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

Xiangcheng Ma, Christopher C. Hayward, Caitlin M. Casey, Philip F. Hopkins, Eliot Quataert, Lichen Liang, Claude-Andre Faucher-Giguere, Robert Feldmann, Dušan Kereš

Research output: Contribution to journalArticle

2 Citations (Scopus)

Abstract

We present a suite of 34 high-resolution cosmological zoom-in simulations consisting of thousands of haloes up to Mhalo ~ 1012M (M ~ 1010.5M) 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 (IRXΞFIR/FUV) 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 lawand is independent of its normalization (set by the dust-to-gas ratio). The bolometric IR luminosity (LIR) correlates with the intrinsic UV luminosity and the star formation rate (SFR) averaged over the past 10Myr. We predict that at a given LIR, 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.

Original languageEnglish (US)
Pages (from-to)1844-1864
Number of pages21
JournalMonthly Notices of the Royal Astronomical Society
Volume487
Issue number2
DOIs
StatePublished - Jan 1 2019

Fingerprint

FIRE (climatology)
dust
attenuation
galaxies
simulation
luminosity
temperature
star formation rate
spectral energy distribution
radiative transfer
halos

Keywords

  • (ISM:) dust, extinction
  • Cosmology: theory
  • Galaxies: evolution
  • Galaxies: formation
  • Galaxies: high-redshift

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Ma, Xiangcheng ; Hayward, Christopher C. ; Casey, Caitlin M. ; Hopkins, Philip F. ; Quataert, Eliot ; Liang, Lichen ; Faucher-Giguere, Claude-Andre ; Feldmann, Robert ; Kereš, Dušan. / Dust attenuation, dust emission, and dust temperature in galaxies at z ≥ 5 : A view from the FIRE-2 simulations. In: Monthly Notices of the Royal Astronomical Society. 2019 ; Vol. 487, No. 2. pp. 1844-1864.
@article{c3f22370ae0c4d50bc7f6a8ef440fc3d,
title = "Dust attenuation, dust emission, and dust temperature in galaxies at z ≥ 5: A view from the FIRE-2 simulations",
abstract = "We present a suite of 34 high-resolution cosmological zoom-in simulations consisting of thousands of haloes up to Mhalo ~ 1012M⊙ (M∗ ~ 1010.5M⊙) 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 (IRXΞFIR/FUV) 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 lawand is independent of its normalization (set by the dust-to-gas ratio). The bolometric IR luminosity (LIR) correlates with the intrinsic UV luminosity and the star formation rate (SFR) averaged over the past 10Myr. We predict that at a given LIR, 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.",
keywords = "(ISM:) dust, extinction, Cosmology: theory, Galaxies: evolution, Galaxies: formation, Galaxies: high-redshift",
author = "Xiangcheng Ma and Hayward, {Christopher C.} and Casey, {Caitlin M.} and Hopkins, {Philip F.} and Eliot Quataert and Lichen Liang and Claude-Andre Faucher-Giguere and Robert Feldmann and Dušan Kereš",
year = "2019",
month = "1",
day = "1",
doi = "10.1093/mnras/stz1324",
language = "English (US)",
volume = "487",
pages = "1844--1864",
journal = "Monthly Notices of the Royal Astronomical Society: Letters",
issn = "1745-3933",
publisher = "Oxford University Press",
number = "2",

}

Dust attenuation, dust emission, and dust temperature in galaxies at z ≥ 5 : A view from the FIRE-2 simulations. / Ma, Xiangcheng; Hayward, Christopher C.; Casey, Caitlin M.; Hopkins, Philip F.; Quataert, Eliot; Liang, Lichen; Faucher-Giguere, Claude-Andre; Feldmann, Robert; Kereš, Dušan.

In: Monthly Notices of the Royal Astronomical Society, Vol. 487, No. 2, 01.01.2019, p. 1844-1864.

Research output: Contribution to journalArticle

TY - JOUR

T1 - Dust attenuation, dust emission, and dust temperature in galaxies at z ≥ 5

T2 - A view from the FIRE-2 simulations

AU - Ma, Xiangcheng

AU - Hayward, Christopher C.

AU - Casey, Caitlin M.

AU - Hopkins, Philip F.

AU - Quataert, Eliot

AU - Liang, Lichen

AU - Faucher-Giguere, Claude-Andre

AU - Feldmann, Robert

AU - Kereš, Dušan

PY - 2019/1/1

Y1 - 2019/1/1

N2 - We present a suite of 34 high-resolution cosmological zoom-in simulations consisting of thousands of haloes up to Mhalo ~ 1012M⊙ (M∗ ~ 1010.5M⊙) 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 (IRXΞFIR/FUV) 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 lawand is independent of its normalization (set by the dust-to-gas ratio). The bolometric IR luminosity (LIR) correlates with the intrinsic UV luminosity and the star formation rate (SFR) averaged over the past 10Myr. We predict that at a given LIR, 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.

AB - We present a suite of 34 high-resolution cosmological zoom-in simulations consisting of thousands of haloes up to Mhalo ~ 1012M⊙ (M∗ ~ 1010.5M⊙) 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 (IRXΞFIR/FUV) 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 lawand is independent of its normalization (set by the dust-to-gas ratio). The bolometric IR luminosity (LIR) correlates with the intrinsic UV luminosity and the star formation rate (SFR) averaged over the past 10Myr. We predict that at a given LIR, 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.

KW - (ISM:) dust, extinction

KW - Cosmology: theory

KW - Galaxies: evolution

KW - Galaxies: formation

KW - Galaxies: high-redshift

UR - http://www.scopus.com/inward/record.url?scp=85071149016&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=85071149016&partnerID=8YFLogxK

U2 - 10.1093/mnras/stz1324

DO - 10.1093/mnras/stz1324

M3 - Article

AN - SCOPUS:85071149016

VL - 487

SP - 1844

EP - 1864

JO - Monthly Notices of the Royal Astronomical Society: Letters

JF - Monthly Notices of the Royal Astronomical Society: Letters

SN - 1745-3933

IS - 2

ER -