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Fig. 5
Ca abundances from the same sources as in Fig. 3, with Fe and Ca values for the Hercules UFD taken from A11. The red lines are chemical evolution models for Hercules (Lanfranchi & Matteucci 2004; Koch et al. 2012b), assuming star-forming efficiencies ν of (top to bottom) 0.1, 0.01, 0.001, and 0.0001 Gyr-1.
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