  The majority of basaltic objects in the main belt are dynamically connected
to Vesta, the largest differentiated asteroid known. Others, due to their
current orbital parameters, cannot be easily dynamically linked to Vesta. This
is particularly true for all the basaltic asteroids located beyond 2.5 au,
where lies the 3:1 mean motion resonance with Jupiter. In order to investigate
the presence of other V-type asteroids in the middle and outer main belt (MOVs)
we started an observational campaign to spectroscopically characterize in the
visible range MOV candidates. We observed 18 basaltic candidates from TNG and
ESO - NTT between 2015 and 2016. We derived spectral parameters using the same
approach adopted in our recent statistical analysis and we compared our data
with orbital parameters to look for possible clusters of MOVs in the main belt,
symptomatic for a new basaltic family. Our analysis seemed to point out that
MOVs show different spectral parameters respect to other basaltic bodies in the
main belt, which could account for a diverse mineralogy than Vesta; moreover,
some of them belong to the Eos family, suggesting the possibility of another
basaltic progenitor. This could have strong repercussions on the temperature
gradient present in the early Solar System, and on our current understanding of
differentiation processes.
