{"paper":{"title":"Ram pressure stripping in a galaxy formation model. I. A novel numerical approach","arxiv_id":"1006.5446","primary_cat":"astro-ph.CO","submitted_at":"2010-06-28T19:59:51+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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(ICM).","hedge":{"p":1.0,"label":"asserted"},"own_p":0.9,"main_claim_p":0.04,"quantitative":false,"quantitative_p":0.03,"role_probabilities":{"gap":0.0,"method":0.41,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.59,"interpretation":0.0}},{"i":2,"p":0.49,"id":"s2","own":true,"role":"method","text":"This allows a self-consistent estimation of the RPS experienced by satellite galaxies.","hedge":{"p":0.97,"label":"asserted"},"own_p":0.61,"main_claim_p":0.08,"quantitative":false,"quantitative_p":0.03,"role_probabilities":{"gap":0.0,"method":0.49,"result":0.02,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.3,"interpretation":0.19}},{"i":3,"p":1.0,"id":"s3","own":true,"role":"result","text":"We find that the ram pressure (RP) in the central regions of clusters increases approximately one order of magnitude between z = 1 and 0, consistent with the increase in the density of the ICM.","hedge":{"p":0.97,"label":"asserted"},"own_p":0.96,"main_claim_p":0.13,"quantitative":true,"quantitative_p":0.98,"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":1.0,"id":"s4","own":true,"role":"result","text":"The mean RP experienced by galaxies within the virial radius increases with decreasing redshift.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.91,"main_claim_p":0.11,"quantitative":true,"quantitative_p":0.56,"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":1.0,"id":"s5","own":true,"role":"result","text":"In clusters with virial masses M_vir ~10^15 h^-1 M_Sun, over 50 per cent of satellite galaxies have experienced RP ~10^(-11) h^2 dyn cm^-2 or higher for z <= 0.5.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.95,"main_claim_p":0.13,"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":6,"p":1.0,"id":"s6","own":true,"role":"result","text":"In smaller clusters (M_vir ~10^14 h^-1 M_Sun) the mean RP are approximately one order of magnitude lower at all redshifts.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.92,"main_claim_p":0.06,"quantitative":true,"quantitative_p":0.98,"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":7,"p":1.0,"id":"s7","own":true,"role":"result","text":"RPS has a strong effect on the cold gas content of galaxies for all cluster masses.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.88,"main_claim_p":0.24,"quantitative":false,"quantitative_p":0.09,"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":8,"p":1.0,"id":"s8","own":true,"role":"result","text":"At z = 0, over 70 per cent of satellite galaxies within the virial radius are completely depleted of cold gas.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.93,"main_claim_p":0.2,"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":9,"p":0.97,"id":"s9","own":true,"role":"result","text":"For the more massive clusters the fraction of depleted galaxies is already established at z ~ 1, whereas for the smaller clusters this fraction increases appreciably between z = 1 and 0.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.92,"main_claim_p":0.12,"quantitative":true,"quantitative_p":0.91,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.97,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.03}},{"i":10,"p":0.99,"id":"s10","own":true,"role":"interpretation","text":"This indicates that the rate at which the cold gas is stripped depends on the virial mass of the host cluster.","hedge":{"p":0.96,"label":"hedged_possibility"},"own_p":0.86,"main_claim_p":0.2,"quantitative":false,"quantitative_p":0.06,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.01,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.99}},{"i":11,"p":0.98,"id":"s11","own":true,"role":"result","text":"Compared to our new approach, the use of an analytic profile to describe the ICM results in an overestimation of the RP larger than 50 per cent for z >= 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