Our fluorine abundances compared with the predictions of our bulge models including AGB stars, excluding and including the ν-process with two different energies, and excluding W-R stars. The abundances have been transformed to the scale of the models with log ϵ(F)_⊙ = 4.56 and log ϵ(O)_⊙ = 8.93 (Anders & Grevesse 1989). The stars are color-coded as the corresponding fields in Fig. 1 with the BW-stars of Cunha et al. (2008) added in the right panel in light green. Conservative estimates of the uncertainties are marked in the upper left-hand corners. We note that the star BMB-78, still after the re-analysis, falls below the rest of the trend; see Sect. 5 for possible explanations.