{"paper":{"title":"Long Duration X-Ray Flash and X-Ray Rich Gamma Ray Burst from Low Mass Population III Star","arxiv_id":"1207.2835","primary_cat":"astro-ph.HE","submitted_at":"2012-07-12T03:27:33+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. No sentence in this record was written by a language model.","schema":"pith.compiled-record/v0","status":"compiled","abstract":{"source":"arXiv listing abstract v2","sentences":[{"i":0,"p":1.0,"id":"s0","own":false,"role":"background","text":"Recent numerical simulations suggest that Population III (Pop III) stars were born with masses not larger than $\\sim 100 M_{\\odot}$ but typically $\\sim 40M_{\\odot}$.","hedge":{"p":0.99,"label":"hedged_possibility"},"own_p":0.05,"main_claim_p":0.03,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":1.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":1,"p":0.71,"id":"s1","own":true,"role":"result","text":"By self-consistently considering the jet generation and propagation in the envelope of these low mass Pop III stars, we find that a Pop III blue super giant star has the possibility to raise a gamma-ray burst (GRB) even though it keeps a massive hydrogen envelope.","hedge":{"p":0.86,"label":"hedged_possibility"},"own_p":0.95,"main_claim_p":0.42,"quantitative":false,"quantitative_p":0.09,"role_probabilities":{"gap":0.0,"method":0.05,"result":0.71,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.24,"interpretation":0.0}},{"i":2,"p":1.0,"id":"s2","own":true,"role":"result","text":"We evaluate observational characters of Pop III GRBs and predict that Pop III GRBs have the duration of $\\sim 10^5$ sec in the observer frame and the peak luminosity of $\\sim 5 \\times 10^{50} {\\rm erg} {\\rm sec}^{-1}$.","hedge":{"p":0.89,"label":"asserted"},"own_p":0.91,"main_claim_p":0.34,"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":3,"p":1.0,"id":"s3","own":true,"role":"result","text":"Assuming that the $E_p-L_p$ (or $E_p-E_{\\gamma, \\rm iso}$) correlation holds for Pop III GRBs, we find that the spectrum peak energy falls $\\sim$ a few keV (or $\\sim 100$ keV) in the observer frame.","hedge":{"p":0.87,"label":"asserted"},"own_p":0.89,"main_claim_p":0.1,"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":4,"p":0.54,"id":"s4","own":true,"role":"contribution","text":"We discuss the detectability of Pop III GRBs by future satellite missions such as EXIST and Lobster.","hedge":{"p":0.82,"label":"asserted"},"own_p":0.55,"main_claim_p":0.05,"quantitative":false,"quantitative_p":0.05,"role_probabilities":{"gap":0.0,"method":0.02,"result":0.03,"background":0.0,"limitation":0.0,"future_work":0.25,"contribution":0.54,"interpretation":0.16}},{"i":5,"p":0.52,"id":"s5","own":true,"role":"interpretation","text":"If the $E_p-E_{\\gamma, \\rm iso}$ correlation holds, we have the possibility to detect Pop III GRBs at $z \\sim 9$ as long duration X-ray rich GRBs by EXIST.","hedge":{"p":1.0,"label":"hedged_possibility"},"own_p":0.66,"main_claim_p":0.26,"quantitative":true,"quantitative_p":0.97,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.47,"background":0.0,"limitation":0.0,"future_work":0.01,"contribution":0.0,"interpretation":0.52}},{"i":6,"p":0.52,"id":"s6","own":true,"role":"interpretation","text":"On the other hand, if the $E_p-L_p$ correlation holds, we have the possibility to detect Pop III GRBs up to $z \\sim 19$ as long duration X-ray flashes by Lobster.","hedge":{"p":1.0,"label":"hedged_possibility"},"own_p":0.77,"main_claim_p":0.25,"quantitative":true,"quantitative_p":0.98,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.47,"background":0.0,"limitation":0.0,"future_work":0.01,"contribution":0.0,"interpretation":0.52}}]},"compiled":{"main_claim":{"p":0.93,"text":"By self-consistently considering the jet generation and propagation in the envelope of these low mass Pop III stars, we 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