Probing black hole accretion tracks, scaling relations, and radiative efficiencies from stacked X-ray active galactic nuclei

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dc.contributor.authorShankar, Francesco
dc.contributor.authorWeinberg, David H.
dc.contributor.authorMarsden, Christopher
dc.contributor.authorGrylls, Philip J.
dc.contributor.authorBernardi, Mariangela
dc.contributor.authorYang, Guang
dc.contributor.authorMoster, Benjamin
dc.contributor.authorFu, Hao
dc.contributor.authorCarraro, Rosamaria
dc.contributor.authorAlexander, David M.
dc.contributor.authorAllevato, Viola
dc.contributor.authorAnanna, Tonima T.
dc.contributor.authorBongiorno, Angela
dc.contributor.authorCalderone, Giorgio
dc.contributor.authorCivano, Francesca
dc.contributor.authorDaddi, Emanuele
dc.contributor.authorDelvecchio, Ivan
dc.contributor.authorDuras, Federica
dc.contributor.authorLa Franca, Fabio
dc.contributor.authorLapi, Andrea
dc.contributor.authorLu, Youjun
dc.contributor.authorMenci, Nicola
dc.contributor.authorMezcua, Mar
dc.contributor.authorRicci, Federica
dc.contributor.authorRodighiero, Giulia
dc.contributor.authorSheth, Ravi K.
dc.contributor.authorSuh, Hyewon
dc.contributor.authorVillforth, Carolin
dc.contributor.authorZanisi, Lorenzo
dc.date.accessioned2025-01-23T19:46:06Z
dc.date.available2025-01-23T19:46:06Z
dc.date.issued2020
dc.description.abstractThe masses of supermassive black holes at the centres of local galaxies appear to be tightly correlated with the mass and velocity dispersions of their galactic hosts. However, the local M-bh-M-star relation inferred from dynamically measured inactive black holes is up to an order-of-magnitude higher than some estimates from active black holes, and recent work suggests that this discrepancy arises from selection bias on the sample of dynamical black hole mass measurements. In this work, we combine X-ray measurements of the mean black hole accretion luminosity as a function of stellar mass and redshift with empirical models of galaxy stellar mass growth, integrating over time to predict the evolving M-bh-M-star relation. The implied relation is nearly independent of redshift, indicating that stellar and black hole masses grow, on average, at similar rates. Matching the de-biased local M-bh-M-star relation requires a mean radiative efficiency epsilon greater than or similar to 0.15, in line with theoretical expectations for accretion on to spinning black holes. However, matching the 'raw' observed relation for inactive black holes requires epsilon similar to 0.02, far below theoretical expectations. This result provides independent evidence for selection bias in dynamically estimated black hole masses, a conclusion that is robust to uncertainties in bolometric corrections, obscured active black hole fractions, and kinetic accretion efficiency. For our fiducial assumptions, they favour moderate-to-rapid spins of typical supermassive black holes, to achieve epsilon similar to 0.12-0.20. Our approach has similarities to the classic Soltan analysis, but by using galaxy-based data instead of integrated quantities we are able to focus on regimes where observational uncertainties are minimized.
dc.fuente.origenWOS
dc.identifier.doi10.1093/mnras/stz3522
dc.identifier.eissn1365-2966
dc.identifier.issn0035-8711
dc.identifier.urihttps://doi.org/10.1093/mnras/stz3522
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/100263
dc.identifier.wosidWOS:000518156100112
dc.issue.numero1
dc.language.isoen
dc.pagina.final1511
dc.pagina.inicio1500
dc.revistaMonthly notices of the royal astronomical society
dc.rightsacceso restringido
dc.subjectblack hole physics
dc.subjectgalaxies: fundamental parameters
dc.subjectgalaxies: nuclei quasars: supermassive black holes
dc.subjectgalaxies: star formation
dc.titleProbing black hole accretion tracks, scaling relations, and radiative efficiencies from stacked X-ray active galactic nuclei
dc.typeartículo
dc.volumen493
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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