[Å]{}. We considered the strong depression in the continuum of the 6362.34 [Å]{} line, which is caused by the wings of the 6361.79 [Å]{} line suffering from autoionization. CN lines blending the 6362.34 [Å]{} line are also included in the calculations. ]{} [We find \[Zn/Fe\]=+0.24$\pm$0.02 in the range $-$1.3 $<$ \[Fe/H\] $<$ $-$0.5 and \[Zn/Fe\]=+0.06$\pm$0.02 in the range $-$0.5 $<$ \[Fe/H\] $<$ $-$0.1, whereas for \[Fe/H\]$\geq$ $-$0.1, it shows a spread of $-$0.60 $<$ \[Zn/Fe\] $<$ +0.15, with most of these stars having low \[Zn/Fe\]$<$0.0. These low zinc abundances at the high metallicity end of the bulge define a decreasing trend in \[Zn/Fe\] with increasing metallicities. A comparison with Zn abundances in DLA systems is presented, where a dust-depletion correction was applied for both Zn and Fe. When we take these corrections into account, the \[Zn/Fe\] vs. \[Fe/H\] of the DLAs fall in the same region as the thick disk and bulge stars. Finally, we present a chemical evolution model of Zn enrichment in massive spheroids, representing a typical classical bulge evolution.]{}

Introduction
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Zinc is an interesting element to study because it can be observed in damped Lyman-$\alpha$ systems (DLAs), where it is assumed as a proxy for Fe 