The coevolution of supermassive black holes and massive galaxies at high redshift

Lapi, A., Raimundo, S., Aversa, R., Cai, Z.-Y., Negrello, M. ORCID: https://orcid.org/0000-0002-7925-7663, Celotti, A., De Zotti, G. and Danese, L. 2014. The coevolution of supermassive black holes and massive galaxies at high redshift. Astrophysical Journal 782 (2) , 69. 10.1088/0004-637X/782/2/69

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Abstract

We exploit the recent, wide samples of far-infrared (FIR) selected galaxies followed up in X-rays and of X-ray/optically selected active galactic nuclei (AGNs) followed up in the FIR band, along with the classic data on AGNs and stellar luminosity functions at high redshift z gsim 1.5, to probe different stages in the coevolution of supermassive black holes (BHs) and host galaxies. The results of our analysis indicate the following scenario: (1) the star formation in the host galaxy proceeds within a heavily dust-enshrouded medium at an almost constant rate over a timescale lesssim 0.5-1 Gyr and then abruptly declines due to quasar feedback, over the same timescale; (2) part of the interstellar medium loses angular momentum, reaches the circum-nuclear regions at a rate proportional to the star formation, and is temporarily stored in a massive reservoir/proto-torus wherefrom it can be promptly accreted; (3) the BH grows by accretion in a self-regulated regime with radiative power that can slightly exceed the Eddington limit L/L Edd lesssim 4, particularly at the highest redshifts; (4) for massive BHs, the ensuing energy feedback at its maximum exceeds the stellar one and removes the interstellar gas, thus stopping the star formation and the fueling of the reservoir; (5) afterward, if the latter has retained enough gas, a phase of supply-limited accretion follows, exponentially declining with a timescale of about two e-folding times. We also discuss how the detailed properties and the specific evolution of the reservoir can be investigated via coordinated, high-resolution observations of star-forming, strongly lensed galaxies in the (sub-)mm band with ALMA and in the X-ray band with Chandra and the next-generation X-ray instruments.

Item Type:	Article
Date Type:	Publication
Status:	Published
Schools:	Physics and Astronomy
Subjects:	Q Science > QC Physics
Publisher:	American Astronomical Society
ISSN:	0004-637X
Date of First Compliant Deposit:	6 July 2020
Date of Acceptance:	12 December 2013
Last Modified:	05 May 2023 23:14
URI:	https://orca.cardiff.ac.uk/id/eprint/84005

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