Speaker
Description
We perform a cosmological simulation with a comoving volume of 1 Mpc$^{3}$ to study the birthplaces of Population III stars, using the adaptive mesh refinement code Enzo. We investigate the distribution of host halo masses and its relationship to the Lyman-Werner background intensity. In our sample of 697 host halos, we find that 84% of them have masses below the Machecek et al. (2001) relation because of the inclusion of H2 self-shielding. In our simulation above a redshift of 12.5, the mean halo mass is time-independent and ~10$^{5.8}$ solar masses. Afterwards, it steadily rises above the Machacek et al. relation to a mean value of ~10$^{6.6}$ solar masses. Most of these halos form multiple Population III stars, with a median number of four, up to a maximum of 16. We also find that a few halos do form stars below the Machacek et al. relation but in a high Lyman-Werner radiation field with values up to ~50 J$_{21}$. Our results suggest that Population III star formation may be less affected by Lyman-Werner radiation feedback than previously thought and that Population III multiple systems are common
Affiliation
Georgia Institute of Technology
| Talk/Poster | Poster |
|---|
