{"paper":{"title":"On the fundamental dichotomy in the local radio-AGN population: accretion, evolution, and host galaxy properties","arxiv_id":"1201.2397","primary_cat":"astro-ph.CO","submitted_at":"2012-01-11T20:32:26+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":0.79,"id":"s0","own":true,"role":"method","text":"A sample of 18286 radio-loud AGN is presented, constructed by combining the SDSS DR7 with the NVSS and FIRST radio surveys.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.91,"main_claim_p":0.02,"quantitative":true,"quantitative_p":0.97,"role_probabilities":{"gap":0.0,"method":0.79,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.21,"interpretation":0.0}},{"i":1,"p":0.87,"id":"s1","own":true,"role":"contribution","text":"Using this sample, the differences between `high-excitation' (or `quasar-mode'; HERG) and `low-excitation' (`radio-mode'; LERG) radio galaxies are investigated.","hedge":{"p":0.7,"label":"asserted"},"own_p":0.85,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.12,"role_probabilities":{"gap":0.0,"method":0.1,"result":0.0,"background":0.03,"limitation":0.0,"future_work":0.0,"contribution":0.87,"interpretation":0.0}},{"i":2,"p":1.0,"id":"s2","own":true,"role":"result","text":"A primary difference is the distinct nature of the Eddington-scaled accretion rate onto their central black holes: HERGs typically have accretion rates between 1 and 10% of Eddington, whereas LERGs predominatly accrete at a rate below 1% Eddington.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.8,"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":3,"p":1.0,"id":"s3","own":false,"role":"interpretation","text":"This is consistent with models where the population dichotomy is caused by a switch between radiatively efficient and inefficient accretion modes at low accretion rates.","hedge":{"p":0.99,"label":"hedged_possibility"},"own_p":0.16,"main_claim_p":0.17,"quantitative":false,"quantitative_p":0.07,"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":4,"p":1.0,"id":"s4","own":true,"role":"result","text":"Local radio luminosity functions are derived separately for the two populations, showing that although LERGs dominate at low luminosity and HERGs above 1e26 W/Hz, examples of both classes are found at all radio luminosities.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.96,"main_claim_p":0.08,"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":5,"p":0.99,"id":"s5","own":true,"role":"result","text":"Using the V/Vmax test it is shown that the populations show differential cosmic evolution at fixed radio luminosity: HERGs evolve strongly at all luminosities, while LERGs show weak or no evolution.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.95,"main_claim_p":0.12,"quantitative":true,"quantitative_p":0.85,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.99,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.01,"interpretation":0.0}},{"i":6,"p":1.0,"id":"s6","own":true,"role":"interpretation","text":"This suggests that the luminosity-dependent evolution of the radio luminosity function is driven, at least in part, by the changing relative contributions of these two populations with luminosity.","hedge":{"p":1.0,"label":"hedged_possibility"},"own_p":0.78,"main_claim_p":0.16,"quantitative":false,"quantitative_p":0.13,"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":1.0,"id":"s7","own":true,"role":"result","text":"The host galaxies of the sources are also distinct: HERGs are typically of lower stellar mass, with lower black hole masses, bluer colours and weaker 4000-Ang breaks indicating younger stellar populations.","hedge":{"p":0.98,"label":"asserted"},"own_p":0.87,"main_claim_p":0.06,"quantitative":true,"quantitative_p":0.81,"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":1.0,"id":"s8","own":false,"role":"interpretation","text":"These results offer strong support to the picture in which HERGs are fuelled at high rates through radiative accretion disks by cold gas, perhaps from mergers and interactions, while LERGs are fuelled via radiatively inefficient flows at low accretion rates, often by gas associated with the hot X-ray haloes of their host galaxy/cluster, as part of a radio-AGN feedback loop (abridged).","hedge":{"p":0.73,"label":"hedged_possibility"},"own_p":0.47,"main_claim_p":0.7,"quantitative":false,"quantitative_p":0.19,"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}}]},"compiled":{"main_claim":{"p":0.97,"text":"These results offer strong support to the picture in which HERGs are fuelled at high rates through radiative accretion disks by cold gas, perhaps from mergers and interactions, while LERGs are fuelled via radiatively inefficient flows at low accretion rates, often by gas associated with the hot X-ray haloes of their host galaxy/cluster, as part of a radio-AGN feedback loop (abridged).","location":"abstract s8","hedge_strength":{"p":0.73,"label":"hedged possibility"}},"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":7391,"cost_usd_reported":0.00031},"compiled_at":"2026-09-23","bank_version":"abstract-p1-20260923","model_version":"classifier-1.13-20260917","abstract_states":{"claims_first":0.02,"states_limitation":0.22,"human_participants":0.01,"controlled_comparison":0.23,"randomized_assignment":0.01,"states_quantitative_result":0.98,"compares_with_prior_results":0.21,"mentions_code_or_data_availability":0.02},"evidential_basis":{"p":1.0,"value":"analysis of existing data","probabilities":{"argument":0.0,"literature":0.0,"proof_or_derivation":0.0,"analysis_of_existing_data":1.0,"observation_or_experiment":0.0,"simulation_or_computation":0.0}},"contribution_type":{"p":0.99,"value":"empirical study","probabilities":{"review":0.0,"method_or_tool":0.0,"empirical_study":0.99,"simulation_study":0.0,"theoretical_result":0.0,"dataset_or_benchmark":0.01,"position_or_commentary":0.0}},"contribution_statement":{"p":0.79,"text":"A sample of 18286 radio-loud AGN is presented, constructed by combining the SDSS DR7 with the NVSS and FIRST radio surveys.","location":"abstract s0"}},"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}}