{"paper":{"title":"The Atomic-to-Molecular Transition in Galaxies. III. A New Method for Determining the Molecular Content of Primordial and Dusty Clouds","arxiv_id":"0908.0330","primary_cat":"astro-ph.GA","submitted_at":"2009-08-03T20:00:58+00:00","version_compiled":"v2"},"notice":"Every quoted sentence is the authors' text from the arXiv listing abstract. Labels and probabilities are the outputs of classifier-1.13-20260917 on the question bank abstract-p1-20260923, exactly as returned. 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field.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.94,"main_claim_p":0.21,"quantitative":false,"quantitative_p":0.06,"role_probabilities":{"gap":0.0,"method":0.28,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.72,"interpretation":0.0}},{"i":2,"p":0.91,"id":"s2","own":true,"role":"method","text":"We consider both planar and spherical clouds, and H_2 formation either in the gas phase or catalyzed by dust grains.","hedge":{"p":0.79,"label":"asserted"},"own_p":0.76,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.06,"role_probabilities":{"gap":0.0,"method":0.91,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.09,"interpretation":0.0}},{"i":3,"p":0.43,"id":"s3","own":true,"role":"method","text":"Under the assumption that the transition from atomic to molecular gas is sharp, our method gives the solution without any reference to the photodissociation cross 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