Papers › AstraeusIV : Quantifying the star formation histories of galaxies in the Epoch of Reionization
AstraeusIV : Quantifying the star formation histories of galaxies in the Epoch of Reionization
Laurent Legrand, Anne Hutter, Pratika Dayal, Graziano Ucci, Stefan Gottlöber, Gustavo Yepes
The archive published only this paper's code-link row. Authors, date and abstract are from arXiv's metadata (CC0), read from the Kaggle arXiv metadata snapshot of 2026-09-12 where its title matched the archive's; the title is the archive's.
We use the \textsc{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 Δ_(SFR)=0.6dex. 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_⋆≲10^(8.5)M_⊙ 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_⋆∼10^(8-10.5)M_⊙ and M_(UV)∼-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.
Code
Repository list and official/mentioned flags are the archive's, frozen 2025-07-28. Reachability, where shown, is from one Syntology probe window (2026-09-16 to 2026-09-18); repositories not probed show nothing. GitHub stars are not tracked.
Code Syntology ran Syntology
Not run by Syntology. Nothing on this page verifies that the listed code works.
Results from the paper archive 2025-07-28
No leaderboard rows for this paper in the archive.
Report a problem or propose a change · a person checks every report against the paper or source before anything changes; decisions are listed on /corrections