CaltechAUTHORS
  A Caltech Library Service

Gusty, gaseous flows of FIRE: galactic winds in cosmological simulations with explicit stellar feedback

Muratov, Alexander L. and Kereš, Dušan and Faucher-Giguère, Claude-André and Hopkins, Philip F. and Quataert, Eliot and Murray, Norman (2015) Gusty, gaseous flows of FIRE: galactic winds in cosmological simulations with explicit stellar feedback. Monthly Notices of the Royal Astronomical Society, 454 (3). pp. 2691-2713. ISSN 0035-8711. http://resolver.caltech.edu/CaltechAUTHORS:20160205-132422140

[img] PDF - Published Version
See Usage Policy.

1967Kb

Use this Persistent URL to link to this item: http://resolver.caltech.edu/CaltechAUTHORS:20160205-132422140

Abstract

We present an analysis of the galaxy-scale gaseous outflows from the Feedback in Realistic Environments (FIRE) simulations. This suite of hydrodynamic cosmological zoom simulations resolves formation of star-forming giant molecular clouds to z = 0, and features an explicit stellar feedback model on small scales. Our simulations reveal that high-redshift galaxies undergo bursts of star formation followed by powerful gusts of galactic outflows that eject much of the interstellar medium and temporarily suppress star formation. At low redshift, however, sufficiently massive galaxies corresponding to L* progenitors develop stable discs and switch into a continuous and quiescent mode of star formation that does not drive outflows far into the halo. Mass-loading factors for winds in L* progenitors are η ≈ 10 at high redshift, but decrease to η ≪ 1 at low redshift. Although lower values of η are expected as haloes grow in mass over time, we show that the strong suppression of outflows with decreasing redshift cannot be explained by mass evolution alone. Circumgalactic outflow velocities are variable and broadly distributed, but typically range between one and three times the circular velocity of the halo. Much of the ejected material builds a reservoir of enriched gas within the circumgalactic medium, some of which could be later recycled to fuel further star formation. However, a fraction of the gas that leaves the virial radius through galactic winds is never regained, causing most haloes with mass M_h ≤ 10^(12) M_⊙ to be deficient in baryons compared to the cosmic mean by z = 0.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1093/mnras/stv2126DOIArticle
http://mnras.oxfordjournals.org/content/454/3/2691PublisherArticle
http://fire.northwestern.eduRelated ItemFIRE website
ORCID:
AuthorORCID
Kereš, Dušan0000-0002-1666-7067
Hopkins, Philip F.0000-0003-3729-1684
Quataert, Eliot0000-0001-9185-5044
Additional Information:© 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2015 September 11. Received 2015 September 10; in original form 2015 January 12. First published online October 13, 2015. We thank Tsang-Keung Chan, Xiangcheng Ma, Daniel Anglés-Alcázar, Freeke van de Voort, Robert Feldmann, Chris Hayward, and Michael Anderson for various constructive suggestions. We thank Romeel Davé for providing details on wind implementation for our simulation comparison section. We thank the anonymous referee for providing suggestions that improved this work. DK was supported by a Hellman Fellowship and NSF grant AST-1412153, and by funds from the University of California San Diego. Support for PFH was provided by the Gordon and Betty Moore Foundation through Grant 776 to the Caltech Moore Center for Theoretical Cosmology and Physics, by the Alfred P. Sloan Foundation through Sloan Research Fellowship BR2014-022, and by NSF through grant AST-1411920. C-AF-G was supported by NSF through grant AST-1412836, by NASA through grant NNX15AB22G, and by Northwestern University funds. EQ was supported by NASA ATP grant 12-APT12-0183, a Simons Investigator award from the Simons Foundation, the David and Lucile Packard Foundation, and the Thomas Alison Schneider Chair in Physics at UC Berkeley. The simulations analysed in this paper were run on XSEDE computational resources (allocations TG-AST120025, TG-AST130039, and TG-AST140023). We would like to thank the Simons Foundation and the participants of the Galactic Super Winds symposium for stimulating discussions. We would also like to thank the Kavli Institute for Theoretical Physics and the participants of the Physics of Star Formation Feedback program for interactions that improved this work.
Group:TAPIR, Moore Center for Theoretical Cosmology and Physics
Funders:
Funding AgencyGrant Number
NSFAST-1412153
University of California San DiegoUNSPECIFIED
Gordon and Betty Moore Foundation776
Caltech Moore Center for Theoretical Cosmology and PhysicsUNSPECIFIED
Alfred P. Sloan FoundationBR2014-022
NSFAST-1411920
NSFAST-1412836
NASANNX15AB22G
Northwestern UniversityUNSPECIFIED
NASA12-APT12-0183
Simons FoundationUNSPECIFIED
David and Lucile Packard FoundationUNSPECIFIED
Thomas Alison Schneider Chair in Physics at UC BerkeleyUNSPECIFIED
NSFTG-AST120025
NSFTG-AST130039
NSFTG-AST140023
Subject Keywords:stars: formation – galaxies: evolution – galaxies: formation – cosmology: theory
Record Number:CaltechAUTHORS:20160205-132422140
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20160205-132422140
Official Citation:Alexander L. Muratov, Dušan Kereš, Claude-André Faucher-Giguère, Philip F. Hopkins, Eliot Quataert, and Norman Murray Gusty, gaseous flows of FIRE: galactic winds in cosmological simulations with explicit stellar feedback MNRAS (December 11, 2015) Vol. 454 2691-2713 doi:10.1093/mnras/stv2126 First published online October 13, 2015
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:64281
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:08 Feb 2016 17:55
Last Modified:17 Aug 2017 19:30

Repository Staff Only: item control page