{"paper":{"title":"The Link Between the Hidden Broad Line Region and the Accretion Rate in Seyfert 2 Galaxies","arxiv_id":"1201.5397","primary_cat":"astro-ph.CO","submitted_at":"2012-01-25T21:22:40+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":"In the past few years more and more pieces of evidence have been presented for a revision of the widely accepted Unified Model of Active Galactic Nuclei.","hedge":{"p":0.98,"label":"asserted"},"own_p":0.04,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.17,"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":0.76,"id":"s1","own":false,"role":"background","text":"A model based solely on orientation cannot explain all the observed phenomenology.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.07,"main_claim_p":0.04,"quantitative":false,"quantitative_p":0.05,"role_probabilities":{"gap":0.24,"method":0.0,"result":0.0,"background":0.76,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":2,"p":0.96,"id":"s2","own":false,"role":"contribution","text":"In the following, we will present evidence that accretion rate is also a key parameter for the presence of Hidden Broad Line Regions in Seyfert 2 galaxies.","hedge":{"p":0.81,"label":"asserted"},"own_p":0.33,"main_claim_p":0.7,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.01,"method":0.0,"result":0.01,"background":0.0,"limitation":0.0,"future_work":0.02,"contribution":0.96,"interpretation":0.0}},{"i":3,"p":0.85,"id":"s3","own":true,"role":"method","text":"Our sample consists of 21 sources with polarized Hidden Broad Lines and 18 sources without Hidden Broad Lines.","hedge":{"p":0.96,"label":"asserted"},"own_p":0.79,"main_claim_p":0.02,"quantitative":true,"quantitative_p":0.98,"role_probabilities":{"gap":0.0,"method":0.85,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.15,"interpretation":0.0}},{"i":4,"p":1.0,"id":"s4","own":true,"role":"method","text":"We use stellar velocity dispersions from several studies on the CaII and Mg b triplets in Seyfert 2 galaxies, to estimate the mass of the central black holes via the Mbh-{\\sigma}\\ast relation.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.73,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.19,"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":5,"p":0.87,"id":"s5","own":false,"role":"method","text":"The ratio between the bolometric luminosity, derived from the intrinsic (i.e. unabsorbed) X-ray luminosity, and the Eddington luminosity is a measure of the rate at which matter accretes onto the central supermassive black hole.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.19,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.06,"role_probabilities":{"gap":0.0,"method":0.87,"result":0.0,"background":0.12,"limitation":0.0,"future_work":0.0,"contribution":0.01,"interpretation":0.0}},{"i":6,"p":1.0,"id":"s6","own":true,"role":"result","text":"A separation between Compton-thin HBLR and non-HBLR sources is clear, both in accretion rate (log Lbol/LEdd = -1.9) and in luminosity (log Lbol = 43.90).","hedge":{"p":1.0,"label":"asserted"},"own_p":0.9,"main_claim_p":0.44,"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":0.98,"id":"s7","own":true,"role":"result","text":"When, properly luminosity-corrected, Compton-thick sources are included, the separation between HBLR and non-HBLR is less sharp but no HBLR source falls below the Eddington ratio threshold.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.88,"main_claim_p":0.19,"quantitative":true,"quantitative_p":0.7,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.98,"background":0.0,"limitation":0.01,"future_work":0.0,"contribution":0.0,"interpretation":0.01}},{"i":8,"p":1.0,"id":"s8","own":false,"role":"interpretation","text":"We speculate that non-HBLR Compton-thick sources with accretion rate higher than the threshold, do possess a BLR, but something, probably related to their heavy absorption, is preventing us from observing it even in polarized light.","hedge":{"p":1.0,"label":"speculative"},"own_p":0.31,"main_claim_p":0.12,"quantitative":false,"quantitative_p":0.34,"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":9,"p":0.89,"id":"s9","own":true,"role":"interpretation","text":"Our results for Compton-thin sources support theoretical expectations.","hedge":{"p":0.89,"label":"asserted"},"own_p":0.76,"main_claim_p":0.09,"quantitative":false,"quantitative_p":0.06,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.11,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.89}},{"i":10,"p":0.6,"id":"s10","own":false,"role":"interpretation","text":"In a model presented by Nicastro (2000), the presence of broad emission lines is intrinsically connected with disk instabilities occuring in proximity of a transition radius, which is a function of the accretion rate, becoming smaller than the innermost stable orbit for very low accretion rates and therefore luminosities.","hedge":{"p":0.87,"label":"asserted"},"own_p":0.04,"main_claim_p":0.07,"quantitative":false,"quantitative_p":0.36,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":0.4,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.6}}]},"compiled":{"main_claim":{"p":0.76,"text":"In the following, we will present evidence that accretion rate is also a key parameter for the presence of Hidden Broad Line Regions in Seyfert 2 galaxies.","location":"abstract s2","hedge_strength":{"p":0.81,"label":"asserted"}},"provenance":{"route":{"via":"OpenRouter","model":"classifier-1.13","endpoint":"https://openrouter.ai/api/v1/systemone","provider":"TypeSafe"},"packing":"one request per 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