POLAR

Context. Galaxies may suffer some starburst and quenched periods in their history due to galaxy mergers and feedback. However, semi-numerical simulations of the Epoch of Reionization (EoR) do not accurately model the effects of the star formation history (SFH) of galaxies. Aims. Keeping the same total ionizing photon budget from galaxies, we investigate how the ionization and heating of the intergalactic medium (IGM), as well as the associated 21 cm signal during the EoR, depend on the variations in modeling the SFH of galaxies. Methods. We adopted the J<ns0:sc>IUTIAN</ns0:sc>-300 N-body dark matter simulation and the semi-analytic model L-G<ns0:sc>ALAXIES</ns0:sc> 2020 to model galaxy formation. Using the galaxy catalog from L-G<ns0:sc>ALAXIES</ns0:sc> 2020 as input, we post-processed the J<ns0:sc>IUTIAN</ns0:sc>-300 density field with the 1D radiative transfer code G<ns0:sc>RIZZLY</ns0:sc> to model the reionization process and the 21 cm signal. Results. We find that the ionized regions produced by galaxies with a SFH derived from L-G<ns0:sc>ALAXIES</ns0:sc> 2020 are slightly larger and warmer than the ones obtained with a constant star formation rate. For a fixed stellar mass, galaxies produce smaller ionized regions with increasing stellar-mass-weighted stellar age τage. This results in a different topology and timing of the IGM ionization and heating obtained from G<ns0:sc>RIZZLY</ns0:sc>. Conclusions. The SFH of galaxies is highly dependent on τage and redshift. Different models of the galactic SFH affect the gas heating and ionizing processes during the EoR and, as a consequence, also affect the 21 cm global signal and power spectrum.