A detailed view of a Molecular Cloud in the far outer disk of M33
  The amount of H$_2$ present in spiral galaxies remains uncertain,
particularly in the dim outer regions and in low-metallicity environments. We
present high-resolution CO(1--0) observations with the Plateau de Bure
interferometer of the most distant molecular cloud in the local group galaxy M
33. The cloud is a single entity rather than a set of smaller clouds within the
broad beam of the original single-dish observations. The interferometer and
single-dish fluxes are very similar and the line widths are indistinguishable,
despite the difference in beamsize. At a spatial resolution of 10 pc, beyond
the optical radius of the M 33, the CO brightness temperature reaches 2.4
Kelvins. A virial mass estimate for the cloud yields a mass of $4.3 \times
10^4$ \msun and a ratio $\ratio \simeq 3.5 \times 10^{20} \Xunit$. While no
velocity gradient is seen where the emission is strong, the velocity is
redshifted to the extreme SW and blue-shifted to the far NE. If the orientation
of the cloud is along the plane of the disk (i.e. not perpendicular), then
these velocities correspond to slow infall or accretion. The rather modest
infall rate would be about $2 \times 10^{-4}$\moyr.
