{"paper":{"title":"A self-consistent phase-space distribution function for the anisotropic Dark Matter halo of the Milky Way","arxiv_id":"1311.5477","primary_cat":"astro-ph.CO","submitted_at":"2013-11-21T16:57:51+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":1.0,"id":"s0","own":false,"role":"background","text":"Dark Matter (DM) direct detection experiments usually assume the simplest possible 'Standard Halo Model' for the Milky Way (MW) halo in which the velocity distribution is Maxwellian.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.04,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.08,"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":0.87,"id":"s1","own":false,"role":"background","text":"This model assumes that the MW halo is an isotropic, isothermal sphere, hypotheses that are unlikely to be valid in reality.","hedge":{"p":0.7,"label":"hedged_possibility"},"own_p":0.05,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.06,"role_probabilities":{"gap":0.12,"method":0.0,"result":0.0,"background":0.87,"limitation":0.01,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":2,"p":0.97,"id":"s2","own":false,"role":"background","text":"An alternative approach is to derive a self-consistent solution for a particular mass model of the MW (i.e. obtained from its gravitational potential) using the Eddington formalism, which assumes isotropy.","hedge":{"p":0.94,"label":"asserted"},"own_p":0.06,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.05,"role_probabilities":{"gap":0.01,"method":0.02,"result":0.0,"background":0.97,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":3,"p":0.99,"id":"s3","own":true,"role":"contribution","text":"In this paper we extend this approach to incorporate an anisotropic phase-space distribution function.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.89,"main_claim_p":0.06,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.0,"method":0.01,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.99,"interpretation":0.0}},{"i":4,"p":0.95,"id":"s4","own":true,"role":"method","text":"We perform Bayesian scans over the parameters defining the mass model of the MW and parameterising the phase-space density, implementing constraints from a wide range of astronomical observations.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.96,"main_claim_p":0.04,"quantitative":false,"quantitative_p":0.06,"role_probabilities":{"gap":0.0,"method":0.95,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.05,"interpretation":0.0}},{"i":5,"p":0.47,"id":"s5","own":true,"role":"method","text":"The scans allow us to estimate the precision reached in the reconstruction of the velocity distribution (for different DM halo profiles).","hedge":{"p":0.93,"label":"asserted"},"own_p":0.9,"main_claim_p":0.07,"quantitative":false,"quantitative_p":0.09,"role_probabilities":{"gap":0.0,"method":0.47,"result":0.18,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.35,"interpretation":0.0}},{"i":6,"p":0.99,"id":"s6","own":true,"role":"result","text":"As expected, allowing for an anisotropic velocity tensor increases the uncertainty in the reconstruction of f(v) but the distribution can still be determined with a precision of a factor of 4-5.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.95,"main_claim_p":0.38,"quantitative":true,"quantitative_p":0.99,"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":7,"p":1.0,"id":"s7","own":true,"role":"result","text":"The mean velocity distribution resembles the isotropic case, however the amplitude of the high-velocity tail is up to a factor of 2 larger.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.94,"main_claim_p":0.22,"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":8,"p":0.57,"id":"s8","own":true,"role":"result","text":"Our results agree with the phenomenological parametrization proposed in Mao et al. (2013) as a good fit to N-body simulations (with or without baryons), since their velocity distribution is contained in our 68% credible interval.","hedge":{"p":0.93,"label":"asserted"},"own_p":0.75,"main_claim_p":0.22,"quantitative":true,"quantitative_p":0.97,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.57,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.43}}]},"compiled":{"main_claim":{"p":0.71,"text":"As expected, allowing for an anisotropic velocity tensor increases the uncertainty in the reconstruction of f(v) but the distribution can still be determined with a precision of a factor of 4-5.","location":"abstract s6","hedge_strength":{"p":0.99,"label":"asserted"}},"provenance":{"route":{"via":"OpenRouter","model":"classifier-1.13","endpoint":"https://openrouter.ai/api/v1/systemone","provider":"TypeSafe"},"packing":"one request per paper","requests":1,"input_tokens":7039,"cost_usd_reported":0.000296},"compiled_at":"2026-09-23","bank_version":"abstract-p1-20260923","model_version":"classifier-1.13-20260917","abstract_states":{"claims_first":0.06,"states_limitation":0.91,"human_participants":0.01,"controlled_comparison":0.23,"randomized_assignment":0.01,"states_quantitative_result":0.98,"compares_with_prior_results":0.97,"mentions_code_or_data_availability":0.02},"evidential_basis":{"p":0.67,"value":"simulation or computation","probabilities":{"argument":0.0,"literature":0.0,"proof_or_derivation":0.0,"analysis_of_existing_data":0.33,"observation_or_experiment":0.0,"simulation_or_computation":0.67}},"contribution_type":{"p":0.44,"value":"method or tool","probabilities":{"review":0.0,"method_or_tool":0.44,"empirical_study":0.0,"simulation_study":0.17,"theoretical_result":0.39,"dataset_or_benchmark":0.0,"position_or_commentary":0.0}},"contribution_statement":{"p":0.99,"text":"In this paper we extend this approach to incorporate an anisotropic phase-space distribution function.","location":"abstract s3"}},"coverage":{"tier":"abstract","levels_run":["P abstract"],"not_examined":["full text","figures and tables","references and citing sentences","relations to other papers"],"sources_read":["arXiv listing abstract v1"],"levels_not_run":["S sections","T body sentences","C citations","R cross-paper relations"],"sentences_examined":9,"sentences_in_abstract":9},"measured_accuracy":{"url":"https://pith.science/accuracy","measured_on":"2026-10-02","method":"two independent model families labelled a fresh random sample blind; the figure is how often the published label matches their consensus","sentence_role_agreement":0.92,"main_claim_agreement":0.908,"typed_citation_agreement":0.933,"typed_citation_agreement_95_interval":[0.917,0.945],"review_comments_accurate":0.758,"review_comments_accurate_95_interval":[0.684,0.82],"review_caught_admitted_error_found_or_related":0.448}}