2 10
M
molecular gas which probably still feeds star formation of its internal
stellar cluster.
When comparing the molecular gas mass, calculated for Galactic conditions,
and the virial mass we obtain a conversion factor 
20 times higher than
the Galactic value. However, we believe that the molecular clouds near the
stellar clusters are not in kinematic equilibrium so that the virial theorem
does not apply; we therefore reject this conversion factor as unrealistic.
Our spectroscopic observations seem to indicate an optical counterpart of the
HI cavity around A, though being smaller in extent, and a surrounding
shell of ionized gas of 
50 pc diameter.
The compact galaxy NGC 1705 contains a
stellar cluster even brighter than A and B. We did not detect CO in this
galaxy.
to be published in A&A
Figure 4: Sample spectra from the central 8
of the
2.5
spatial resolution CO map. Spectral resolution is 10 kms
.
The 2
spacing of the spectra are indicated in the
upper left corner of each box as offsets relative to the nuclear
pointing position. The velocity scale is relative to the ``nominal''
systemic LSR velocity of 4925 kms
.