Cookies

We use cookies to ensure that we give you the best experience on our website. By continuing to browse this repository, you give consent for essential cookies to be used. You can read more about our Privacy and Cookie Policy.


Durham Research Online
You are in:

The evolution of SMBH spin and AGN luminosities for z < 6 within a semi-analytic model of galaxy formation.

Griffin, Andrew J. and Lacey, Cedric G. and Gonzalez-Perez, Violeta and del P Lagos, Claudia and Baugh, Carlton M. and Fanidakis, Nikos (2019) 'The evolution of SMBH spin and AGN luminosities for z < 6 within a semi-analytic model of galaxy formation.', Monthly notices of the Royal Astronomical Society., 487 (1). pp. 198-227.

Abstract

Understanding how Active Galactic Nuclei (AGN) evolve through cosmic time allows us to probe the physical processes that control their evolution. We use an updated model for the evolution of masses and spins of supermassive black holes (SMBHs), coupled to the latest version of the semi-analytical model of galaxy formation GALFORM using the Planck cosmology and a high resolution Millennium style dark matter simulation to make predictions for AGN and SMBH properties for 0 < z < 6. We compare the model to the observed black hole mass function and the SMBH versus galaxy bulge mass relation at z = 0, and compare the predicted bolometric, hard X-ray, soft X-ray and optical AGN luminosity functions to observations at z < 6, and find that the model is in good agreement with the observations. The model predicts that at z < 2 and Lbol < 1043ergs−1, the AGN luminosity function is dominated by objects accreting in an Advection Dominated Accretion Flow (ADAF) disc state, while at higher redshifts and higher luminosities the dominant contribution is from objects accreting via a thin disc or at super-Eddington rates. The model also predicts that the AGN luminosity function at z < 3 and Lbol < 1044ergs−1 is dominated by the contribution from AGN fuelled by quiescent hot halo accretion, while at higher luminosities and higher redshifts, the AGN luminosity function is dominated by the contribution from AGN fuelled by starbursts triggered by disc instabilities. We employ this model to predict the evolution of SMBH masses, Eddington ratios, and spins, finding that the median SMBH spin evolves very little for 0 < z < 6.

Item Type:Article
Full text:(AM) Accepted Manuscript
Download PDF
(1915Kb)
Full text:(VoR) Version of Record
Download PDF
(12599Kb)
Status:Peer-reviewed
Publisher Web site:https://doi.org/10.1093/mnras/stz1216
Publisher statement:© 2019 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society.
Date accepted:30 April 2019
Date deposited:07 May 2019
Date of first online publication:04 May 2019
Date first made open access:No date available

Save or Share this output

Export:
Export
Look up in GoogleScholar