  We present near-infrared (0.78-2.45 {\mu}m) reflectance spectra for nine
middle and outer main belt (a > 2.5 AU) basaltic asteroids. Three of these
objects are spectrally distinct from all classifications in the Bus-DeMeo
system and could represent spectral end members in the existing taxonomy or be
representatives of a new spectral type. The remainder of the sample are
classified as V- or R- type. All of these asteroids are dynamically detached
from the Vesta collisional family, but are too small to be intact
differentiated parent bodies, implying that they originated from differentiated
planetesimals which have since been destroyed or ejected from the solar system.
The 1- and 2-{\mu}m band centers of all objects, determined using the Modified
Gaussian Model (MGM), were compared to those of 47 Vestoids and fifteen HED
meteorites of known composition. The HEDs enabled us to determine formulas
relating Band 1 and Band 2 centers to pyroxene ferrosilite (Fs) compositions.
Using these formulas we present the most comprehensive compositional analysis
to date of middle and outer belt basaltic asteroids. We also conduct a careful
error analysis of the MGM-derived band centers for implementation in future
analyses. The six outer belt V- and R-type asteroids show more dispersion in
parameter space than the Vestoids, reflecting greater compositional diversity
than Vesta and its associated bodies. The objects analyzed have Fs numbers
which are, on average, between five and ten molar percent lower than those of
the Vestoids; however, identification and compositional analysis of additional
outer belt basaltic asteroids would help to confirm or refute this result.
Given the gradient in oxidation state which existed within the solar nebula,
these results tentatively suggest that these objects formed at either a
different time or location than 4 Vesta.
