{"paper":{"title":"Efficient exploration of cosmology dependence in the EFT of LSS","arxiv_id":"1606.03633","primary_cat":"astro-ph.CO","submitted_at":"2016-06-11T21:35:27+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-1.13.0 on the question bank abstract-p1-20260923, exactly as returned. 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regime.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.07,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.05,"role_probabilities":{"gap":0.0,"method":0.01,"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 develop efficient implementations of these computations that allow for an exploration of their dependence on cosmological parameters.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.95,"main_claim_p":0.15,"quantitative":false,"quantitative_p":0.04,"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":0.9,"id":"s3","own":false,"role":"method","text":"They are based on two ideas.","hedge":{"p":0.77,"label":"asserted"},"own_p":0.34,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.1,"role_probabilities":{"gap":0.0,"method":0.9,"result":0.0,"background":0.01,"limitation":0.0,"future_work":0.0,"contribution":0.09,"interpretation":0.0}},{"i":4,"p":0.98,"id":"s4","own":true,"role":"method","text":"First, once an observable has been computed with high precision for a reference cosmology, for a new cosmology the same can be easily obtained with comparable precision just by adding the difference in that observable, evaluated with much less precision.","hedge":{"p":0.94,"label":"asserted"},"own_p":0.59,"main_claim_p":0.12,"quantitative":false,"quantitative_p":0.46,"role_probabilities":{"gap":0.0,"method":0.98,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.02,"interpretation":0.0}},{"i":5,"p":0.96,"id":"s5","own":false,"role":"method","text":"Second, most cosmologies of interest are sufficiently close to the Planck best-fit cosmology that observables can be obtained from a Taylor expansion around the reference cosmology.","hedge":{"p":0.77,"label":"asserted"},"own_p":0.26,"main_claim_p":0.07,"quantitative":false,"quantitative_p":0.31,"role_probabilities":{"gap":0.0,"method":0.96,"result":0.0,"background":0.0,"limitation":0.01,"future_work":0.0,"contribution":0.03,"interpretation":0.0}},{"i":6,"p":0.92,"id":"s6","own":true,"role":"contribution","text":"These ideas are implemented for the matter power spectrum at two loops and are released as public codes.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.94,"main_claim_p":0.14,"quantitative":false,"quantitative_p":0.25,"role_probabilities":{"gap":0.0,"method":0.07,"result":0.01,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.92,"interpretation":0.0}},{"i":7,"p":1.0,"id":"s7","own":true,"role":"result","text":"When applied to cosmologies that are within 3$\\sigma$ of the Planck best-fit model, the first method evaluates the power 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