  We present J=1-0 and J=2-1 12CO maps of several star-forming regions in both
the Large and the Small Magellanic Cloud, and briefly discuss their structure.
Many of the detected molecular clouds are relatively isolated and quite small
with dimensions of typically 20 pc. Some larger complexes have been detected,
but in all cases the extent of the molecular clouds sampled by CO emission is
significantly less than the extent of the ionized gas of the star-formation
region. Very little diffuse extended CO emission was seen; diffuse CO in
between or surrounding the detected discrete clouds is either very weak or
absent. The majority of all LMC lines of sight detected in 13CO has an isotopic
emission ratio I(12CO)/I(13CO) of about 10, i.e. twice higher than found in
Galactic star-forming complexes. At the lowest 12CO intensities, the spread of
isotopic emission ratios rapidly increases, low ratios representing relatively
dense and cold molecular gas and high ratios marking CO photo-dissociation at
cloud edges.
