{"paper":{"title":"Halo model and halo properties in Galileon gravity cosmologies","arxiv_id":"1401.1497","primary_cat":"astro-ph.CO","submitted_at":"2014-01-07T20:59:53+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":0.94,"id":"s0","own":true,"role":"contribution","text":"We investigate the performance of semi-analytical modelling of large-scale structure in Galileon gravity cosmologies using results from N-body simulations.","hedge":{"p":0.52,"label":"asserted"},"own_p":0.94,"main_claim_p":0.05,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.0,"method":0.06,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.94,"interpretation":0.0}},{"i":1,"p":0.36,"id":"s1","own":false,"role":"background","text":"We focus on the Cubic and Quartic Galileon models that provide a reasonable fit to CMB, SNIa and BAO data.","hedge":{"p":0.88,"label":"asserted"},"own_p":0.23,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.09,"role_probabilities":{"gap":0.0,"method":0.31,"result":0.0,"background":0.36,"limitation":0.01,"future_work":0.0,"contribution":0.32,"interpretation":0.0}},{"i":2,"p":0.97,"id":"s2","own":true,"role":"result","text":"We demonstrate that the Sheth-Tormen mass function and linear halo bias can be calibrated to provide a very good fit to our simulation results.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.95,"main_claim_p":0.22,"quantitative":false,"quantitative_p":0.16,"role_probabilities":{"gap":0.0,"method":0.01,"result":0.97,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.02,"interpretation":0.0}},{"i":3,"p":1.0,"id":"s3","own":true,"role":"result","text":"We also find that the halo concentration-mass relation is well fitted by a power law.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.94,"main_claim_p":0.07,"quantitative":false,"quantitative_p":0.07,"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":0.98,"id":"s4","own":true,"role":"result","text":"The nonlinear matter power spectrum computed in the halo model approach is found to be inaccurate in the mildly nonlinear regime, but captures reasonably well the effects of the Vainshtein screening mechanism on small scales.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.95,"main_claim_p":0.24,"quantitative":false,"quantitative_p":0.46,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.98,"background":0.0,"limitation":0.02,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":5,"p":0.9,"id":"s5","own":true,"role":"result","text":"In the Cubic model, the screening mechanism hides essentially all of the effects of the fifth force inside haloes.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.88,"main_claim_p":0.1,"quantitative":false,"quantitative_p":0.36,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.9,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.1}},{"i":6,"p":0.92,"id":"s6","own":true,"role":"result","text":"In the case of the Quartic model, the screening mechanism leaves behind residual modifications to gravity, which make the effective gravitational strength time-varying and smaller than the standard value.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.9,"main_claim_p":0.13,"quantitative":true,"quantitative_p":0.85,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.92,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.08}},{"i":7,"p":0.59,"id":"s7","own":true,"role":"interpretation","text":"Compared to normal gravity, this causes a deficiency of massive haloes and leads to a weaker matter clustering on small 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