{"paper":{"title":"Evolution of faint radio sources in the VIDEO-XMM3 field","arxiv_id":"1309.0358","primary_cat":"astro-ph.CO","submitted_at":"2013-09-02T10:49:51+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. 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history of the universe.","hedge":{"p":0.96,"label":"asserted"},"own_p":0.04,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.03,"role_probabilities":{"gap":0.01,"method":0.0,"result":0.0,"background":0.99,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":2,"p":1.0,"id":"s2","own":true,"role":"contribution","text":"In this paper we present a new investigation of the evolution of faint radio sources out to $z{\\sim}2.5$.","hedge":{"p":0.93,"label":"asserted"},"own_p":0.88,"main_claim_p":0.04,"quantitative":true,"quantitative_p":0.92,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":1.0,"interpretation":0.0}},{"i":3,"p":0.99,"id":"s3","own":true,"role":"method","text":"We combine a 1 square degree VLA radio survey, complete to a depth of 100 $\\mu$Jy, with accurate 10 band photometric redshifts from the VIDEO and CFHTLS surveys.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.94,"main_claim_p":0.02,"quantitative":true,"quantitative_p":0.98,"role_probabilities":{"gap":0.0,"method":0.99,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.01,"interpretation":0.0}},{"i":4,"p":1.0,"id":"s4","own":true,"role":"result","text":"The results indicate that the radio population experiences mild positive evolution out to $z{\\sim}1.2$ increasing their space density by a factor of $\\sim$3, consistent with results of several previous studies.","hedge":{"p":0.93,"label":"hedged_possibility"},"own_p":0.92,"main_claim_p":0.35,"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":5,"p":1.0,"id":"s5","own":true,"role":"result","text":"Beyond $z$=1.2 there is evidence of a slowing down of this evolution.","hedge":{"p":0.8,"label":"hedged_possibility"},"own_p":0.88,"main_claim_p":0.14,"quantitative":true,"quantitative_p":0.93,"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":6,"p":0.91,"id":"s6","own":true,"role":"interpretation","text":"Star-forming galaxies drive the more rapid evolution at low redshifts, $z{<}$1.2, while more slowly evolving AGN populations dominate at higher redshifts resulting in a decline in the evolution of the radio luminosity function at $z{>}$1.2.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.86,"main_claim_p":0.41,"quantitative":true,"quantitative_p":0.97,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.09,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.91}},{"i":7,"p":0.98,"id":"s7","own":true,"role":"result","text":"The evolution is best fit by pure luminosity evolution with star-forming 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