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We implemented Population III (Pop. III) star formation in mini-halos withinthe MERAXES semi-analytic galaxy formation and reionisation model, run on topof a N-body simulation with $L = 10 h^{-1}$ cMpc with 2048$^3$ particlesresolving 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 releasedthrough supernova-driven bubbles that expand according to the Sedov-Taylormodel. We found that SN-driven metal bubbles are generally small, with radiitypically of 150 ckpc at z = 6. Hence, the majority of the first galaxies arelikely enriched by their own star formation. However, as reionizationprogresses, the feedback effects from the UV background become more pronounced,leading to a halt in star formation in low-mass galaxies, after which externalchemical enrichment becomes more relevant. We explore the sensitivity of thestar formation rate density and stellar mass functions on the unknown values offree parameters. We also discuss the observability of Pop. III dominatedsystems with JWST, finding that the inclusion of Pop. III galaxies can have asignificant effect on the total UV luminosity function at z = 12 - 16. Ourresults support the idea that the excess of bright galaxies detected with JWSTmight be explained by the presence of bright top-heavy Pop. III dominatedgalaxies without requiring an increased star formation efficiency.

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