http://arxiv.org/abs/2208.06581
RX J0134.2-4258 is one of the most super-Eddington narrow-line Seyfert 1 (NLS1) galaxies, on which we conducted a monitoring campaign from radio to X-rays. In this paper, we present a detailed analysis of its optical/UV spectra and broadband spectral energy distribution (SED). Our study shows that the preferred black hole mass of RX J0134.2-4258 is $\sim 2~\times~10^{7}~M_{\odot}$, giving a mass accretion rate through the outer disc of $\dot{m}{\rm out} \sim 20$ (assuming zero spin) compared to the observed luminosity ratio $L{\rm bol}/L_{\rm Edd} \sim 6$. This reduction in radiative efficiency is expected for super-Eddington flows, as power can be lost via advection and/or winds. We find that the optical/UV lines of RX J0134.2-4258 resemble those from weak-like quasars (WLQs), as it has notably weak C IV and N V emission lines. It also has dramatic X-ray variability, again similar to that recently observed in some other WLQs. However, WLQs have systematically higher masses ($\gtrsim 10^8~M_{\odot}$), and lower Eddington ratios ($\dot{m}{\rm out} \sim 1-3$) than RX J0134.2-4258. We compare instead to the most extreme NLS1s, with similarly large $\dot{m}{\rm out}$ but smaller masses. These show similarly large reductions in radiative efficiency but their UV lines are not similarly wind-dominated. We suggest a new category of weak-line Seyfert (WLS) galaxies to describe sources like RX J0134.2-4258, and interpret its (so far unique) properties in a model where the lower disc temperature in the higher-mass black holes leads to UV line driving enhancing the super-Eddington radiation pressure driven wind.
C. Jin, C. Done, M. Ward, et. al.
Tue, 16 Aug 22
27/74
Comments: 19 pages, 10 figures, 7 tables, submitted to MNRAS