  We present the observational results of a survey designed to target and
detect asteroids whose colors are similar to those of Vesta family members and
thus may be considered as candidates for having a basaltic composition. Fifty
basaltic candidates were selected with orbital elements that lie outside of the
Vesta dynamical family. Optical and near-infrared spectra were used to assign a
taxonomic type to 11 of the 50 candidates. Ten of these were spectroscopically
confirmed as V-type asteroids, suggesting that most of the candidates are
basaltic and can be used to constrain the distribution of basaltic material in
the Main Belt.
  Using our catalog of V-type candidates and the success rate of the survey, we
calculate unbiased size-frequency and semi-major axis distributions of V-type
asteroids. These distributions, in addition to an estimate for the total mass
of basaltic material, suggest that Vesta was the predominant contributor to the
basaltic asteroid inventory of the Main Belt, however scattered planetesimals
from the inner Solar System (a < 2.0 AU) and other partially/fully
differentiated bodies likely contributed to this inventory. In particular, we
infer the presence of basaltic fragments in the vicinity of asteroid 15
Eunomia, which may be derived from a differentiated parent body in the middle
Main Belt (2.5 < a < 2.8). We find no asteroidal evidence for a large number of
previously undiscovered basaltic asteroids, which agrees with previous theories
suggesting that basaltic fragments from the ~100 differentiated parent bodies
represented in meteorite collections have been "battered to bits" [Burbine,
T.H., Meibom, A., Binzel, R.P., 1996. Mantle material in the Main Belt:
Battered to bits? Met. & Planet. Sci. 31, 607].
