Star Formation and Chemical Enrichment in Protoclusters

We study the protocluster’s (PC's) star formation and gas metallicity evolution at \(z=0.6-10\) using the cosmological SPH simulation code GADGET3-Osaka. The total star formation rate in the PC reaches \(3000\ \mathrm{M}_\odot \mathrm{yr}^{-1}\) at \(z=3\), with the core region accounting for about half of the star formation in the PC at \(z\sim2\). For the chemical abundance evolution, we find that the effect of Type II supernova (SN) appears at \(z>3\), while that of Type Ia SN appear at \(z\sim3\) in the core. We also compare the chemical abundance of the gas in individual PC galaxies with observations.