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We present an analysis of the first space-based far-IR-submm observations ofM 33, which measure the emission from the cool dust and resolve the giantmolecular cloud complexes. With roughly half-solar abundances, M33 is a firststep towards young low-metallicity galaxies where the submm may be able toprovide an alternative to CO mapping to measure their H$_2$ content. In thisLetter, we measure the dust emission cross-section $\sigma$ using SPIRE andrecent CO and \HI\ observations; a variation in $\sigma$ is present from anear-solar neighborhood cross-section to about half-solar with the maximumbeing south of the nucleus. Calculating the total H column density from themeasured dust temperature and cross-section, and then subtracting the \HI\column, yields a morphology similar to that observed in CO. The H$_2$/\HI\ massratio decreases from about unity to well below 10% and is about 15% averagedover the optical disk. The single most important observation to reduce thepotentially large systematic errors is to complete the CO mapping of M 33.

Cool gas and dust in M33: Results from the Herschel M33 extended survey (HERM33ES)