  Globular clusters are tracers of the history of star formation and chemical
enrichment in the early Galaxy. Their abundance pattern can help understanding
their chemical enrichment processes. In particular, the iron-peak elements have
been relatively little studied so far in the Galactic bulge. The abundances of
iron-peak elements are derived for the sample clusters, and compared with bulge
field, and thick disk stars. We derive abundances of the iron-peak elements Sc,
V, Mn, Cu, and Zn in individual stars of five bulge globular clusters (NGC
6528, NGC 6553, NGC 6522, NGC 6558, HP1), and of the reference thick disk/inner
halo cluster 47 Tucanae (NGC 104). High resolution spectra were obtained with
the UVES spectrograph at the Very Large Telescope over the years. The sample
globular clusters studied span metallicities in the range -1.2<Fe/H]<0.0. V and
Sc appear to vary in lockstep with Fe, indicating that they are produced in the
same supernovae as Fe. We find that Mn is deficient in metal-poor stars,
confirming that it is underproduced in massive stars; Mn-over-Fe steadily
increases at the higher metallicities due to a metallicity-dependent enrichment
by supernovae of type Ia. Cu behaves as a secondary element, indicating its
production in a weak-s process in massive stars. Zn has an alpha-like behaviour
at low metallicities, which can be explained in terms of nucleosynthesis in
hypernovae. At the metal-rich end, Zn decreases with increasing metallicity,
similarly to the alpha-elements.
