Fig. 2.

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Comparison of the iron share from simulations and observational data by Renzini & Andreon (2014) (black crosses and solid line with the grey shaded area) and Ghizzardi et al. (2021) (black open circles and dashed shaded area). The two simulation estimates of the iron share are derived by either computing directly the iron mass within stars (as in Fig. 1; large blue asterisks; “sim”) or by converting the stellar mass into iron mass assuming solar abundance, similarly to observations (Eq. (3); small cyan triangles; “obs-like”).
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