M33 dust-selected molecular cloud catalogue

The mass function of these clouds follows a slope proportional to M^-2.84^, steeper than many previous studies of GMCs in local galaxies, implying that M33 is poorer at forming massive clouds than other nearby spirals. While we can rule out interstellar pressure as the major contributing factor, we are unable to disentangle the relative effects of metallicity and HI velocity dispersion. We find a reasonably featureless number density profile with galactocentric radius, and weak correlations between galactocentric radius and dust temperature/mass.

These clouds are reasonably consistent with Larson's scaling relationships, and many of our sources are co-spatial with earlier CO studies. Massive clouds are identified at large galactocentric radius, unlike in these earlier studies, perhaps indicating a population of CO-dark gas dominated clouds at these larger distances.