  In recent years several small basaltic V-type asteroids have been identified
all around the main belt. Most of them are members of the Vesta dynamical
family, but an increasingly large number appear to have no link with it. The
question that arises is whether all these basaltic objects do indeed come from
Vesta. To find the answer to the above questioning, we decided to perform a
statistical analysis of the spectroscopic and mineralogical properties of a
large sample of V-types, with the objective to highlight similarities and
differences among them, and shed light on their unique, or not, origin. The
analysis was performed using 190 visible and near-infrared spectra from the
literature for 117 V-type asteroids. The asteroids were grouped according to
their dynamical properties and their computed spectral parameters compared.
Comparison was also performed with spectral parameters of a sample of HED
meteorites and data of the surface of Vesta taken by the VIR instrument on
board of the Dawn spacecraft. Our analysis shows that although most of the
V-type asteroids in the inner main belt do have a surface composition
compatible with an origin from Vesta, this seem not to be the case for V-types
in the middle and outer main belt.
