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We compare the properties of clouds in simulated M33 galaxies to thoseobserved in the real M33. We apply a friends of friends algorithm and CPROPS toidentify clouds, as well as a pixel by pixel analysis. We obtain very goodagreement between the number of clouds, and maximum mass of clouds. Both arelower than occurs for a Milky Way-type galaxy and thus are a function of thesurface density, size and galactic potential of M33. We reproduce the observeddependence of molecular cloud properties on radius in the simulations, and findthis is due to the variation in gas surface density with radius. The cloudspectra also show good agreement between the simulations and observations, butthe exact slope and shape of the spectra depends on the algorithm used to findclouds, and the range of cloud masses included when fitting the slope.Properties such as cloud angular momentum, velocity dispersions and virialrelation are also in good agreement between the simulations and observations,but do not necessarily distinguish between simulations of M33 and other galaxysimulations. Our results are not strongly dependent on the level of feedbackused here (10 and 20%) although they suggest that 15% feedback efficiency maybe optimal. Overall our results suggest that the molecular cloud properties areprimarily dependent on the gas and mass surface density, and less dependent onthe localised physics such as the details of stellar feedback, or the numericalcode used.

Comparing the Properties of GMCs in M33 from Simulations and Observations