al. (2014), and Allende-Prieto et al. (2004). The data are also compared with the metal-rich dwarf stars from Pompéia (2003). Thick-disk stars by Nissen & Schuster (2011) are also kept in all plots, as a reference for the thick disk. The thin disk Zn abundances from Bensby et al. (2014) are consistent with a mean \[Zn/Fe\]$\sim$0.0, with a fraction of stars showing higher \[Zn/Fe\] up to $\sim$+0.4. The Allende-Prieto et al. (2004) stars show a mean \[Zn/Fe\]$>$0 and a clear and an increasing trend with metallicity. The dwarf stars studied by Pompéia (2003) overlap with the present bulge stars data, except for the more metal-rich ones, which show no under-abundance. This difference may indicate that the Pompéia (2003) sample would be rather old thin disk stars and not bulge-like stars, as concluded in Trevisan et al. (2011) and again discussed in Trevisan & Barbuy (2014).

Inspecting differences with literature samples
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The comparisons with literature data in the previous sections include several samples of dwarf stars: the microlensed dwarf bulge stars from Bensby et al. (2013), the thin and thick disk stars from Bensby et al. (2014), the thin disk stars from Allende-Prieto et al. (2004) and Pompéia (2003), and 