Fig. 10
Observed abundance ratios in our RR Lyr stars from Table 4 (symbols as in Fig. 5) vs. predicted yields for models of super- and hypernovae (HN) by: Limongi et al. (2000) (full black line), Kobayashi et al. (2006) (dotted: SN; dashed: HN), Tominaga et al. (2007) (dot-dashed and triple-dot-dashed: 20 and 40 M⊙ HN; long-dashed: 13 M⊙ SN) and Izutani et al. (2009) 25 M⊙ HN; thick blue solid line.
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