Journal article
Semi-analytic modelling of Pop. III star formation and metallicity evolution – I. Impact on the UV luminosity functions at z = 9–16
EM Ventura, Y Qin, S Balu, JBS Wyithe
Monthly Notices of the Royal Astronomical Society | Published : 2024
Abstract
We implemented Population III (Pop. III) star formation in mini-haloes within the MERAXES semi-analytic galaxy formation and reionization model, run on top of a N-body simulation with L = 10 h−1 cMpc with 20483 particles resolving all dark matter haloes down to the mini-haloes (∼105 M☉). 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. Hence, the majority of the first galaxies are likely enriched by their own star formation. However, as reionization progresses, the feedback effects..
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Grants
Awarded by Australian Government
Funding Acknowledgements
We thank the anonymous referee for their insightful comments which helped us improve this work. This research was supported by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D, project #CE170100013). This work was performed on the OzSTAR national facility at Swinburne University of Technology. OzSTAR is funded by Swinburne University of Technology and the National Collaborative Research Infrastructure Strategy (NCRIS). This research was also undertaken with the assistance of resources from the National Computational Infrastructure (NCI Australia), an NCRIS enabled capability supported by the Australian Government. Finally, we thank D. Schaerer for sharing with us the Pop. III SEDs and for the insightful discussions.