Semi-analytic modelling of Pop. III star formation and metallicity evolution -- I. Impact on the UV luminosity functions at z = 9-16

Understand

We implemented Population III (Pop.

• III) star formation in mini-halos within the MERAXES semi-analytic galaxy formation and reionisation model, run on top of a N-body simulation with $L = 10 h^{-1}$ cMpc with 2048$^3$ particles resolving all dark matter halos down to the mini-halos ($\sim 10^5 M_\odot$).
• Our modelling includes the chemical evolution of the IGM, with metals released through supernova-driven bubbles that expand according to the Sedov-Taylor model.
• We found that SN-driven metal bubbles are generally small, with radii typically of 150 ckpc at z = 6.