{"paper":{"title":"Internal properties and environments of dark matter halos","arxiv_id":"1007.0612","primary_cat":"astro-ph.CO","submitted_at":"2010-07-05T03:39:56+00:00","version_compiled":"v4"},"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 v4","sentences":[{"i":0,"p":0.87,"id":"s0","own":true,"role":"contribution","text":"We use seven high-resolution $N$-body simulations to study the correlations among different halo properties (assembly time, spin, shape and substructure), and how these halo properties are correlated with the large-scale environment in which halos reside.","hedge":{"p":0.8,"label":"asserted"},"own_p":0.96,"main_claim_p":0.05,"quantitative":true,"quantitative_p":0.72,"role_probabilities":{"gap":0.0,"method":0.13,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.87,"interpretation":0.0}},{"i":1,"p":1.0,"id":"s1","own":true,"role":"method","text":"The large-scale tidal field estimated from halos above a mass threshold is used as our primary quantity to characterize the large-scale environment, while other parameters, such as the local overdensity and the morphology of large-scale structure, are used for comparison.","hedge":{"p":0.97,"label":"asserted"},"own_p":0.92,"main_claim_p":0.04,"quantitative":false,"quantitative_p":0.16,"role_probabilities":{"gap":0.0,"method":1.0,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":2,"p":1.0,"id":"s2","own":true,"role":"result","text":"For halos at a fixed mass, all the halo properties depend significantly on environment, particularly the tidal field.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.92,"main_claim_p":0.54,"quantitative":false,"quantitative_p":0.2,"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":3,"p":0.91,"id":"s3","own":true,"role":"result","text":"The environmental dependence of halo assembly time is primarily driven by local tidal field.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.92,"main_claim_p":0.16,"quantitative":false,"quantitative_p":0.09,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.91,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.09}},{"i":4,"p":1.0,"id":"s4","own":true,"role":"result","text":"The mass of the unbound fraction in substructure is boosted in strong tidal force region, while the bound fraction is suppressed.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.9,"main_claim_p":0.06,"quantitative":true,"quantitative_p":0.64,"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 have a tendency to spin faster in stronger tidal field and the trend is stronger for more massive halos.","hedge":{"p":0.95,"label":"asserted"},"own_p":0.93,"main_claim_p":0.09,"quantitative":true,"quantitative_p":0.72,"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":0.98,"id":"s6","own":true,"role":"result","text":"The spin vectors show significant alignment with the intermediate axis of the tidal field, as expected from the tidal torque theory.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.87,"main_claim_p":0.07,"quantitative":false,"quantitative_p":0.15,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.98,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.02}},{"i":7,"p":1.0,"id":"s7","own":true,"role":"result","text":"Both the major and minor axes of halos are strongly aligned with the corresponding principal axes of the tidal field.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.92,"main_claim_p":0.09,"quantitative":false,"quantitative_p":0.31,"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":0.99,"id":"s8","own":true,"role":"result","text":"In general, a halo that can accrete more material after the formation of its main halo on average is younger, is more elongated, spins faster, and contains a larger amount of substructure.","hedge":{"p":0.88,"label":"asserted"},"own_p":0.9,"main_claim_p":0.15,"quantitative":true,"quantitative_p":0.7,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.99,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.01}},{"i":9,"p":0.84,"id":"s9","own":true,"role":"interpretation","text":"Higher density environments not only provide more material for halo to accrete, but also are places of stronger tidal field that tends to suppress halo accretion.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.63,"main_claim_p":0.13,"quantitative":false,"quantitative_p":0.44,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.16,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.84}},{"i":10,"p":0.98,"id":"s10","own":true,"role":"interpretation","text":"The environmental dependencies are the results of these two competing effects.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.65,"main_claim_p":0.15,"quantitative":false,"quantitative_p":0.12,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.02,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.98}},{"i":11,"p":0.91,"id":"s11","own":true,"role":"interpretation","text":"The tidal field based on halos can be estimated from observation, and we discuss the implications of our results for the environmental dependence of galaxy 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