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Fig. 10


[X/Fe] versus [Fe/H] for SFRs with known high-resolution abundances. The references are Biazzo et al. (2011; B11), D’Orazi et al. (2011; D11), Santos et al. (2008; S08), King et al. (2000; K00), and González-Hernández et al. (2008; GH08). The errors in [Fe/H] are around 0.02−0.12 dex. The dashed lines mark the solar abundances. The filled dots in the background represent the [X/Fe] distribution of nearby field stars in the Galactic thin disk (Soubiran & Girard 2005).

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