  Improving constraints on the abundance of basaltic asteroids in the main
asteroid belt is necessary for better understanding the thermal and collisional
environment in the early solar system, for more rigorously identifying the
genetic family for (4) Vesta, for determining the effectiveness of
Yarkovsky/YORP in dispersing asteroid families, and for better quantifying the
population of basaltic asteroids in the outer main belt (a greater than 2.5 AU)
that are likely unrelated to (4) Vesta.
  NIR spectral observations in this work were obtained for the Vp-type
asteroids (2011) Veteraniya, (5875) Kuga, (8149) Ruff, (9147) Kourakuen, (9553)
Colas, (15237) 1988 RL6, (31414) Rotaryusa, and (32940) 1995 UW4 during August
and September 2014 utilizing the SpeX spectrograph at the NASA Infrared
Telescope Facility (IRTF), Mauna Kea, Hawaii. Spectral band parameter (band
centers, Band Area Ratios) and mineralogical analysis (pyroxene chemistry) for
each average asteroid NIR reflectance spectrum suggests a
howardite-eucrite-diogenite (HED) meteorite analog for each asteroid. (5875)
Kuga is most closely associated with the eucrite meteorites, (31414) Rotaryusa
is most closely associated with the diogenites, and the remaining other six
asteroids are most closely associated with the howardite meteorites. Along with
orbital locations in the inner main belt and in the vicinity of (4) Vesta, the
existing evidence suggests that these eight Vp-type asteroids are also likely
Vestoids.
