  Models of the Solar System's dynamical evolution predict the dispersal of
primitive planetesimals from their formative regions amongst the gas-giant
planets due to the early phases of planetary migration. Consequently,
carbonaceous objects were scattered both into the outer asteroid belt and out
to the Kuiper Belt. These models predict that the Kuiper Belt should contain a
small fraction of objects with carbonaceous surfaces, though to date, all
reported visible reflectance spectra of small Kuiper Belt Objects (KBOs) are
linear and featureless. We report the unusual reflectance spectrum of a small
KBO, (120216) 2004 EW95, exhibiting a large drop in its near-UV reflectance and
a broad shallow optical absorption feature centered at ~700 nm which is
detected at greater than 4-sigma significance. These features, confirmed
through multiple epochs of spectral photometry and spectroscopy, have
respectively been associated with ferric oxides and phyllosilicates. The
spectrum bears striking resemblance to those of some C-type asteroids,
suggesting that 2004 EW95 may share a common origin with those objects. 2004
EW95 orbits the Sun in a stable mean motion resonance with Neptune, at
relatively high eccentricity and inclination, suggesting it may have been
emplaced there by some past dynamical instability. These results appear
consistent with the aforementioned model predictions and are the first to show
a reliably confirmed detection of silicate material on a small KBO.
