Zn-to-iron essentially solar, whereas our sample includes stars with low Zn-to-iron. The metallicity limits for the thick disk often give \[Fe/H\]=$-$0.3 as an upper limit; however, Bensby et al. classify some of their more metal-rich stars as probable thick-disk members, based on kinematics, as explained above, and they tend to be younger than $\simless$ 8 Gyr. Comments on the Bensby et al. sample consisting of dwarfs are given below in Sect. 4.3.

In the metallicity range occupied by the old thick disk stars, the bulge appears compatible with the thick disk abundances for the samples from Bensby et al. (2014), Mishenina et al. (2011), Prochaska et al. (2000), and Reddy et al. (2006). A distinction between the present data and thick disk stars may be present for the metal-rich stars, where most stars in the present sample show Zn under-abundances, and the Bensby et al. data show \[Zn/Fe\]$\sim$0.0. It is important to note that there are not as many such old metal-rich stars in the thick disk population studied by Bensby et al. (2013).

Comparison with thin disk Zn abundances
---------------------------------------

In Fig. \[plotzn3\] we compare the present Zn abundances with those for thin disk stars derived by Bensby et 