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The impact of baryonic physics on the structure of dark matter haloes: the view from the FIRE cosmological simulations

Chan, T. K. and Kereš, D. and Oñorbe, J. and Hopkins, P. F. and Muratov, A. L. and Faucher-Giguère, C.-A. and Quataert, E. (2015) The impact of baryonic physics on the structure of dark matter haloes: the view from the FIRE cosmological simulations. Monthly Notices of the Royal Astronomical Society, 454 (3). pp. 2981-3001. ISSN 0035-8711. http://resolver.caltech.edu/CaltechAUTHORS:20160205-120908533

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Abstract

We study the distribution of cold dark matter (CDM) in cosmological simulations from the FIRE (Feedback In Realistic Environments) project, for M_* ∼ 10^(4–11) M_⊙ galaxies in M_h ∼ 10^(9–12) M_⊙ haloes. FIRE incorporates explicit stellar feedback in the multiphase interstellar medium, with energetics from stellar population models. We find that stellar feedback, without ‘fine-tuned’ parameters, greatly alleviates small-scale problems in CDM. Feedback causes bursts of star formation and outflows, altering the DM distribution. As a result, the inner slope of the DM halo profile (α) shows a strong mass dependence: profiles are shallow at M_h ∼ 10^(10)–10^(11) M_⊙ and steepen at higher/lower masses. The resulting core sizes and slopes are consistent with observations. This is broadly consistent with previous work using simpler feedback schemes, but we find steeper mass dependence of α, and relatively late growth of cores. Because the star formation efficiency M_*/M_h is strongly halo mass dependent, a rapid change in α occurs around M_h ∼ 10^(10) M_⊙ (M_* ∼ 10^6–10^7 M_⊙), as sufficient feedback energy becomes available to perturb the DM. Large cores are not established during the period of rapid growth of haloes because of ongoing DM mass accumulation. Instead, cores require several bursts of star formation after the rapid build-up has completed. Stellar feedback dramatically reduces circular velocities in the inner kpc of massive dwarfs; this could be sufficient to explain the ‘Too Big To Fail’ problem without invoking non-standard DM. Finally, feedback and baryonic contraction in Milky Way-mass haloes produce DM profiles slightly shallower than the Navarro–Frenk–White profile, consistent with the normalization of the observed Tully–Fisher relation.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1093/mnras/stv2165DOIArticle
http://mnras.oxfordjournals.org/content/454/3/2981PublisherArticle
ORCID:
AuthorORCID
Kereš, D.0000-0002-1666-7067
Hopkins, P. F.0000-0003-3729-1684
Quataert, E.0000-0001-9185-5044
Additional Information:© 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2015 September 16. Received 2015 September 14; in original form 2015 July 9. First published online October 17, 2015. We would like to thank N. Murray, J. Bullock, M. Boylan-Kolchin and P. Salucci for useful discussion. DK and TKC were supported in part by NSF grant AST-1412153, Hellman Fellowship and funds from the University of California San Diego. Support for PFH was provided by an Alfred P. Sloan Research Fellowship, NASA ATP Grant NNX14AH35G, and NSF Collaborative Research Grant no. 1411920. EQ was supported in part by NASA ATP grant 12-APT12-0183, a Simons Investigator award from the Simons Foundation, and the David and Lucile Packard Foundation. CAFG was supported by NSF through grant AST-1412836, by NASA through grant NNX15AB22G, and by Northwestern University funds. The simulation presented here used computational resources granted by the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by National Science Foundation grant no. OCI-1053575, specifically allocations TG-AST120025 (PI Kereš), TG-AST130039 (PI Hopkins) and TG-AST1140023 (PI Faucher-Giguère).
Group:TAPIR
Funders:
Funding AgencyGrant Number
NSFAST-1412153
Hellman FellowshipUNSPECIFIED
University of California San DiegoUNSPECIFIED
Alfred P. Sloan FoundationUNSPECIFIED
NASANNX14AH35G
NSF1411920
NASA12-APT12-0183
Simons FoundationUNSPECIFIED
David and Lucile Packard FoundationUNSPECIFIED
NSFAST-1412836
NASANNX15AB22G
Northwestern UniversityUNSPECIFIED
NSFOCI-1053575
NSFTG-AST120025
NSFTG-AST130039
NSFTG-AST1140023
Subject Keywords:galaxies: evolution – galaxies: haloes – galaxies: kinematics and dynamics – galaxies: structure – dark matter
Record Number:CaltechAUTHORS:20160205-120908533
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20160205-120908533
Official Citation:T. K. Chan, D. Kereš, J. Oñorbe, P. F. Hopkins, A. L. Muratov, C.-A. Faucher-Giguère, and E. Quataert The impact of baryonic physics on the structure of dark matter haloes: the view from the FIRE cosmological simulations MNRAS (December 11, 2015) Vol. 454 2981-3001 doi:10.1093/mnras/stv2165 First published online October 17, 2015
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:64277
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:08 Feb 2016 18:51
Last Modified:17 Aug 2017 19:31

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