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Fig. 4


[S/Fe] vs. iron content for the clusters with known S abundance. NGC 6397 from Koch & Caffau (2011); NGC 6752 and 47 Tuc from Sbordone et al. (2009); Terzan 7 from Caffau et al. (2005b). The results of M 4 and Trumpler 5, based on Mult. 1, are discussed in this paper. The analysis of NGC 5822 and NGC 2477 are based on the lines of Mult. 8. For comparison we plot sulphur abundances in Galactic stars. “LP stars” is an average in metallicity and [S/Fe] for the stars with [Fe/H] < −2.9 from Spite et al. (2011), from Mult. 1; the metal-poor sample from Jönsson et al. (2011) (blue open circles) based on Mult. 3, and from the forbidden [SI] line at 108.2 nm line; the solar-metallicity sample of comparison stars from Ecuvillon et al. (2004) (red filled squares) where Mult. 8 has been analysed. All the points have been scaled to our adopted solar abundances A(S) = 7.16 and A(Fe) = 7.52 (Caffau et al. 2011).

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