Key points are not available for this paper at this time.
Carbon abundances, especially at low metallicity, reveal the early chemical evolution of a system, tracing the supernovae (SNe) that contributed and how much of their ejecta made it into the next stellar generation. Our sample from the Pristine Inner Galaxy Survey (PIGS) includes 350 metal-poor (Fe/H~+0. 7) as in the Galaxy under-predicts the number of CEMP stars in DGs, and for Sgr a cut at C/Fe~ +0. 35 may be more appropriate, which brings the frequency of CEMP stars in agreement with that in the Galaxy.
Sestito et al. (Wed,) studied this question.
Synapse has enriched 5 closely related papers on similar clinical questions. Consider them for comparative context: