{"paper":{"title":"Light-cone effect on higher-order clustering in redshift surveys","arxiv_id":"astro-ph/9708121","primary_cat":"astro-ph","submitted_at":"1997-08-13T05:47:26+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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evolution.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.83,"main_claim_p":0.12,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.0,"method":0.5,"result":0.03,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.47,"interpretation":0.0}},{"i":2,"p":0.89,"id":"s2","own":true,"role":"method","text":"The general theory of this effect combined with the ansatz describing the non-linear evolution of clustering in simulations enables us to estimate the magnitude of the correction factor in different cosmologies.","hedge":{"p":0.96,"label":"asserted"},"own_p":0.72,"main_claim_p":0.07,"quantitative":false,"quantitative_p":0.05,"role_probabilities":{"gap":0.0,"method":0.89,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.11,"interpretation":0.0}},{"i":3,"p":1.0,"id":"s3","own":true,"role":"result","text":"In a series of numerical calculations assuming an array of cold dark matter models, it is found that, as long as galaxies are unbiased tracers of underlying density field, the effect is relatively small ($ \\simeq 10%$) for the shallow surveys ($z <0.2$), while it becomes significant (order of unity) in deep surveys ($z \\sim1$).","hedge":{"p":1.0,"label":"asserted"},"own_p":0.94,"main_claim_p":0.47,"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":4,"p":0.53,"id":"s4","own":true,"role":"result","text":"Depending on the scales of interest, the required correction is comparable to or smaller than the expected errors of on-going wide-field galaxy surveys such as the SDSS and 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