{"paper":{"title":"X-ray binary accretion states in Active Galactic Nuclei? Sensing the accretion disc of supermassive black holes with mid-infrared nebular lines","arxiv_id":"2104.09538","primary_cat":"astro-ph.HE","submitted_at":"2021-04-19T18:00:56+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-1.13.0 on the question bank abstract-p1-20260923, exactly as returned. 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populations.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.07,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.29,"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":2,"p":0.71,"id":"s2","own":false,"role":"gap","text":"Previous attempts to extend this framework to a wider AGN population have been extremely challenging due to heavy hydrogen absorption of the accretion disc continuum and starlight contamination from the host galaxies.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.04,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.07,"role_probabilities":{"gap":0.71,"method":0.0,"result":0.0,"background":0.29,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":3,"p":0.58,"id":"s3","own":true,"role":"method","text":"We present the luminosity-excitation diagram (LED), based on the [OIV]$_{25.9\\mu m}$ and [NeII]$_{12.8\\mu m}$ mid-infrared nebular line fluxes.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.96,"main_claim_p":0.05,"quantitative":false,"quantitative_p":0.1,"role_probabilities":{"gap":0.0,"method":0.58,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.42,"interpretation":0.0}},{"i":4,"p":0.59,"id":"s4","own":true,"role":"method","text":"This tool enables to probe the accretion disc contribution to the ionising continuum.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.55,"main_claim_p":0.06,"quantitative":false,"quantitative_p":0.03,"role_probabilities":{"gap":0.0,"method":0.59,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.4,"interpretation":0.01}},{"i":5,"p":0.98,"id":"s5","own":true,"role":"result","text":"When applied to a sample of 167 nearby AGN, the LED recovers the characteristic q-shaped morphology outlined by individual X-ray binaries during a typical accretion episode, allowing us to tentatively identify the main accretion states.","hedge":{"p":0.55,"label":"asserted"},"own_p":0.95,"main_claim_p":0.68,"quantitative":true,"quantitative_p":0.96,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.98,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.02}},{"i":6,"p":0.81,"id":"s6","own":true,"role":"interpretation","text":"The soft state would include broad-line Seyferts and about half of the Seyfert 2 population, showing highly excited gas and radio-quiet cores consistent with disc-dominated nuclei.","hedge":{"p":0.77,"label":"asserted"},"own_p":0.78,"main_claim_p":0.13,"quantitative":true,"quantitative_p":0.6,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.19,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.81}},{"i":7,"p":0.71,"id":"s7","own":true,"role":"interpretation","text":"The hard state mostly includes low-luminosity AGN ($\\leq 10^{-3}\\, \\rm{L_{Edd}}$) characterised by low-excitation radio-loud nuclei and a negligible disc contribution.","hedge":{"p":0.98,"label":"asserted"},"own_p":0.77,"main_claim_p":0.1,"quantitative":true,"quantitative_p":0.98,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.29,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.71}},{"i":8,"p":0.84,"id":"s8","own":true,"role":"interpretation","text":"The remaining half of Seyfert 2 nuclei and the bright LINERs show low excitation at high accretion luminosities, and could be identified with the bright-hard and intermediate states.","hedge":{"p":0.99,"label":"hedged_possibility"},"own_p":0.81,"main_claim_p":0.1,"quantitative":true,"quantitative_p":0.66,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.16,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.84}},{"i":9,"p":0.81,"id":"s9","own":true,"role":"result","text":"Their hosts show ongoing star formation in the central kiloparsecs.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.7,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.07,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.81,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.19}},{"i":10,"p":0.8,"id":"s10","own":false,"role":"interpretation","text":"We discuss the above scenario, its potential links with the galaxy evolution picture and the possible presence of accretion state transitions in AGN, as suggested by the growing population of changing-look quasars.","hedge":{"p":0.88,"label":"hedged_possibility"},"own_p":0.37,"main_claim_p":0.06,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.19,"contribution":0.01,"interpretation":0.8}}]},"compiled":{"main_claim":{"p":1.0,"text":"When applied to a sample of 167 nearby AGN, the LED recovers the characteristic q-shaped morphology outlined by 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