, Henkel C.
, Bomans D.J.
, Wilson T.L.
GKSS Forschungszentrum, Institut für Physik, Maz-Plank-Strasse,
D-21502 Geestacht, Germany
Max Planck Institut für Radioastronomie, Auf dem Hügel 69,
D-53121 Bonn, Germany
Sternwarte der Universität Bonn, Auf dem Hügel 71,
D-53121 Bonn, Germany 
(340
pc at 
Mpc) toward 20 positions. At eight positions,
emission was detected from a molecular cloud complex with a size of
1000 pc
700 pc (at the 0.7 K kms
contour) and a mass of a
few 
. The 
line
intensity ratio is 0.4, indicating emission from optically thick
subthermally excited lines. Comparing virial masses with masses
deduced from the integrated CO intensities yields a 
conversion factor, which is a few times the
standard Galactic value of 
(cm
K kms
)
. On the
basis of radial velocity, the huge CO complex is resolved into a
western, a central, and an eastern component. The radial velocities,
298, 308, and 305 kms
, demonstrate that the E--W velocity change
across the central bar is not smooth on linear scales <1 kpc. A
prominent loop of H
emission (diameter : 
pc) is found
at the interface between the western and eastern complex. A narrow
linewidth and a lack of associated H
emission indicates
that the western CO complex is in a quiescent state. The eastern
region, being located close to the starburst knot at the optical
center of the galaxy, exhibits broader CO lines and intense
H
emission and must form massive stars.