{"paper":{"title":"An Explanation for the Different X-ray to Optical Column Densities in the Environments of Gamma Ray Bursts: A Progenitor Embedded in a Dense Medium","arxiv_id":"1307.7199","primary_cat":"astro-ph.GA","submitted_at":"2013-07-27T00:36:24+00:00","version_compiled":"v1"},"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. No sentence in this record was written by a language model.","schema":"pith.compiled-record/v0","status":"compiled","abstract":{"source":"arXiv listing abstract v1","sentences":[{"i":0,"p":0.82,"id":"s0","own":true,"role":"contribution","text":"We study the > 10 ratios in the X-ray to optical column densities inferred from afterglow spectra of Gamma Ray Bursts due to gas surrounding their progenitors.","hedge":{"p":0.66,"label":"asserted"},"own_p":0.74,"main_claim_p":0.03,"quantitative":true,"quantitative_p":0.95,"role_probabilities":{"gap":0.02,"method":0.0,"result":0.0,"background":0.16,"limitation":0.0,"future_work":0.0,"contribution":0.82,"interpretation":0.0}},{"i":1,"p":0.83,"id":"s1","own":true,"role":"method","text":"We present time-evolving photoionization calculations for these afterglows and explore different conditions for their environment.","hedge":{"p":0.77,"label":"asserted"},"own_p":0.94,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.0,"method":0.83,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.17,"interpretation":0.0}},{"i":2,"p":1.0,"id":"s2","own":true,"role":"result","text":"We find that homogenous models of the environment (constant density) predict X-ray columns similar to those found in the optical spectra, with the bulk of the opacity being produced by neutral material at large distances from the burst.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.95,"main_claim_p":0.07,"quantitative":true,"quantitative_p":0.76,"role_probabilities":{"gap":0.0,"method":0.0,"result":1.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":3,"p":0.95,"id":"s3","own":true,"role":"result","text":"This result is independent of gas density or metallicity.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.86,"main_claim_p":0.04,"quantitative":false,"quantitative_p":0.06,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.95,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.05}},{"i":4,"p":1.0,"id":"s4","own":true,"role":"result","text":"Only models assuming a progenitor immersed in a dense (10^(2-4) cm-3) cloud of gas (with radius ~10 pc), with a strong, declining gradient of density for the surrounding interstellar medium are able to account for the large X-ray to optical column density ratios.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.92,"main_claim_p":0.82,"quantitative":true,"quantitative_p":0.98,"role_probabilities":{"gap":0.0,"method":0.0,"result":1.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":5,"p":0.54,"id":"s5","own":true,"role":"limitation","text":"However, to avoid an unphysical correlation between the size of this cloud, and the size of the ionization front produced by the GRB, the models also require that the circumburst medium is already ionized prior to the burst.","hedge":{"p":0.98,"label":"asserted"},"own_p":0.8,"main_claim_p":0.09,"quantitative":false,"quantitative_p":0.08,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.42,"background":0.0,"limitation":0.54,"future_work":0.0,"contribution":0.0,"interpretation":0.04}},{"i":6,"p":1.0,"id":"s6","own":true,"role":"result","text":"The inferred cloud masses are <10^6 M_solar, even if low metallicities in the medium are assumed (Z~0.1 Z_solar).","hedge":{"p":0.99,"label":"asserted"},"own_p":0.91,"main_claim_p":0.05,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.0,"method":0.0,"result":1.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":7,"p":0.99,"id":"s7","own":true,"role":"interpretation","text":"These cloud properties are consistent with those found in giant molecular clouds and our results support a scenario in which the progenitors reside within intense star formation regions of galaxies.","hedge":{"p":0.81,"label":"hedged_possibility"},"own_p":0.67,"main_claim_p":0.35,"quantitative":false,"quantitative_p":0.4,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.01,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.99}},{"i":8,"p":0.77,"id":"s8","own":true,"role":"future_work","text":"Finally, we show that modeling over large samples of GRB afterglows may offer strong constraints on the range of properties in these clouds, and the host galaxy ISM.","hedge":{"p":0.87,"label":"hedged_possibility"},"own_p":0.79,"main_claim_p":0.08,"quantitative":false,"quantitative_p":0.06,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.12,"background":0.0,"limitation":0.0,"future_work":0.77,"contribution":0.04,"interpretation":0.07}}]},"compiled":{"main_claim":{"p":0.79,"text":"Only models assuming a 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