Dependence of the Spin of Supermassive Black Holes on the Eddington Factor for Accretion Disks in Active Galactic Nuclei

Piotrovich, M. Yu.; Buliga, S. D.; Gnedin, Yu. N.; Михайлов, А. Г.; Natsvlishvili, T. M.

doi:10.1007/s10511-016-9447-4

Cited by 2 publications

(1 citation statement)

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“…There have been various attempts to indirectly estimate SMBH spins, e.g. from the Eddington factor of accretion discs (Piotrovich et al 2016) or jet properties (Kun et al 2013;Mościbrodzka et al 2016;Daly 2009;Daly & Sprinkle 2014;Daly 2016Daly , 2019. Evolution of the SMBH population over cosmic time also provides constraints on the radiative efficiency, which appears to be low (Soltan 1982;Merloni & Heinz 2008;Davies et al 2019), implying low spin values, but this estimate is degenerate with SMBH mass density and/or obscuration (Davies et al 2019).…”

Section: Discussion and Summarymentioning

confidence: 99%

Slow and massive: low-spin SMBHs can grow more

Zubovas

King

2019

Monthly Notices of the Royal Astronomical Society

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Active galactic nuclei (AGN) probably control the growth of their host galaxies via feedback in the form of wide-angle wind-driven outflows. These establish the observed correlations between supermassive black hole (SMBH) masses and host galaxy properties, e.g. the spheroid velocity dispersion σ. In this paper we consider the growth of the SMBH once it starts driving a large-scale outflow through the galaxy. To clear the gas and ultimately terminate further growth of both the SMBH and the host galaxy, the black hole must continue to grow its mass significantly, by up to a factor of a few, after reaching this point. The mass increment ∆M BH depends sensitively on both galaxy size and SMBH spin. The galaxy size dependence leads to ∆M BH ∝ σ 5 and a steepening of the M − σ relation beyond the analytically calculated M ∝ σ 4 , in agreement with observation. Slowly-spinning black holes are much less efficient in producing feedback, so at any given σ the slowest-spinning black holes should be the most massive. Current observational constraints are consistent with this picture, but insufficient to test it properly; however, this should change with upcoming surveys.

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