Nissen & Schuster (2011) are maintained in all panels in Fig. \[plotzn1\], showing good agreement with other samples of thick disk stars. Given the narrow spread and the metallicity range covered by these data, we adopted the Nissen & Schuster (2011) results as a reference for the thick disk. Panels a, b, c, d show the Zn abundances derived respectively by Bensby et al. (2014), Mishenina et al. (2011), Prochaska et al. (2000), and Reddy et al. (2006). All thick disk samples show very good agreement with the present data, in the metallicity range of thick disk stars (-1.2 $\simless$ \[Fe/H\] $\simless$ 0.0). The Bensby et al. (2014) thick disk stars were selected based on kinematical criteria TD/D $>$ 2, with these numbers corresponding to a probability defined in Bensby et al. (2003). Thick disk stars from Bensby et al. (2014) displayed in Fig. \[plotzn1\]a include an old metal-poor thick disk, whereas the more metal-rich thick disk stars are younger ($<$8Gyr). The Bensby et al. old metal-poor thick disk stars, reaching down to \[Fe/H\]$\approx$-2.0, show a moderate enhancement of \[Zn/Fe\]$\approx$+0.15, compatible with our results for the metal-poor bulge stars. Their more metal-rich thick disk component with \[Fe/H\] $>$ $-$0.3 show 