Fig. 7.
NLTE abundances as a function of Teff for all cluster stars. The average is shown for all elements. The scatter in [Mg/Fe] is much larger than in [Fe/H] and [Ti/Fe], and it is typically attributed to multiple episodes of star formation and self-enrichment (see the recent review by Bastian & Lardo 2018, and references therein). See Sect. 3.2.4 for details.
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