Triangulum II: Not Especially Dense After All
  Among the Milky Way satellites discovered in the past three years, Triangulum
II has presented the most difficulty in revealing its dynamical status. Kirby
et al. (2015a) identified it as the most dark matter-dominated galaxy known,
with a mass-to-light ratio within the half-light radius of 3600 +3500 -2100
M_sun/L_sun. On the other hand, Martin et al. (2016) measured an outer velocity
dispersion that is 3.5 +/- 2.1 times larger than the central velocity
dispersion, suggesting that the system might not be in equilibrium. From new
multi-epoch Keck/DEIMOS measurements of 13 member stars in Triangulum II, we
constrain the velocity dispersion to be sigma_v < 3.4 km/s (90% C.L.). Our
previous measurement of sigma_v, based on six stars, was inflated by the
presence of a binary star with variable radial velocity. We find no evidence
that the velocity dispersion increases with radius. The stars display a wide
range of metallicities, indicating that Triangulum II retained supernova ejecta
and therefore possesses or once possessed a massive dark matter halo. However,
the detection of a metallicity dispersion hinges on the membership of the two
most metal-rich stars. The stellar mass is lower than galaxies of similar mean
stellar metallicity, which might indicate that Triangulum II is either a star
cluster or a tidally stripped dwarf galaxy. Detailed abundances of one star
show heavily depressed neutron-capture abundances, similar to stars in most
other ultra-faint dwarf galaxies but unlike stars in globular clusters.
