The origin of optical emission from super-Eddington accreting Active Galactic Nuclei: The case of Ton S 180

¹ LUTh/Observatoire de Paris-Meudon et CNRS UMR 8102, Place Jules Janssen, 92195 Meudon Cedex, France e-mail: Toshihiro.Kawaguchi@obspm.fr; Arnaud.Pierens@obspm.fr; Jean-Marc.Hure@obspm.fr
² Postdoctoral Fellow of the Japan Society for the Promotion of Science
³ Université Paris 7 Denis Diderot, 2 place Jussieu, 75251 Paris Cedex 05, France

Corresponding author: T. Kawaguchi, Toshihiro.Kawaguchi@obspm.fr

Received: 2 May 2003
Accepted: 17 October 2003

Abstract

Self-gravitating accretion discs have only been studied in a few nearby objects using maser spots at the parsec-scale. We find a new spectral window for observing the self-gravitating accretion disc in super-Eddington accreting Active Galactic Nuclei (AGNs). This window is determined by calculating the outermost radius () of a non self-gravitating disc and the corresponding emission wavelength () as a function of various disc parameters. We find that reaches ~ for , when (where α, , and are, respectively, the viscosity parameter, gas accretion rate onto the central black hole (BH), the BH mass and the Eddington luminosity). Moreover, is as small as ~ for , which is the smallest α case in this study. Therefore, the window for observing the self-gravitating part of an AGN accretion disc is from ~m to . Incidentally, can be less than the photon trapping radius for . Namely, a self-gravitating, optically-thick, advection-dominated accretion disc is expected to appear in the extremely high accretion rate regime.
Next, we demonstrate that the Mid-Infrared to X-ray spectrum of a bright, well-studied Narrow-Line Seyfert 1 galaxy, Ton S 180, is indeed well fitted by the spectrum arising from the following three components: an inner slim disc (with a corona), an outer, self-gravitating non-Keplerian disc and a dusty torus. The total mass, BH mass plus the entire disc mass, is found to be about . If the surface density varies with radius r in proportion to r^-0.6, the total mass is consistent with the central mass estimated by Hβ and [O III] widths.