Astraeus IV: Quantifying the star foation histories of galaxies in the Epoch of Reionization
Entidad
UAM. Departamento de Física TeóricaEditor
Royal Astronomical Society; Oxford University PressFecha de edición
2021-10-25Cita
10.1093/mnras/stab3034
Monthly Notices of the Royal Astronomical Society 509.1 (2022): 595-613
ISSN
0035-8711 (print); 1365-2966 (online)DOI
10.1093/mnras/stab3034Proyecto
info:eu-repo/grantAgreement/EC/H2020/717001/EU//DELPHI; Gobierno de España. AYA2015-63810-P; Gobierno de España. PGC2018-094975-C21Versión del editor
https://doi.org/10.1093/mnras/stab3034Materias
Methods: Numerical; Galaxy: Evolution; Galaxies: High-Redshift; Galaxies: Star Formation; Galaxies: Stellar Content; Dark Ages, Reionization; First Stars; FísicaNota
This is a pre-copyedited, author-produced PDF of an article accepted for publication in Monthly Notices of the Royal Astronomical Society following peer review. The version of record Monthly Notices of the Royal Astronomical Society 509.1 (2022): 595-613 is available online at: https://academic.oup.com/mnras/article-abstract/509/1/595/6409841?redirectedFrom=fulltext#no-access-messageDerechos
© 2021 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical SocietyResumen
We use the astraeus framework, that couples an N-body simulation with a semi-analytic model for galaxy formation and a semi-numerical model for reionization, to quantify the star formation histories (SFHs) of galaxies in the first billion years. Exploring four models of radiative feedback, we fit the SFH of each galaxy at 𝑧 > 5 as log(SFR(𝑧)) = −𝛼(1 + 𝑧) + 𝛽; star formation is deemed stochastic if it deviates from this fit by more than ΔSFR = 0.6 dex. Our key findings are: (i) The fraction of stellar mass formed and time spent in the stochastic phase decrease with increasing stellar mass and redshift 𝑧. While galaxies with stellar masses of 𝑀★ ∼ 107M at 𝑧 ∼ 5 (10) form ∼ 70% (20%) of their stellar mass in the stochastic phase, this reduces to < 10% at all redshifts for galaxies with 𝑀★ > 1010M ; (ii) the fractional mass assembled and lifetime spent in the stochastic phase do not significantly change with the radiative feedback model used; (iii) at all redshifts, 𝛼 increases (decreases for the strongest radiative feedback model) with stellar mass for galaxies with 𝑀★ <∼ 108.5M and converges to ∼ 0.18 for more massive galaxies; 𝛽 always increases with stellar mass. Our proposed fits can reliably recover the stellar masses and mass-to-light ratios
for galaxies with 𝑀★ ∼ 108−10.5M and MUV ∼ −17 to − 23 at 𝑧 ∼ 5 − 9. This physical model can therefore be used to derive the SFHs for galaxies observed by a number of forthcoming instruments
Lista de ficheros
Google Scholar:Legrand, Laurent
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Hutter, Anne
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Dayal, Pratika
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Ucci, Graziano
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Gottlöber, Stefan
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Yepes Alonso, Gustavo
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