elements is their abundance derivation in different stellar populations. In the present work, we derive Zn abundances for a sample of 56 bulge field stars, observed at high resolution with the FLAMES-UVES spectrograph (Lecureur et al. 2007; Zoccali et al. 2006; Hill et al. 2011), where we adopt the stellar parameters effective temperature T$_{\rm eff}$, gravity log g, metallicity \[Fe/H\][^2], and microturbulence velocity from these previous determinations.

We compare our results with previous Zn abundance determinations for bulge, disk, and halo stars from the literature. Bensby et al. (2013, and references therein) derived Zn for microlensed bulge dwarfs. Prochaska et al. (2000), Reddy et al. (2006), Nissen & Schuster (2011), and Bensby et al. (2014) derived Zn abundances for thick disk stars. A comparison with thin disk abundances is also given, based on work by Allende-Prieto et al. (2004), Bensby et al. (2014), and Pompéia (2003).

We also compare the present results to literature abundances for damped Lyman-alpha systems, where Zn is considered as a proxy for Fe. We included comparisons with analyses by Akerman et al. (2005), Cooke et al. (2011, 2013), Kulkarni et al. (2007), and Vladilo et al. (2011).

Finally, we also present a model of Zn 