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SIDM on fire: hydrodynamical self-interacting dark matter simulations of low-mass dwarf galaxies

Robles, Victor H. and Bullock, James S. and Elbert, Oliver D. and Fitts, Alex and González-Samaniego, Alejandro and Boylan-Kolchin, Michael and Hopkins, Philip F. and Faucher-Giguère, Claude-André and Kereš, Dušan and Hayward, Christopher C. (2017) SIDM on fire: hydrodynamical self-interacting dark matter simulations of low-mass dwarf galaxies. Monthly Notices of the Royal Astronomical Society, 472 (3). pp. 2945-2954. ISSN 0035-8711. PMCID PMC6310025. http://resolver.caltech.edu/CaltechAUTHORS:20171103-075627443

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Abstract

We compare a suite of four simulated dwarf galaxies formed in 10^(10)  M_⊙ haloes of collisionless cold dark matter (CDM) with galaxies simulated in the same haloes with an identical galaxy formation model but a non-zero cross-section for DM self-interactions. These cosmological zoom-in simulations are part of the Feedback In Realistic Environments (FIRE) project and utilize the FIRE-2 model for hydrodynamics and galaxy formation physics. We find the stellar masses of the galaxies formed in self-interacting dark matter (SIDM) with σ/m = 1 cm^2 g^(−1) are very similar to those in CDM (spanning M⋆ ≈ 10^(5.7–7.0)M_⊙) and all runs lie on a similar stellar mass–size relation. The logarithmic DM density slope (α = d log ρ/d log r) in the central 250-500pc remains steeper than α = −0.8 for the CDM-Hydro simulations with stellar mass M⋆ ∼ 10^(6.6) M_⊙ and core-like in the most massive galaxy. In contrast, every SIDM hydrodynamic simulation yields a flatter profile, with α > −0.4. Moreover, the central density profiles predicted in SIDM runs without baryons are similar to the SIDM runs that include FIRE-2 baryonic physics. Thus, SIDM appears to be much more robust to the inclusion of (potentially uncertain) baryonic physics than CDM on this mass scale, suggesting that SIDM will be easier to falsify than CDM using low-mass galaxies. Our FIRE simulations predict that galaxies less massive than M⋆ ≲ 3 × 10^6  M_⊙ provide potentially ideal targets for discriminating models, with SIDM producing substantial cores in such tiny galaxies and CDM producing cusps.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1093/mnras/stx2253DOIArticle
https://www.ncbi.nlm.nih.gov/pmc/articles/PMC6310025PubMed CentralArticle
https://arxiv.org/abs/1706.07514arXivDiscussion Paper
ORCID:
AuthorORCID
Boylan-Kolchin, Michael0000-0002-9604-343X
Hopkins, Philip F.0000-0003-3729-1684
Faucher-Giguère, Claude-André0000-0002-4900-6628
Kereš, Dušan0000-0002-1666-7067
Hayward, Christopher C.0000-0003-4073-3236
Additional Information:© 2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2017 August 30. Received 2017 August 26; in original form 2017 June 16. Published: 05 September 2017. VHR acknowledges support from University of California Institute for Mexico and the United States (UC MEXUS) and Consejo Nacional de Ciencia y Tecnología (CONACyT) through the postdoctoral fellowship. AG-S acknowledges support from UC-MEXUS through the postdoctoral Fellowship. JSB and ODE are supported by National Science Foundation (NSF) AST-1518291, HST-AR-14282, HST-AR-13888 and NSF-PHY-1520921. MB-K acknowledges support from NSF grant AST-1517226 and from NASA grants NNX17AG29G and HST-AR-12836, HST-AR-13888, HST-AR-13896 and HST-AR-14282 from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. DK was supported by NSF grant AST-1412153 and the Cottrell Scholar Award from the Research Corporation for Science Advancement. C-AF-G was supported by NSF through grants AST-1412836 and AST-1517491, and by NASA through grant NNX15AB22G. Our simulations used computational resources provided via the NASA Advanced Supercomputing (NAS) Division and the NASA Center for Climate Simulation (NCCS) and the Extreme Science and Engineering Discovery Environment, which is supported by National Science Foundation grant number OCI-1053575.
Group:TAPIR
Funders:
Funding AgencyGrant Number
University of California Institute for Mexico and the United States (UC MEXUS)UNSPECIFIED
Consejo Nacional de Ciencia y Tecnología (CONACyT)UNSPECIFIED
NSFAST-1518291
NASAHST-AR-14282
NASAHST-AR-13888
NSFPHY-1520921
NSFAST-1517226
NASANNX17AG29G
NASAHST-AR-12836
NASAHST-AR-13896
NASANAS5-26555
NSFAST-1412153
Research Corporation for Science AdvancementUNSPECIFIED
NSFAST-1412836
NSFAST-1517491
NASANNX15AB22G
NSFOCI-1053575
Subject Keywords:galaxies: dwarf – galaxies: evolution – galaxies: formation – galaxies: haloes – Local Group
PubMed Central ID:PMC6310025
Record Number:CaltechAUTHORS:20171103-075627443
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20171103-075627443
Official Citation:Victor H. Robles, James S. Bullock, Oliver D. Elbert, Alex Fitts, Alejandro González-Samaniego, Michael Boylan-Kolchin, Philip F. Hopkins, Claude-André Faucher-Giguère, Dušan Kereš, Christopher C. Hayward; SIDM on FIRE: hydrodynamical self-interacting dark matter simulations of low-mass dwarf galaxies, Monthly Notices of the Royal Astronomical Society, Volume 472, Issue 3, 11 December 2017, Pages 2945–2954, https://doi.org/10.1093/mnras/stx2253
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:82926
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:03 Nov 2017 17:07
Last Modified:02 Jan 2019 16:54

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