{"paper":{"title":"Relativistic corrections and non-Gaussianity in radio continuum surveys","arxiv_id":"1206.0732","primary_cat":"astro-ph.CO","submitted_at":"2012-06-04T20:00:01+00:00","version_compiled":"v4"},"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 v4","sentences":[{"i":0,"p":1.0,"id":"s0","own":false,"role":"background","text":"Forthcoming radio continuum surveys will cover large volumes of the observable Universe and will reach to high redshifts, making them potentially powerful probes of dark energy, modified gravity and non-Gaussianity.","hedge":{"p":0.99,"label":"hedged_possibility"},"own_p":0.06,"main_claim_p":0.05,"quantitative":false,"quantitative_p":0.06,"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":0.99,"id":"s1","own":true,"role":"contribution","text":"Here we extend recent works by analyzing the general relativistic (GR) corrections to the angular power spectrum.","hedge":{"p":0.93,"label":"asserted"},"own_p":0.9,"main_claim_p":0.05,"quantitative":false,"quantitative_p":0.05,"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":2,"p":0.74,"id":"s2","own":false,"role":"result","text":"These GR corrections to the standard Newtonian analysis of the power spectrum become significant on scales near and beyond the Hubble scale at each redshift.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.4,"main_claim_p":0.15,"quantitative":false,"quantitative_p":0.22,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.74,"background":0.17,"limitation":0.0,"future_work":0.0,"contribution":0.02,"interpretation":0.07}},{"i":3,"p":0.88,"id":"s3","own":false,"role":"method","text":"We consider the continuum surveys with LOFAR, WSRT and ASKAP, and examples of continuum surveys with the SKA.","hedge":{"p":0.75,"label":"asserted"},"own_p":0.34,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.05,"role_probabilities":{"gap":0.0,"method":0.88,"result":0.0,"background":0.01,"limitation":0.0,"future_work":0.0,"contribution":0.11,"interpretation":0.0}},{"i":4,"p":1.0,"id":"s4","own":true,"role":"result","text":"We find that the GR corrections are at most percent-level in LOFAR, WODAN and EMU surveys, but they can produce $O(10%)$ changes for high enough sensitivity SKA continuum surveys.","hedge":{"p":0.97,"label":"asserted"},"own_p":0.95,"main_claim_p":0.31,"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":0.38,"id":"s5","own":true,"role":"interpretation","text":"The signal is however dominated by cosmic variance, and multiple-tracer observations will be needed to overcome this problem.","hedge":{"p":0.97,"label":"asserted"},"own_p":0.61,"main_claim_p":0.15,"quantitative":false,"quantitative_p":0.1,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.13,"background":0.0,"limitation":0.33,"future_work":0.16,"contribution":0.0,"interpretation":0.38}},{"i":6,"p":0.72,"id":"s6","own":true,"role":"interpretation","text":"The GR corrections are suppressed in continuum surveys because of the integration over redshift -- we expect that GR corrections will be enhanced for future SKA HI surveys in which the source redshifts will be known.","hedge":{"p":0.48,"label":"hedged_possibility"},"own_p":0.59,"main_claim_p":0.11,"quantitative":false,"quantitative_p":0.25,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.17,"background":0.0,"limitation":0.03,"future_work":0.08,"contribution":0.0,"interpretation":0.72}},{"i":7,"p":0.99,"id":"s7","own":true,"role":"contribution","text":"We also provide predictions for the angular power spectra in the case where the primordial perturbations have local non-Gaussianity.","hedge":{"p":0.88,"label":"asserted"},"own_p":0.86,"main_claim_p":0.06,"quantitative":false,"quantitative_p":0.06,"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":8,"p":1.0,"id":"s8","own":true,"role":"result","text":"We find that non-Gaussianity dominates over GR corrections, and rises above cosmic variance when $f_{\\rm NL}\\gtrsim5$ for SKA continuum surveys.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.95,"main_claim_p":0.36,"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}}]},"compiled":{"main_claim":{"p":0.85,"text":"We find that non-Gaussianity dominates over GR corrections, and rises above cosmic variance when $f_{\\rm NL}\\gtrsim5$ for SKA continuum 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