[O/Fe] vs. [Fe/H] for the present results together with literature abundances for and bulge and thick disk stars and the predictions of the chemodynamical model for the bulge. Panel a): the data derived for the sample bulge giant stars are compared with the results for bulge giants from Cunha & Smith (2006) and Ryde et al. (2010). The lines are the predictions of the model assumig a specific star formation rate of ν_SF = 3 Gyr^-1. Panel b): same data as in panel a) and the predicted O/Fe] vs. [Fe/H] for the model with no hypernovae. The dot-dashed line is the prediction by the model with hypernovae for r< 0.5 kpc; panel c): the [O/Fe] vs. [Fe/H] of the thick disk dwarfs from Bensby et al. (2004), thick disk giants from Alves-Brito et al. (2010) are superposed on the model predictions of panel a).