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Fig. 4


[X/Fe] for the observed giants in red, compared to abundances of the 604 solar neighborhood dwarf stars of Bensby et al. (2014) with Teff> 5400 K in gray. Especially for O and Ti a clear separation of thin and thick disk-type abundances can be seen in our sample. Since our sample is mostly made up of the very brightest, closest, giants, it is not surprising that a majority of the stars show thin disk-type chemistry. In the plots we use A(O) = 8.69, A(Mg) = 7.60, A(Ca) = 6.34, A(Ti) = 4.95, and A(Fe) = 7.50 (Asplund et al. 2009).

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