{"paper":{"title":"On the Outskirts of Dark Matter Haloes","arxiv_id":"2210.11499","primary_cat":"astro-ph.CO","submitted_at":"2022-10-20T18:02:45+00:00","version_compiled":"v3"},"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 v3","sentences":[{"i":0,"p":1.0,"id":"s0","own":false,"role":"background","text":"Halo Models of large scale structure provide powerful and indispensable tools for phenomenological understanding of the clustering of matter in the Universe.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.04,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.03,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":1.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":1,"p":0.84,"id":"s1","own":false,"role":"gap","text":"While the halo model builds structures out of the superposition of haloes, defining halo profiles in their outskirts - beyond their virial radii - becomes increasingly ambiguous, as one cannot assign matter to individual haloes in a clear way.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.06,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.15,"role_probabilities":{"gap":0.84,"method":0.0,"result":0.0,"background":0.16,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":2,"p":0.73,"id":"s2","own":true,"role":"contribution","text":"In this paper, we tackle this question by using numerical N-body simulations to find a systematic definition of mean halo profile that can be extended to large radii.","hedge":{"p":0.91,"label":"asserted"},"own_p":0.91,"main_claim_p":0.05,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.0,"method":0.27,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.73,"interpretation":0.0}},{"i":3,"p":0.56,"id":"s3","own":false,"role":"background","text":"These profiles must be compensated and are the key ingredients for the computation of cosmological correlation functions in the Amended Halo Model.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.23,"main_claim_p":0.07,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.0,"method":0.01,"result":0.02,"background":0.56,"limitation":0.0,"future_work":0.0,"contribution":0.1,"interpretation":0.3}},{"i":4,"p":0.9,"id":"s4","own":false,"role":"background","text":"The latter, introduced in our earlier work (arXiv:1912.04872), provides a more physically accurate phenomenological description of nonlinear structure formation, which respects conservation laws on large scales.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.33,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.42,"role_probabilities":{"gap":0.0,"method":0.02,"result":0.0,"background":0.9,"limitation":0.0,"future_work":0.0,"contribution":0.06,"interpretation":0.02}},{"i":5,"p":0.94,"id":"s5","own":true,"role":"contribution","text":"Here, we extend this model from the matter auto-power spectrum to the halo-matter cross-power spectra, using N-body simulations.","hedge":{"p":0.93,"label":"asserted"},"own_p":0.9,"main_claim_p":0.04,"quantitative":false,"quantitative_p":0.08,"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":6,"p":1.0,"id":"s6","own":true,"role":"result","text":"We find that the (dimensionless) compensated halo profile, $r^3 \\times \\rho(r)/M_{200c}$ has a near-universal maximum in the small range $0.03-0.04$ around the virial radius, $r \\simeq r_{\\rm 200c}$, independent of the halo mass.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.97,"main_claim_p":0.6,"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":7,"p":1.0,"id":"s7","own":true,"role":"result","text":"The profiles cross zero into negative values in the halo outskirts, beyond 2-3$\\times r_{\\rm 200c}$, consistent with our previous results.","hedge":{"p":0.55,"label":"hedged_possibility"},"own_p":0.86,"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":8,"p":0.86,"id":"s8","own":true,"role":"contribution","text":"We provide preliminary fitting functions for compensated Navarro-Frenk-White (NFW) profiles, and this can be used to compute more physical observables in the Amended Halo Model of large scale structure.","hedge":{"p":0.53,"label":"asserted"},"own_p":0.92,"main_claim_p":0.16,"quantitative":false,"quantitative_p":0.05,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.07,"background":0.0,"limitation":0.01,"future_work":0.05,"contribution":0.86,"interpretation":0.01}}]},"compiled":{"main_claim":{"p":0.98,"text":"We find that the (dimensionless) compensated halo profile, $r^3 \\times \\rho(r)/M_{200c}$ 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