{"paper":{"title":"An Accurate Comprehensive Approach to Substructure: I. Accreted Subhaloes","arxiv_id":"2109.06484","primary_cat":"astro-ph.CO","submitted_at":"2021-09-14T07:29:45+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-1.13.0 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":0.88,"id":"s0","own":false,"role":"background","text":"This is the first of a series of three Papers devoted to the study of halo substructure in hierarchical cosmologies by means of the CUSP formalism.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.3,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.32,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":0.88,"limitation":0.0,"future_work":0.05,"contribution":0.07,"interpretation":0.0}},{"i":1,"p":1.0,"id":"s1","own":true,"role":"contribution","text":"In the present Paper we derive the properties of subhaloes and diffuse dark matter (dDM) accreted onto haloes and their progenitors.","hedge":{"p":0.95,"label":"asserted"},"own_p":0.95,"main_claim_p":0.06,"quantitative":false,"quantitative_p":0.03,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":1.0,"interpretation":0.0}},{"i":2,"p":0.95,"id":"s2","own":true,"role":"contribution","text":"Specifically, we relate the dDM present at any time in the inter-halo medium of the real Universe or a cosmological simulation with the corresponding free-streaming mass or the halo resolution mass, respectively, and establish the link between subhaloes and their seeds in the initial density field.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.87,"main_claim_p":0.07,"quantitative":false,"quantitative_p":0.08,"role_probabilities":{"gap":0.0,"method":0.05,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.95,"interpretation":0.0}},{"i":3,"p":0.75,"id":"s3","own":true,"role":"method","text":"By monitoring the collapse and virialisation of haloes, we derive from first principles and with no single free parameter the abundance and radial distribution of dDM and subhaloes accreted onto them.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.97,"main_claim_p":0.2,"quantitative":false,"quantitative_p":0.12,"role_probabilities":{"gap":0.0,"method":0.75,"result":0.07,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.18,"interpretation":0.0}},{"i":4,"p":0.96,"id":"s4","own":true,"role":"result","text":"Our predictions are in excellent agreement with the results of simulations, but for the predicted fraction of accreted dDM, which is larger than reported in previous works as they only count the dDM accreted onto the final halo, not onto its progenitors.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.86,"main_claim_p":0.19,"quantitative":true,"quantitative_p":0.92,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.96,"background":0.0,"limitation":0.03,"future_work":0.0,"contribution":0.0,"interpretation":0.01}},{"i":5,"p":1.0,"id":"s5","own":true,"role":"interpretation","text":"The derivation pursued here clarifies the origin of some key features of substructure.","hedge":{"p":0.97,"label":"asserted"},"own_p":0.79,"main_claim_p":0.12,"quantitative":false,"quantitative_p":0.02,"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":6,"p":0.97,"id":"s6","own":true,"role":"interpretation","text":"Overall, our results demonstrate that CUSP is a powerful tool for understanding halo substructure and extending the results of simulations to haloes with arbitrary masses, redshifts and formation times in any hierarchical 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