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Simulating galaxies in the reionization era with FIRE-2: galaxy scaling relations, stellar mass functions, and luminosity functions


Ma, Xiangcheng; Hopkins, Philip F; Garrison-Kimmel, Shea; Faucher-Giguère, Claude-André; Quataert, Eliot; Boylan-Kolchin, Michael; Hayward, Christopher C; Feldmann, Robert; Kereš, Dušan (2018). Simulating galaxies in the reionization era with FIRE-2: galaxy scaling relations, stellar mass functions, and luminosity functions. Monthly Notices of the Royal Astronomical Society, 478(2):1694-1715.

Abstract

We present a suite of cosmological zoom-in simulations at z ≥ 5 from the Feedback In Realistic Environments project, spanning a halo mass range Mhalo ∼ 108–1012 M⊙ at z = 5. We predict the stellar mass–halo mass relation, stellar mass function, and luminosity function in several bands from z = 5 to 12. The median stellar mass–halo mass relation does not evolve strongly at z = 5–12. The faint-end slope of the luminosity function steepens with increasing redshift, as inherited from the halo mass function at these redshifts. Below z ∼ 6, the stellar mass function and ultraviolet (UV) luminosity function slightly flatten below M* ∼ 104.5 M⊙ (fainter than M1500 ∼ −12), owing to the fact that star formation in low-mass haloes is suppressed by the ionizing background by the end of reionization. Such flattening does not appear at higher redshifts. We provide redshift-dependent fitting functions for the SFR–Mhalo, SFR–M*, and broad-band magnitude–stellar mass relations. We derive the star formation rate density and stellar mass density at z = 5–12 and show that the contribution from very faint galaxies becomes more important at z > 8. Furthermore, we find that the decline in the z ∼ 6 UV luminosity function brighter than M1500 ∼ −20 is largely due to dust attenuation. Approximately 37 per cent (54 per cent) of the UV luminosity from galaxies brighter than M1500 = −13 (−17) is obscured by dust at z ∼ 6. Our results broadly agree with current data and can be tested by future observations.

Abstract

We present a suite of cosmological zoom-in simulations at z ≥ 5 from the Feedback In Realistic Environments project, spanning a halo mass range Mhalo ∼ 108–1012 M⊙ at z = 5. We predict the stellar mass–halo mass relation, stellar mass function, and luminosity function in several bands from z = 5 to 12. The median stellar mass–halo mass relation does not evolve strongly at z = 5–12. The faint-end slope of the luminosity function steepens with increasing redshift, as inherited from the halo mass function at these redshifts. Below z ∼ 6, the stellar mass function and ultraviolet (UV) luminosity function slightly flatten below M* ∼ 104.5 M⊙ (fainter than M1500 ∼ −12), owing to the fact that star formation in low-mass haloes is suppressed by the ionizing background by the end of reionization. Such flattening does not appear at higher redshifts. We provide redshift-dependent fitting functions for the SFR–Mhalo, SFR–M*, and broad-band magnitude–stellar mass relations. We derive the star formation rate density and stellar mass density at z = 5–12 and show that the contribution from very faint galaxies becomes more important at z > 8. Furthermore, we find that the decline in the z ∼ 6 UV luminosity function brighter than M1500 ∼ −20 is largely due to dust attenuation. Approximately 37 per cent (54 per cent) of the UV luminosity from galaxies brighter than M1500 = −13 (−17) is obscured by dust at z ∼ 6. Our results broadly agree with current data and can be tested by future observations.

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Item Type:Journal Article, refereed, original work
Communities & Collections:07 Faculty of Science > Institute for Computational Science
Dewey Decimal Classification:530 Physics
Uncontrolled Keywords:Space and Planetary Science, Astronomy and Astrophysics
Language:English
Date:1 August 2018
Deposited On:01 Mar 2019 15:56
Last Modified:17 Sep 2019 19:39
Publisher:Oxford University Press
ISSN:0035-8711
OA Status:Green
Free access at:Publisher DOI. An embargo period may apply.
Publisher DOI:https://doi.org/10.1093/mnras/sty1024

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