{"paper":{"title":"Galaxy-Induced Transformation of Dark Matter Halos","arxiv_id":"0902.2477","primary_cat":"astro-ph.GA","submitted_at":"2009-02-14T16:49:04+00:00","version_compiled":"v1"},"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 v1","sentences":[{"i":0,"p":0.55,"id":"s0","own":true,"role":"contribution","text":"We use N-body/gasdynamical LambdaCDM cosmological simulations to examine the effect of the assembly of a central galaxy on the shape and mass profile of its dark halo.","hedge":{"p":0.79,"label":"asserted"},"own_p":0.95,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.05,"role_probabilities":{"gap":0.0,"method":0.45,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.55,"interpretation":0.0}},{"i":1,"p":0.98,"id":"s1","own":true,"role":"method","text":"Two series of simulations are compared; one that follows only the evolution of the dark matter component and a second one where a baryonic component is added.","hedge":{"p":0.93,"label":"asserted"},"own_p":0.88,"main_claim_p":0.02,"quantitative":true,"quantitative_p":0.57,"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":2,"p":0.82,"id":"s2","own":true,"role":"limitation","text":"These simulations include radiative cooling but neglect star formation and feedback, leading most baryons to collect at the halo center in a disk which is too small and too massive when compared with typical spiral.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.81,"main_claim_p":0.03,"quantitative":true,"quantitative_p":0.69,"role_probabilities":{"gap":0.0,"method":0.18,"result":0.0,"background":0.0,"limitation":0.82,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":3,"p":0.95,"id":"s3","own":false,"role":"limitation","text":"This unrealistic model allows us, nevertheless, to gauge the maximum effect that galaxies may have in transforming their dark halos.","hedge":{"p":0.87,"label":"asserted"},"own_p":0.44,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.18,"role_probabilities":{"gap":0.0,"method":0.02,"result":0.0,"background":0.0,"limitation":0.95,"future_work":0.0,"contribution":0.0,"interpretation":0.03}},{"i":4,"p":1.0,"id":"s4","own":true,"role":"result","text":"We find that the shape of the halo becomes more axisymmetric: halos are transformed from triaxial into essentially oblate systems, with well-aligned isopotential contours of roughly constant flattening (c/a ~ 0.85).","hedge":{"p":1.0,"label":"asserted"},"own_p":0.95,"main_claim_p":0.35,"quantitative":true,"quantitative_p":0.97,"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":"Halos always contract as a result of galaxy assembly, but the effect is substantially less pronounced than predicted by the \"adiabatic contraction\" hypothesis.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.94,"main_claim_p":0.37,"quantitative":true,"quantitative_p":0.96,"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":"interpretation","text":"The reduced contraction helps to reconcile LambdaCDM halos with constraints on the dark matter content inside the solar circle and should alleviate the long-standing difficulty of matching simultaneously the scaling properties of galaxy disks and the luminosity function.","hedge":{"p":0.63,"label":"hedged_possibility"},"own_p":0.55,"main_claim_p":0.19,"quantitative":false,"quantitative_p":0.18,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":1.0}},{"i":7,"p":0.53,"id":"s7","own":true,"role":"interpretation","text":"The halo contraction is also less pronounced than found in earlier simulations, a disagreement that suggests that halo contraction is not solely a function of the initial and final distribution of baryons.","hedge":{"p":0.7,"label":"hedged_possibility"},"own_p":0.57,"main_claim_p":0.11,"quantitative":true,"quantitative_p":0.89,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.47,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.53}},{"i":8,"p":0.59,"id":"s8","own":true,"role":"interpretation","text":"Not only how much baryonic mass has been deposited at the center of a halo matters, but also the mode of its deposition.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.81,"main_claim_p":0.31,"quantitative":false,"quantitative_p":0.14,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.41,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.59}},{"i":9,"p":0.8,"id":"s9","own":false,"role":"interpretation","text":"It might prove impossible to predict the halo response without a detailed understanding of a galaxy's assembly history. 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