enrichment in massive spheroid systems, which is based on the code described in Lanfranchi & Friaça (2003). It would represent the early bulge enrichment and its chemical evolution.

In Sect. 2 the observations are summarized and the adopted atomic constants and solar abundances given. In Sect. 3 the basic stellar parameters are listed, and the abundance derivation of Zn is described. The results are compared with literature data and discussed in Sect. 4. A summary is given in Sect. 5.

Observations, atomic line parameters, and solar abundances
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The present UVES data were obtained using the UVES-FLAMES instrument at the 8.2 m Kueyen ESO telescope, as described in Zoccali et al. (2006), Lecureur et al. (2007), and Hill et al. (2011). The spectra cover the wavelength range 4800-6800 [Å]{} with a resolution of R $\sim$ 45 000 and a pixel scale of 0.0147 [Å]{}/pix. Targets are bulge K giants, with magnitudes $\sim$0.5 above the red clump, in four fields, including Baade’s Window. Zinc lines were checked against oscillator strengths log gf in the literature, using in particular the data bases from Kurúcz (1995) website[^3], NIST[^4], and VALD (Piskunov et al. 1995). Table \[lines2\] reports excitation potential, log gf values from 