Zanisi, Lorenzo and Villforth, Carolin and Suh, Hyewon and Sheth, Ravi K. and Rodighiero, Giulia and Ricci, Federica and Mezcua, Mar and Menci, Nicola and Lu, Youjun and Lapi, Andrea and La Franca, Fabio and Duras, Federica and Delvecchio, Ivan and Daddi, Emanuele and Civano, Francesca and Calderone, Giorgio and Bongiorno, Angela and Ananna, Tonima T. and Allevato, Viola and Alexander, David M. and Carraro, Rosamaria and Fu, Hao and Moster, Benjamin and Yang, Guang and Bernardi, Mariangela and Grylls, Philip J. and Marsden, Christopher and Weinberg, David H. and Shankar, Francesco (2020) 'Probing black hole accretion tracks, scaling relations, and radiative efficiencies from stacked X-ray active galactic nuclei.', Monthly notices of the Royal Astronomical Society., 493 (1). pp. 1500-1511.
The 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 Mbh–Mstar 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 Mbh–Mstar 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 Mbh–Mstar relation requires a mean radiative efficiency ε ≳ 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 ε ∼ 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 ε ∼ 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.
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|Publisher Web site:||https://doi.org/10.1093/mnras/stz3522|
|Publisher statement:||This article has been accepted for publication in Monthly notices of the Royal Astronomical Society. ©: 2020 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.|
|Date accepted:||09 December 2019|
|Date deposited:||04 November 2020|
|Date of first online publication:||16 December 2019|
|Date first made open access:||04 November 2020|
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