  We present a study of the recently discovered compact stellar system
Triangulum II. From observations conducted with the DEIMOS spectrograph on Keck
II, we obtained spectra for 13 member stars that follow the CMD features of
this very faint stellar system and include two bright red giant branch stars.
Tri II has a very negative radial velocity (<v_r>=-383.7^{+3.0}_{-3.3} km/s)
that translates to <v_{r,gsr}> ~ -264 km/s and confirms it is a Milky Way
satellite. We show that, despite the small data set, there is evidence that Tri
II has complex internal kinematics. Its radial velocity dispersion increases
from 4.4^{+2.8}_{-2.0} km/s in the central 2' to 14.1^{+5.8}_{-4.2} km/s
outwards. The velocity dispersion of the full sample is inferred to be
\sigma_{vr}=9.9^{+3.2}_{-2.2} km/s. From the two bright RGB member stars we
measure an average metallicity <[Fe/H]>=-2.6+/-0.2, placing Tri II among the
most metal-poor Milky Way dwarf galaxies. In addition, the spectra of the
fainter member stars exhibit differences in their line widths that could be the
indication of a metallicity dispersion in the system. All these properties
paint a complex picture for Tri II, whose nature and current state are largely
speculative. The inferred metallicity properties of the system however lead us
to favor a scenario in which Tri II is a dwarf galaxy that is either disrupting
or embedded in a stellar stream.
