High Density Reflection Spectroscopy – II. The density of the inner black hole accretion disc in AGN
We present a high density disc reflection spectral analysis of a sample of 17 Seyfert 1 galaxies to study the inner disc densities at different black hole mass scales and accretion rates. All the available XMM–Newton observations in the archive are used. OM observations in the optical/UV band are used to estimate their accretion rates. We find that 65 per cent of sources in our sample show a disc density significantly higher than n_e = 10^(15) cm^(−3), which was assumed in previous reflection-based spectral analyses. The best-fitting disc densities show an anticorrelation with black hole mass and mass accretion rate. High density disc reflection model can successfully explain the soft excess emission and significantly reduce inferred iron abundances. We also compare our black hole spin and disc inclination angle measurements with previous analyses.
Additional Information© 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). Accepted 2019 August 17. Received 2019 August 14; in original form 2019 June 3. Published: 23 August 2019. JJ acknowledges support by the Cambridge Trust and the Chinese Scholarship Council Joint Scholarship Programme (201604100032). DJW acknowledges support from an STFC Ernest Rutherford Fellowship. ACF acknowledges support by the ERC Advanced Grant 340442. MLP is supported by European Space Agency (ESA) Research Fellowships. JAG acknowledges support from the Alexander von Humboldt Foundation. The authors are also grateful to Andrew J. Young, Paul C. Hewett, and Sergei Dyda for valuable discussion.
Published - stz2326.pdf
Accepted Version - 1908.07272.pdf