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Fig. 13

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Filled circles indicate the width σ[ Fe / H ] of the stellar metallicity distribution in Galactic GCs plotted vs. their absolute visual magnitude MV, compiled from Willman & Strader (2012) and da Costa et al. (2014). The blue curve indicates the width σ[ Fe / H ] predicted from the best-fitting self enrichment model of the Centaurus cluster GCs, the red (dashed) curve represents the predictions from the best-fit model of the Hydra cluster GCs. The bold curves correspond to average primordial rh = 1 pc, the finer ones to rh = 1.5 pc.

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