Fig. 11
Present day abundance gradients from H to Ni: models vs. observations. Observations are from H-II regions (Rudolph et al. 2006), B-stars (Daflon & Cunha 2004), Planetary nebulae (Henry et al. 2004) and Cepheids (Luck & Lambert 2011; Luck et al. 2011; Lemasle et al. 2013). Model results are obtained with the model described here and three different sets of yields, from Nomoto et al. (2013), Woosley & Weaver (1995) and Chieffi & Limongi (2004), as indicated by the open symbols and discussed in the text.
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