The left frame depicts the evolution of the density field for a 16 Mpc on-a-side simulation. Galaxies are forming throughout the box and are indicated by lighter colors/white.
The right frame depicts the pollution of the gas by supernova.
Observational data is limited at redshift 10 and completely lacking at higher redshifts. However, using our simulation, we makes predictions for the number of detectable (by JWST) galaxies as a function of brightness out to z=12. These will be some of the faintest objects detectable (without lensing).
Our simulation tracks the pristine fraction of gas at subgrid scales to better model the formation of Pop III stars in the early universe.
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