Context : Elements heavier than Li are produced in the interiors of stars .
However , for many elements the exact production sites and the timescales on which they are dispersed into the interstellar medium are unknown .
Having a clear picture on the origins of the elements is important for our ability to trace and understand the formation and chemical evolution of the Milky Way and its stellar populations .

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 the 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 the solar neighborhood .
The method is based on spectral synthesis and using one-dimensional , plane-parallel , local thermodynamic equilibrium ( LTE ) model stellar atmospheres calculated with the MARCS 2012 code .
The non-LTE ( NLTE ) corrections from the 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 .
In addition , for Mn , when NLTE corrections are applied , the trend changes and is almost flat over the entire metallicity range of the stars in our sample ( -2 \lesssim [ Fe / H ] \lesssim + 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 : The elements Sc and V present trends compatible with production from type II supernovae ( SNII ) events .
In addition , Sc clearly shows a metallicity dependence for [ Fe/H ] ¡ - 1 .
Instead , Mn is produced in SNII events for [ Fe / H ] \lesssim - 0.4 and then type Ia supernovae start to produce Mn .
Finally , Co appears to be produced mainly in SNII with suggestion of enrichment from hypernovae at low metallicities .