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Dust attenuation, dust emission, and dust temperature in galaxies at z ≥ 5: a view from the FIRE-2 simulations

Ma, Xiangcheng and Hayward, Christopher C. and Casey, Caitlin M. and Hopkins, Philip F. and Quataert, Eliot and Liang, Lichen and Faucher-Giguère, Claude-André and Feldmann, Robert and Kereš, Dušan (2019) Dust attenuation, dust emission, and dust temperature in galaxies at z ≥ 5: a view from the FIRE-2 simulations. Monthly Notices of the Royal Astronomical Society, 487 (2). pp. 1844-1864. ISSN 0035-8711. https://resolver.caltech.edu/CaltechAUTHORS:20190725-125944777

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Abstract

We present a suite of 34 high-resolution cosmological zoom-in simulations consisting of thousands of haloes up to M_(halo) ∼ 10^(12) M_⊙ (⁠M_∗ ∼ 10^(10.5) M_⊙⁠) at z ≥ 5 from the Feedback in Realistic Environments project. We post-process our simulations with a three-dimensional Monte Carlo dust radiative transfer code to study dust attenuation, dust emission, and dust temperature within these simulated z ≥ 5 galaxies. Our sample forms a tight correlation between infrared excess (IRX ≡ F_(IR)/F_(UV)) and ultraviolet (UV)-continuum slope (βUV), despite the patchy, clumpy dust geometry shown in our simulations. We find that the IRX–βUV relation is mainly determined by the shape of the attenuation law and is independent of its normalization (set by the dust-to-gas ratio). The bolometric IR luminosity (L_(IR)) correlates with the intrinsic UV luminosity and the star formation rate (SFR) averaged over the past 10 Myr. We predict that at a given L_(IR), the peak wavelength of the dust spectral energy distributions for z ≥ 5 galaxies is smaller by a factor of 2 (due to higher dust temperatures on average) than at z = 0. The higher dust temperatures are driven by higher specific SFRs and SFR surface densities with increasing redshift. We derive the galaxy UV luminosity functions (UVLFs) at z = 5–10 from our simulations and confirm that a heavy attenuation is required to reproduce the observed bright-end UVLFs. We also predict the IR luminosity functions (IRLFs) and UV luminosity densities at z = 5–10. We discuss the implications of our results on current and future observations probing dust attenuation and emission in z ≥ 5 galaxies.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1093/mnras/stz1324DOIArticle
https://arxiv.org/abs/1902.10152arXivDiscussion Paper
ORCID:
AuthorORCID
Ma, Xiangcheng0000-0001-8091-2349
Hayward, Christopher C.0000-0003-4073-3236
Casey, Caitlin M.0000-0002-0930-6466
Hopkins, Philip F.0000-0003-3729-1684
Quataert, Eliot0000-0001-9185-5044
Liang, Lichen0000-0001-9422-0095
Faucher-Giguère, Claude-André0000-0002-4900-6628
Feldmann, Robert0000-0002-1109-1919
Kereš, Dušan0000-0002-1666-7067
Additional Information:© 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model) Accepted 2019 May 8. Received 2019 May 5; in original form 2019 February 25. We thank our referee, Maarten Baes, for helpful suggestions and for pointing out our mistakes in an earlier version of this paper in describing the technical details of the SKIRT code. The simulations used in this paper were run on XSEDE computational resources (allocations TG-AST120025, TG-AST130039, TG-AST140023, and TG-AST140064). CMC thanks the University of Texas at Austin College of Natural Sciences, NSF grants AST-1714528, AST-1814034, and a 2019 Cottrell Scholar Award for support from the Research Corporation for Science Advancement. PFH was supported by an Alfred P. Sloan Research Fellowship, NASA ATP Grant NNX14AH35G, and NSF Collaborative Research Grant #1411920 and CAREER grant #1455342. CAFG was supported by NSF through grants AST-1517491, AST-1715216, and CAREER award AST-1652522; by NASA through grant 17-ATP17-0067; by STScI through grant HST-AR-14562.001; and by a Cottrell Scholar Award from the Research Corporation for Science Advancement. EQ was supported by NASA ATP grant 12-APT12-0183, a Simons Investigator award from the Simons Foundation, and the David and Lucile Packard Foundation. RF acknowledges financial support from the Swiss National Science Foundation (grant no. 157591). DK was supported by NSF grant AST-1412153, funds from the University of California, San Diego, and a Cottrell Scholar Award from the Research Corporation for Science Advancement. The Flatiron Institute is supported by the Simons Foundation.
Group:TAPIR, Astronomy Department
Funders:
Funding AgencyGrant Number
NSFTG-AST120025
NSFTG-AST130039
NSFTG-AST140023
NSFTG-AST140064
University of Texas at AustinUNSPECIFIED
NSFAST-1714528
NSFAST-1814034
Cottrell Scholar of Research CorporationUNSPECIFIED
Alfred P. Sloan FoundationUNSPECIFIED
NASANNX14AH35G
NSFAST-1411920
NSFAST-1455342
NSFAST-1517491
NSFAST-1715216
NSFAST-1652522
NASA17-ATP17-0067
NASA Hubble FellowshipHST-AR-14562.001
NASA12-APT12-0183
Simons FoundationUNSPECIFIED
Swiss National Science Foundation (SNSF)157591
David and Lucile Packard FoundationUNSPECIFIED
NSFAST-1412153
University of California San DiegoUNSPECIFIED
Flatiron InstituteUNSPECIFIED
Subject Keywords:(ISM:) dust, extinction, galaxies: evolution, galaxies: formation, galaxies: high-redshift, cosmology: theory
Issue or Number:2
Record Number:CaltechAUTHORS:20190725-125944777
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20190725-125944777
Official Citation:Xiangcheng Ma, Christopher C Hayward, Caitlin M Casey, Philip F Hopkins, Eliot Quataert, Lichen Liang, Claude-André Faucher-Giguère, Robert Feldmann, Dušan Kereš, Dust attenuation, dust emission, and dust temperature in galaxies at z ≥ 5: a view from the FIRE-2 simulations, Monthly Notices of the Royal Astronomical Society, Volume 487, Issue 2, August 2019, Pages 1844–1864, https://doi.org/10.1093/mnras/stz1324
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:97418
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:25 Jul 2019 20:41
Last Modified:03 Oct 2019 21:31

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