Abundances of disk and Bulge giants from high-resolution optical spectra
  III. Sc, V, Cr, Mn, Co, Ni
  Context. Recent observations of the Bulge, e.g., its X-shape, cylindrical
stellar motions, and a potential fraction of young stars propose that it formed
through secular evolution of the disk and not through gas dissipation and/or
mergers, as thought previously. Aims. We measure abundances of six iron-peak
elements (Sc, V, Cr, Mn, Co and Ni) in the local thin and thick disks as well
as the Bulge to provide additional observational constraints for Galaxy
formation and chemical evolution models. Methods. We use high-resolution
optical spectra of 291 K giants in the local disk mostly obtained by the FIES
at NOT (signal-to-noise (S/N) ratio of 80-100) and 45 K giants in the Bulge
obtained by the UVES/FLAMES at VLT (S/N ratio of 10-80). We measure abundances
in SME and apply NLTE corrections to the [Mn/Fe] and [Co/Fe] ratios. To
discriminate between the thin and thick, we use stellar metallicity,
[Ti/Fe]-ratios, and kinematics from Gaia DR2 (proper motions and the radial
velocities). Results. The observed disk trend of V is more enhanced in the
thick disk, while the Co disk trend shows a minor enhancement in the thick
disk. The Bulge trends of V and Co appear even more enhanced w.r.t. the thick
disk, but within the uncertainties. The [Ni/Fe] ratio seems slightly
overabundant in the thick disk and the Bulge w.r.t. the thin disk, although the
difference is minor. The disk and Bulge trends of Sc, Cr and Mn overlap
strongly. Conclusions. The somewhat enhanced [(V,Co)/Fe] ratios observed in the
Bulge suggest that the local thick disk and the Bulge might have experienced
different chemical enrichment and evolutionary paths. However, we are unable to
predict the exact evolutionary path of the Bulge solely based on these
observations. Galactic chemical evolution models could, on the other hand,
provide that using these results.
