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.
Left: Scatter diagram of the corrected A(C) vs. [Fe/H] from Yoon et al. . The blue and red open circles represent the 147 CEMP-s/rs stars and 127 CEMP-no stars, respectively. The black diagonal line identifies a carbon-to-metal ratio: [C/Fe] = 0.7. Right: Joint PDF depicting the mass-weighted probabilities, per Mpc3, for A(C) vs. [Fe/H] for all the stars in my simulation. Red stars are a super-set of CEMP-no stars plotted at left. The PDF correlates well with bimodal pattern of CEMP-no (red) stars analyzed by Yoon et al. .
-- A(C) = log (NC/NH) + 12, is the Carbon abundance where A(C)⊙ = 8.43