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Lookup NU author(s): Dr Christopher HarrisonORCiD
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© 2020 The Author(s). Studies investigating the relationship between active galactic nucleus (AGN) power and the star formation rates (SFRs) of their host galaxies often rely on averaging techniques - such as stacking - to incorporate information from non-detections. However, averages, and especially means, can be strongly affected by outliers and can therefore give a misleading indication of the 'typical' case. Recently, a number of studies have taken a step further by binning their sample in terms of AGN power (approximated by the 2-10 keV luminosity of the AGN), and investigating how the SFR distribution differs between these bins. These bin thresholds are often weakly motivated, and binning implicitly assumes that sources within the same bin have similar (or even identical) properties. In this paper, we investigate whether the distribution of host SFRs - relative to the locus of the star-forming main sequence (i.e. RMS) - changes continuously as a function of AGN power. We achieve this by using a hierarchical Bayesian model that completely removes the need to bin in AGN power. In doing so, we find strong evidence that the RMS distribution changes with 2-10 keV X-ray luminosity. The results suggest that higher X-ray luminosity AGNs have a tighter physical connection to the star-forming process than lower X-ray luminosity AGNs, at least within the 0.8 < z < 1.2 redshift range considered here.
Author(s): Grimmett LP, Mullaney JR, Bernhard EP, Harrison CM, Alexander DM, Stanley F, Masoura VA, Walters K
Publication type: Article
Publication status: Published
Journal: Monthly Notices of the Royal Astronomical Society
Year: 2020
Volume: 495
Issue: 1
Pages: 1392-1402
Print publication date: 01/06/2020
Online publication date: 16/05/2020
Acceptance date: 01/05/2020
ISSN (print): 0035-8711
ISSN (electronic): 1365-2966
Publisher: Oxford University Press
URL: https://doi.org/10.1093/MNRAS/STAA1255
DOI: 10.1093/MNRAS/STAA1255
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