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Chemical tagging is a powerful tool to reveal the origin of stars andglobular clusters (GCs), especially when dynamics alone cannot provide robustanswers. So far, mostly $\alpha$- and neutron capture elements have been usedto distinguish stars born in the Milky Way (MW) from those born in externalenvironments such as that of dwarf galaxies. Here, instead, we use iron-peakelements abundances to investigate the origin of a sample of metal-richglobular clusters. By homogeneously analyzing high-resolution UVES spectra ofgiant stars belonging to four metal-rich GCs (namely NGC 5927, NGC 6388, NGC6441, NGC 6496), we find that while the $\alpha$-elements Si and Ca havesimilar abundance ratios for all the four GCs, and Ti and neutron captureelements (La, Ba and Eu) only show a marginal discrepancy, a stark differenceis found when considering the abundances of some iron-peak elements (Sc, V andZn). In particular, NGC 6388 and NGC 6441 have abundance ratios for theseiron-peak elements significantly lower (by ~ 0.5 dex) than those measured inNGC 5927 and NGC 6496, which are clearly identified as born in-situ MW clustersthrough an analysis of their orbital properties. These measurements indicatethat the environment in which these clusters formed is different, and providerobust evidence supporting an accreted origin from the same progenitor for NGC6388 and NGC 6441.

A new set of chisels for Galactic archaeology: Sc, V and Zn as taggers of accreted globular clusters