  There is a great deal of scientific interest in characterizing the basaltic
asteroids (spectrally classified as V-types), as they are the key to
understanding planetesimal formation and evolution in the early Solar System.
These have long been recognized as parts of the crusts of fully differentiated
planetesimals. Thus, their multiplicity, distribution, and physical
characteristics are crucial for providing context for and constraining the
theoretical evolution models of the Solar System. In this work, we perform
spectral analysis with an extended data set of spectral measurements from the
ESA Gaia mission Data Release 3, thus increasing the sample size of the
analyzed V-types by more than three times as compared to the literature. Using
the data provided by Gaia we identified ~2000 possible V-type asteroids. About
350 of them successfully pass our data validation criteria. This sample
includes 31 new V-type asteroids beyond 2.5 au and 6 in the Phocaea region. We
confirm that the V-type asteroids in the middle and outer part of the main belt
show distinct spectral properties compared to typical vestoids. In the inner
main belt, we found a great diversity of spectral parameters among the V-types
in all populations. Number of asteroids show band depths even greater than that
of (1459) Magnya. Furthermore, some objects present 0.9~\textmu{}m band-centers
more than one standard deviation away from the typical value for vestoids.
However since the DR3 band centers are often overestimated, those findings are
to be confirmed. Overall our results indicate that the inner main belt may
contain remnants of multiple differentiated planetesimals, not just (4) Vesta.
