{"paper":{"title":"The black hole-galaxy correlations of the 12 micron local AGN sample: a NuSTAR perspective","arxiv_id":"2610.30285","primary_cat":"astro-ph.GA","submitted_at":"2026-10-21T18:03:35+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. 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":"The M-sigma correlation of inactive galaxies plays a crucial role in estimating the black hole mass (MBH) in active galactic nuclei (AGN): 1) it is used to calibrate the reverberation mapping (RM) method; 2) the RM is the basis of the single epoch method, the most-used technique to determine MBH of broad-line AGN; and 3) in narrow-line AGN, MBH is often directly inferred from the M-sigma correlation.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.04,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.15,"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":"contribution","text":"The main goal of this work is to test whether the M-sigma relation calibrated from inactive galaxies can be reliably applied to a local AGN population spanning Seyfert 1, Seyfert 2, and hidden broad-line region galaxies (HBLRs), and whether the resulting AGN relation has sufficient predictive power to be used as an indirect MBH estimator.","hedge":{"p":0.45,"label":"unclear"},"own_p":0.16,"main_claim_p":0.05,"quantitative":false,"quantitative_p":0.14,"role_probabilities":{"gap":0.11,"method":0.0,"result":0.0,"background":0.02,"limitation":0.0,"future_work":0.0,"contribution":0.87,"interpretation":0.0}},{"i":2,"p":0.9,"id":"s2","own":true,"role":"method","text":"To investigate this hypothesis, we used the 12 micron AGN sample, a local representative and largely unbiased sample.","hedge":{"p":0.98,"label":"asserted"},"own_p":0.6,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.09,"role_probabilities":{"gap":0.0,"method":0.9,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.1,"interpretation":0.0}},{"i":3,"p":0.99,"id":"s3","own":true,"role":"method","text":"Since a substantial fraction of this sample has good-quality NuSTAR data, we estimated their MBH with the X-ray scaling method, which works for any AGN accreting at moderate or high level.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.93,"main_claim_p":0.02,"quantitative":false,"quantitative_p":0.16,"role_probabilities":{"gap":0.0,"method":0.99,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.01,"interpretation":0.0}},{"i":4,"p":1.0,"id":"s4","own":true,"role":"result","text":"We find that the M-sigma correlation of the 12 micron AGN sample is different from the one obtained with inactive galaxies and has a substantial scatter.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.97,"main_claim_p":0.47,"quantitative":true,"quantitative_p":0.78,"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":0.86,"id":"s5","own":true,"role":"interpretation","text":"Therefore, its predictive power for MBH estimates is fairly limited.","hedge":{"p":0.97,"label":"asserted"},"own_p":0.86,"main_claim_p":0.39,"quantitative":false,"quantitative_p":0.12,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.12,"background":0.0,"limitation":0.02,"future_work":0.0,"contribution":0.0,"interpretation":0.86}},{"i":6,"p":1.0,"id":"s6","own":true,"role":"result","text":"We also find that the MBH-Mgal correlation based on the 12 micron AGN sample is consistent with the analogous correlation obtained from a large sample of nearby type 1 AGN and inconsistent with that of inactive galaxies.","hedge":{"p":0.64,"label":"asserted"},"own_p":0.95,"main_claim_p":0.13,"quantitative":true,"quantitative_p":0.74,"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":"Finally, we find suggestive evidence that Seyfert 1 and HBLRs have similar and systematically higher Eddington ratios than Seyfert 2 galaxies.","hedge":{"p":0.93,"label":"hedged_possibility"},"own_p":0.95,"main_claim_p":0.05,"quantitative":true,"quantitative_p":0.93,"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}}]},"compiled":{"main_claim":{"p":0.59,"text":"Therefore, its predictive power for MBH estimates is fairly limited.","location":"abstract s5","hedge_strength":{"p":0.97,"label":"asserted"}},"provenance":{"route":{"via":"TypeSafe 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