The origin and evolution of the odd-Z iron-peak elements Sc, V, Mn, and
  Co in the Milky Way stellar disk
  AIMS: The aim of this study is to investigate the origin and evolution of Sc,
V, Mn, and Co for a homogeneous and statistically significant sample of stars
probing the different populations of the Milky Way, in particular the thin and
thick disks. METHODS: Using high-resolution spectra obtained with MIKE, FEROS,
SOFIN, FIES, UVES and HARPS spectrographs, we determine Sc, V, Mn, and Co
abundances for a large sample of F and G dwarfs in Solar neighbourhood. The
method is based on spectral synthesis and using one-dimensional (1-D),
plane-parallel, LTE model stellar atmospheres calculated with the MARCS 2012
code. NLTE corrections from literature were applied to Mn and Co. RESULTS: We
find that the abundance trends derived for Sc (594 stars), V (466 stars), and
Co (567 stars) are very similar to what has been observed for the
alpha-elements in the thin and thick disks. On the contrary Mn (569 stars) is
generally underabundant relative to the Sun (i.e. [Mn/Fe]<0) for [Fe/H]<0.
Also, for Mn, when NLTE corrections are applied, the trend changes and is
almost flat over the entire metallicity range that the stars in our sample span
(-2<[Fe/H]<+0.4). The [Sc/Fe]-[Fe/H] abundance trends show a small separation
between the thin and thick disks, while for V and Co they completely overlap.
For Mn there is a small difference in [Mn/Fe] but only when NLTE corrections
are used. Comparisons with Ti as a reference element show flat trends for all
the elements except for Mn that show well separated [Mn/Ti]-[Ti/H] trends for
the thin and thick disks. CONCLUSIONS: Sc and V present trends compatible with
production from SNII events. In addition, Sc clearly shows a metallicity
dependence for [Fe/H]<-1. Mn instead is produced in SNII events for [Fe/H]<-0.4
and then SNIa start to produce Mn. Finally, Co appears to be produced mainly in
SNII with suggestion of enrichment from hypernovae at low metallicities.
