, D. Reynaud
, P. M. Solomon
,
S. J. E. Radford
Institut de Radio Astronomie Millimétrique,
38406 St. Martin d'Hères, France
Astronomy Program, State University of New York,
Stony Brook, NY 11794
National Radio Astronomy Observatory, Tucson AZ 85721-0665 
. Most of the molecular gas in the
galaxy is in a central ellipse with a major axis of 3.5 kpc. This
major axis and the strongest velocity gradients are
perpendicular to the bar. Position-velocity diagrams are consistent
with the molecular gas following elliptical orbits along the bar, but
show important deviations at the strong shock fronts and close to the
nucleus, where the gas follows orbits perpendicular to the bar. We
also detect giant molecular complexes near the ends of the bar and
much fainter CO in molecular clouds in the SE spiral arm. In spite of
its high CO luminosity and great central concentration of molecular
gas, the galaxy has only a modest 
ratio,
which suggests a relatively low rate of star formation. Although the
molecular gas has a latent capacity to fuel a large starburst, further
infall to the center is probably hindered by the closed orbits 1.5 kpc
from the nucleus. Hence most of the gas cannot attain the critical
density needed for a large starburst.