Fig. A.5.
Modelled and observed RGB stars metallicity distributions. We compare the metallicity distributions of the RGB stars from the best-model CMD for tests A, B, and C (blue, red, and green) with that presented in Kirby et al. (2017) determined through the spectroscopic analysis of individual stars (black, 113 stars). The distributions are built as the sum of individual Gaussians for each star.
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