A Framework to Calibrate a Semi-analytic Model of the First Stars and Galaxies to the Renaissance Simulations

Ryan Hazlett, Mihir Kulkarni, Eli Visbal, John H. Wise

Published 2024-03-08Version 1

We present a method that calibrates a semi-analytic model to the Renaissance Simulations, a suite of cosmological hydrodynamical simulations with high-redshift galaxy formation. This approach combines the strengths of semi-analytic techniques and hydrodynamical simulations, enabling the extension to larger volumes and lower redshifts inaccessible to simulations due to computational expense. Using a sample of Renaissance star formation histories (SFHs) from an average density region of the Universe, we construct a four parameter prescription for metal-enriched star formation characterized by an initial bursty stage followed by a steady stage where stars are formed at constant efficiencies. Our model also includes a treatment of Population III star formation where a minimum halo mass and log-normal distribution of stellar mass are adopted to match the numerical simulations. Star formation is generally well reproduced for halos with masses $\lesssim$$10^{9} M_{\mathrm{\odot}}$. Between $11<z<25$ our model produces metal-enriched star formation rate densities (SFRDs) that typically agree with Renaissance within a factor of $\sim$2 for the average density region. Additionally, the total metal-enriched stellar mass only differs from Renaissance by about $10\%$ at $z \sim 11$. For regions that are either more overdense or rarefied not included in the calibration, we produce metal-enriched SFRDs that agree with Renaissance within a factor of $\sim$2 at high-$z$, but eventually differ by higher factors for later times. This is likely due to environmental dependencies not included in the model. Our star formation prescriptions can easily be adopted in other analytic or semi-analytic works to match our calibration to Renaissance.