods : numerical – galaxies : dwarf – galaxies : haloes – cosmology : dark matter – cosmology : theory
Record Number:CaltechAUTHORS:20210428-103121850
Persistent URL:
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:108858
Deposited By: Tony Diaz
Deposited On:28 Apr 2021 18:14
Last Modified:28 Apr 2021 18:14

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