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X-rays across the galaxy population - II. The distribution of AGN accretion rates as a function of stellar mass and redshift

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posted on 2018-05-16, 16:21 authored by J. Aird, A. L. Coil, A. Georgakakis
We use deepChandra X-ray imaging to measure the distribution of specific black hole accretion rates (LX relative to the stellar mass of the galaxy) and thus trace active galactic nucleus (AGN) activity within star-forming and quiescent galaxies, as a function of stellar mass (from 108.5 to 1011.5 M) and redshift (to z ∼ 4). We adopt near-infrared-selected samples of galaxies from the CANDELS and UltraVISTA surveys, extract X-ray data for every galaxy, and use a flexible Bayesian method to combine these data and to measure the probability distribution function of specific black hole accretion rates, λsBHAR. We identify a broad distribution of λsBHAR in both star-forming and quiescent galaxies – likely reflecting the stochastic nature of AGN fuelling – with a roughly power-law shape that rises towards lower λsBHAR, a steep cut-off at λsBHAR 0.1–1 (in Eddington equivalent units), and a turnover or flattening at λsBHAR 10−3 to 10−2. We find that the probability of a star-forming galaxy hosting a moderate λsBHAR AGN depends on stellar mass and evolves with redshift, shifting towards higher λsBHAR at higher redshifts. This evolution is truncated at a point corresponding to the Eddington limit, indicating black holes may self-regulate their growth at high redshifts when copious gas is available. The probability of a quiescent galaxy hosting an AGN is generally lower than that of a starforming galaxy, shows signs of suppression at the highest stellar masses and evolves strongly with redshift. The AGN duty cycle in high-redshift (z 2) quiescent galaxies thus reaches ∼20 per cent, comparable to the duty cycle in star-forming galaxies of equivalent stellar mass and redshift.

Funding

JA acknowledges support from ERC Advanced Grant FEEDBACK 340442. AG acknowledges the THALES project 383549 that is jointly funded by the European Union and the Greek Government in the framework of the programme ‘Education and lifelong learning’. This work is based in part on observations taken by the CANDELS Multi-Cycle Treasury Program and the 3D-HST Treasury Program (GO 12177 and 12328) with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. The scientific results reported in this article are based to a significant degree on observations made by the Chandra X-ray Observatory.

History

Citation

Monthly Notices of the Royal Astronomical Society, 2018, 474(1), pp. 1225–1249

Author affiliation

/Organisation/COLLEGE OF SCIENCE AND ENGINEERING/Department of Physics and Astronomy

Version

  • VoR (Version of Record)

Published in

Monthly Notices of the Royal Astronomical Society

Publisher

Oxford University Press (OUP), Royal Astronomical Society

issn

0035-8711

eissn

1365-2966

Acceptance date

2017-10-13

Copyright date

2017

Available date

2018-05-16

Publisher version

https://academic.oup.com/mnras/article/474/1/1225/4562631

Language

en

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