How the First Stars Shaped the First Galaxies

摘要

Radiation from the first stars expel most of the gas from the shallow DM potential wells in which they formed. We use cosmological radiation hydrodynamical AMR simulations that include self-consistent Population III star formation and feedback. Radiative transport is accurately modelled with adaptive ray tracing. We include supernova (SN) explosions and follow the metal enrichment of the intergalactic medium and surrounding star forming halos. We focus on the formation of several dwarf galaxies and their progenitors. Baryon fractions in Tvir = 104 K halos decrease to 10% with stellar feedback and 5% with SN explosions. We find that gaseous spin parameters increase up to a factor of 5 when SN feedback is included.