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The central densities of Milky Way-mass galaxies in cold and self-interacting dark matter models

Sameie, Omid and Boylan-Kolchin, Michael and Sanderson, Robyn and Vargya, Drona and Hopkins, Philip F. and Wetzel, Andrew and Bullock, James S. and Graus, Andrew and Robles, Victor H. (2021) The central densities of Milky Way-mass galaxies in cold and self-interacting dark matter models. Monthly Notices of the Royal Astronomical Society, 507 (1). pp. 720-729. ISSN 0035-8711. doi:10.1093/mnras/stab2173.

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We present a suite of baryonic cosmological zoom-in simulations of self-interacting dark matter (SIDM) haloes within the ‘Feedback In Realistic Environment’ (FIRE) project. The three simulated haloes have virial masses of ∼10¹²M⊙ at z = 0, and we study velocity-independent self-interaction cross sections of 1 and 10 cm²g⁻¹⁠. We study star formation rates and the shape of dark matter density profiles of the parent haloes in both cold dark matter (CDM) and SIDM models. Galaxies formed in the SIDM haloes have higher star formation rates at z ≤ 1, resulting in more massive galaxies compared to the CDM simulations. While both CDM and SIDM simulations show diverse shape of the dark matter density profiles, the SIDM haloes can reach higher and more steep central densities within few kpcs compared to the CDM haloes. We identify a correlation between the build-up of the stars within the half-mass radii of the galaxies and the growth in the central dark matter densities. The thermalization process in the SIDM haloes is enhanced in the presence of a dense stellar component. Hence, SIDM haloes with highly concentrated baryonic profiles are predicted to have higher central dark matter densities than the CDM haloes. Overall, the SIDM haloes are more responsive to the presence of a massive baryonic distribution than their CDM counterparts.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Sameie, Omid0000-0003-4394-6085
Boylan-Kolchin, Michael0000-0002-9604-343X
Sanderson, Robyn0000-0003-3939-3297
Hopkins, Philip F.0000-0003-3729-1684
Wetzel, Andrew0000-0003-0603-8942
Bullock, James S.0000-0003-4298-5082
Robles, Victor H.0000-0002-9497-9963
Additional Information:© 2021 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model ( Accepted 2021 July 19. Received 2021 June 23; in original form 2021 February 24. Published: 31 July 2021. We thank Hai-Bo Yu for insightful discussions and the anonymous referee for a helpful and constructive report. 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. RES acknowledges support from NASA grant 19-ATP19-0068, the Research Corporation for Scientific Advancement through Scialog-TDA, and grant HST-AR-15809 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS5-26555. 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. AW received support from NASA through ATP grants 80NSSC18K1097 and 80NSSC20K0513; HST grants GO-14734, AR-15057, AR-15809, and GO-15902 from STScI; the Heising-Simons Foundation; and a Hellman Fellowship. ASG is supported by the McDonald Observatory via the Harlan J. Smith postdoctoral fellowship. We ran simulations using: XSEDE, supported by NSF grant ACI-1548562; Blue Waters, supported by the NSF; Pleiades, via the NASA HEC program through the NASA Division at Ames Research Center. The analysis in this paper is carried out by python packages NUMPY (van der Walt, Colbert & Varoquaux 2011), MATPLOTLIB (Hunter 2007), SCIPY (Oliphant 2007), and H5PY (Collette 2013). Data Availability: The data supporting the plots within this article are available on reasonable request to the corresponding author.
Group:Astronomy Department, TAPIR
Funding AgencyGrant Number
Research CorporationUNSPECIFIED
NASA Hubble FellowshipGO-14734
NASA Hubble FellowshipAR-15057
NASA Hubble FellowshipAR-15809
NASA Hubble FellowshipGO-15902
Heising-Simons FoundationUNSPECIFIED
Hellman FellowshipUNSPECIFIED
McDonald ObservatoryUNSPECIFIED
Subject Keywords:methods: numerical – galaxies: evolution – galaxies: formation – galaxies: structure – dark matter
Issue or Number:1
Record Number:CaltechAUTHORS:20211020-212403723
Persistent URL:
Official Citation:Omid Sameie, Michael Boylan-Kolchin, Robyn Sanderson, Drona Vargya, Philip F Hopkins, Andrew Wetzel, James Bullock, Andrew Graus, Victor H Robles, The central densities of Milky Way-mass galaxies in cold and self-interacting dark matter models, Monthly Notices of the Royal Astronomical Society, Volume 507, Issue 1, October 2021, Pages 720–729,
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:111560
Deposited By: Tony Diaz
Deposited On:20 Oct 2021 22:49
Last Modified:21 Oct 2021 16:36

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