Our probability density functions (PDFs) correlate well with the observations of CEMP stars from Keller et al. (2014) (red stars).
Our simulation tracks the pristine fraction of gas at subgrid scales to better model the formation of Pop III stars in the early universe.
We demonstrate that a large number of stars can still form in regions of otherwise polluted gas due to incomplete mixing.
Joint PDFs depicting the mass-weighted probabilities for the chemical abundances of [C/H], [O/H] and [Mg/Ca] as a function of [Fe/H] for all stars in our simulation. We generate chemical abundances for our stars convolving models for Pop III SN and "regular" SN. The red stars are characteristics of observed Milky Way halo CEMP-no stars (Keller et al. 2014). Our metallicity density function at the lower left is overlayed with data (red curves with 1 sigma Poisson noise) from Yoon et al. 2016 and An et al. 2013.