the halo and thick disk stars from Nissen & Schuster (2011). Bensby et al. (2013, 2014) and Allende-Prieto et al. (2004) used the 4810.5 and 6362.2 [Å]{} lines, and Nissen & Schuster (2011) used the 4722.1 and 4810.5 [Å]{} lines. (Pompéia (2003) does not report the lines used.)

The lines used are, in most cases, shared with the present work. The dwarfs are all hotter than the present sample, such that their samples have spectra with essentially no molecular lines. This could explain any difference in abundances from the 6362.2 [Å]{} line, that has a blend with CN lines affecting our determinations. On the other hand, the 4810.5 [Å]{} line has no molecular lines, and it shows the same Zn deficiencies as the 6362.2 [Å]{} line for many of the most metal-rich giant stars, but differently from the dwarfs.

The differences for metal-rich stars could stem from other blends, possibly unknown. At present we cannot identify a reason not to confirm the Zn-under-abundance in some of the present sample of metal-rich bulge giants. The flat or decreasing \[Zn/Fe\] at high metallicities has the important consequence of indicating (or not) the contribution of SNIa (see Sect. 4.5).

Comparison with damped Lyman-$\alpha$ 