{"paper":{"title":"Spallation Backgrounds in Super-Kamiokande Are Made in Muon-Induced Showers","arxiv_id":"1503.04823","primary_cat":"hep-ph","submitted_at":"2015-03-16T20:01:12+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":0.79,"id":"s0","own":false,"role":"background","text":"Crucial questions about solar and supernova neutrinos remain unanswered.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.03,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.03,"role_probabilities":{"gap":0.21,"method":0.0,"result":0.0,"background":0.79,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":1,"p":0.93,"id":"s1","own":false,"role":"background","text":"Super-Kamiokande has the exposure needed for progress, but detector backgrounds are a limiting factor.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.08,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.04,"method":0.0,"result":0.0,"background":0.93,"limitation":0.02,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":2,"p":1.0,"id":"s2","own":false,"role":"background","text":"A leading component is the beta decays of isotopes produced by cosmic-ray muons and their secondaries, which initiate nuclear spallation reactions.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.07,"main_claim_p":0.08,"quantitative":false,"quantitative_p":0.04,"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":3,"p":0.94,"id":"s3","own":false,"role":"background","text":"Cuts of events after and surrounding muon tracks reduce this spallation decay background by $\\simeq 90\\%$ (at a cost of $\\simeq 20\\%$ deadtime), but its rate at 6--18 MeV is still dominant.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.28,"main_claim_p":0.05,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.03,"method":0.0,"result":0.0,"background":0.94,"limitation":0.02,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":4,"p":0.97,"id":"s4","own":false,"role":"background","text":"A better way to cut this background was suggested in a Super-Kamiokande paper [Bays {\\it et al.}, Phys.~Rev.~D {\\bf 85}, 052007 (2012)] on a search for the diffuse supernova neutrino background.","hedge":{"p":0.93,"label":"asserted"},"own_p":0.03,"main_claim_p":0.04,"quantitative":false,"quantitative_p":0.22,"role_probabilities":{"gap":0.01,"method":0.01,"result":0.0,"background":0.97,"limitation":0.0,"future_work":0.0,"contribution":0.01,"interpretation":0.0}},{"i":5,"p":0.95,"id":"s5","own":false,"role":"background","text":"They found that spallation decays above 16 MeV were preceded near the same location by a peak in the apparent Cherenkov light profile from the muon; a more aggressive cut was applied to a limited section of the muon track, leading to decreased background without increased deadtime.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.04,"main_claim_p":0.07,"quantitative":true,"quantitative_p":0.64,"role_probabilities":{"gap":0.0,"method":0.02,"result":0.02,"background":0.95,"limitation":0.0,"future_work":0.0,"contribution":0.01,"interpretation":0.0}},{"i":6,"p":0.96,"id":"s6","own":true,"role":"contribution","text":"We put their empirical discovery on a firm theoretical foundation.","hedge":{"p":0.98,"label":"asserted"},"own_p":0.78,"main_claim_p":0.1,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.03,"method":0.0,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.96,"interpretation":0.01}},{"i":7,"p":0.92,"id":"s7","own":true,"role":"result","text":"We show that almost all spallation decay isotopes are produced by muon-induced showers and that these showers are rare enough and energetic enough to be identifiable.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.94,"main_claim_p":0.81,"quantitative":true,"quantitative_p":0.61,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.92,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.08,"interpretation":0.0}},{"i":8,"p":0.66,"id":"s8","own":true,"role":"contribution","text":"This is the first such demonstration for any detector.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.8,"main_claim_p":0.14,"quantitative":false,"quantitative_p":0.25,"role_probabilities":{"gap":0.08,"method":0.0,"result":0.2,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.66,"interpretation":0.06}},{"i":9,"p":0.78,"id":"s9","own":true,"role":"contribution","text":"We detail how the physics of showers explains the peak in the muon Cherenkov light profile and other Super-K observations.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.85,"main_claim_p":0.09,"quantitative":false,"quantitative_p":0.05,"role_probabilities":{"gap":0.0,"method":0.03,"result":0.05,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.78,"interpretation":0.14}},{"i":10,"p":0.93,"id":"s10","own":true,"role":"interpretation","text":"Our results provide a physical basis for practical improvements in background rejection that will benefit multiple studies.","hedge":{"p":0.94,"label":"asserted"},"own_p":0.64,"main_claim_p":0.19,"quantitative":false,"quantitative_p":0.05,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.01,"background":0.0,"limitation":0.0,"future_work":0.04,"contribution":0.02,"interpretation":0.93}},{"i":11,"p":0.9,"id":"s11","own":true,"role":"interpretation","text":"For solar neutrinos, in particular, it should be possible to dramatically reduce backgrounds at energies as low as 6 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