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We employ optical and UV observations to present SEDs for tworeverberation-mapped samples of super-Eddington and sub-Eddington AGN withsimilar luminosity distributions. The samples are fitted with accretion discmodels in order to look for SED differences that depend on the Eddington ratio.The fitting takes into account measured BH mass and accretion rates, BH spinand intrinsic reddening of the sources. All objects in both groups can befitted by thin AD models over the range 0.2-1$\,\mu$m with reddening as a freeparameter. The intrinsic reddening required to fit the data are relativelysmall, $E(B-V)\leq0.2$~mag, except for one source. Super-Eddington AGN seem torequire more reddening. The distribution of $E(B-V)$ is similar to what isobserved in larger AGN samples. The best fit disc models recover very well theBH mass and accretion for the two groups. However, the SEDs are very different,with super-Eddington sources requiring much more luminous far-UV continuum. Theexact amount depends on the possible saturation of the UV radiation in slimdiscs. In particular, we derive for the super-Eddington sources a typicalbolometric correction at 5100\AA{} of 60-150 compared with a median of $\sim$20for the sub-Eddington AGN. The measured torus luminosity relative to $\lambdaL_{\lambda}(5100\AA{}$) are similar in both groups. The $\alpha_{OX}$distribution is similar too. However, we find extremely small torus coveringfactors for super-Eddington sources, an order of magnitude smaller than thoseof sub-Eddington AGN. The small differences between the groups regarding thespectral range 0.2-22$\,\mu$m, and the significant differences related to thepart of the SED that we cannot observed may be consistent with some slim discmodels. An alternative explanation is that present day slim-disc modelsover-estimate the far UV luminosity of such objects by a large amount.

monthly notices of the royal astronomical society

Super- and sub-Eddington accreting massive black holes: A comparison of  slim and thin accretion discs through study of the spectral energy  distribution