Abstract
We present an approach for analyzing the morphology and physical properties of H I features near giant OB associations in M33, in the context of a model whereby the H I excess arises from photodissociation of the molecular gas in remnants of the parent giant molecular clouds (GMCs). Examples are presented here in the environs of NGC 604 and CPSDP Z204, two prominent H II regions in M33. These are the first results of a detailed analysis of the environs of a large number of OB associations in that galaxy. We present evidence for diffusion of the far-UV radiation from the OB association through a clumpy remnant GMC, and show further that enhanced CO(1-0) emission appears preferentially associated with GMCs of higher volume density.
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