where different symbols represent the four different fields, and the red clump stars. In Fig. \[plotzn\]a, we overplotted the Zn abundances of dwarf bulge stars observed thanks to microlensing magnification, by Bensby et al. (2013). There is good agreement between the present results and those by Bensby et al. at metallicities $-$1.4 $<$ \[Fe/H\] $<$ 0.0. On the other hand, for our metal-rich giants with \[Fe/H\] $>$ 0.0, we find a wide spread of $-$0.6 $<$ \[Zn/Fe\] $<$ +0.15 and a decreasing trend with metallicity. Further comments on the Bensby et al. sample of dwarf bulge stars are given in Sect. 4.3. In Fig. \[plotzn\]b we show the same stars as in Fig. \[plotzn\]a, adding metal-poor halo stars analysed by Cayrel et al. (2004) and halo and thick disk stars results from Ishigaki et al. (2013) and Nissen & Schuster (2011). Ishigaki et al. results seem to show lower \[Zn/Fe\] in the -3.0 $<$ \[Fe/H $<$ $-$1.0 metallicity range with respect to the Nissen & Schuster and Cayrel et al. results.

Comparison with thick disk Zn abundances
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In Fig. \[plotzn1\] we compare the present bulge Zn abundances with those for thick disk stars in the literature. The results by 