{"paper":{"title":"Primordial fluctuations and cosmological inflation after WMAP 1.0","arxiv_id":"hep-ph/0403129","primary_cat":"hep-ph","submitted_at":"2004-03-12T08:32:51+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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inflation.","hedge":{"p":0.82,"label":"asserted"},"own_p":0.37,"main_claim_p":0.23,"quantitative":false,"quantitative_p":0.11,"role_probabilities":{"gap":0.0,"method":0.01,"result":0.74,"background":0.03,"limitation":0.0,"future_work":0.0,"contribution":0.03,"interpretation":0.19}},{"i":2,"p":1.0,"id":"s2","own":true,"role":"result","text":"While observable modes cross the Hubble scale, it changes by less than 3% during one e-folding: d(d_H)/dt < 0.032 at 2 sigma.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.7,"main_claim_p":0.19,"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":0.92,"id":"s3","own":true,"role":"result","text":"The distance scale of inflation itself remains poorly constrained: 1.2 x 10^{-28} cm < d_H < 1 cm.","hedge":{"p":0.92,"label":"asserted"},"own_p":0.69,"main_claim_p":0.08,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.01,"method":0.0,"result":0.92,"background":0.0,"limitation":0.07,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":4,"p":0.99,"id":"s4","own":true,"role":"contribution","text":"(ii) We present a new classification of single-field inflationary scenarios (including scenarios beyond slow-roll inflation), based on physical criteria, namely the behaviour of the kinetic and total energy densities of the inflaton field.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.93,"main_claim_p":0.09,"quantitative":false,"quantitative_p":0.08,"role_probabilities":{"gap":0.0,"method":0.01,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.99,"interpretation":0.0}},{"i":5,"p":0.96,"id":"s5","own":true,"role":"result","text":"The current data show no preference for any of the scenarios.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.81,"main_claim_p":0.17,"quantitative":false,"quantitative_p":0.08,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.96,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.04}},{"i":6,"p":0.88,"id":"s6","own":true,"role":"contribution","text":"(iii) For the first time the slow-roll assumption could be dropped from the data analysis and replaced by the more general assumption that the Hubble scale is (almost) constant during the observable part of inflation.","hedge":{"p":0.95,"label":"hedged_possibility"},"own_p":0.87,"main_claim_p":0.25,"quantitative":false,"quantitative_p":0.08,"role_probabilities":{"gap":0.01,"method":0.09,"result":0.02,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.88,"interpretation":0.0}},{"i":7,"p":0.84,"id":"s7","own":true,"role":"contribution","text":"We present simple analytic expressions for the scalar and tensor power spectra for this 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