IR-optical-UV SEDs of SDSS J0100+2802 and SDSS J0306+1853 (left and right panels, respectively). The solid black line shows the spectrum obtained by Wu et al. (2015, left) and Wang et al. (2015, right). At frequencies larger than Log ν = 15.4, the absorption due to intervening Lyα clouds is clearly visible. Green points are WISE data. The red lines show the best accretion disc fittings. These are performed with a Kubota & Done (2019) model with parameters as labelled and reported in Table 2, but it is used to locate the peak of the emission and derive the KERRBB-based mass and spin estimates. The grey band highlights Kubota & Done profiles obtained with the virial masses and disc luminosities from the bolometric luminosities as derived in Wu et al. (2015, left) and Wang et al. (2015, right). The cyan shaded region in the right panel shows the same model but built with CIV-based virial masses. The yellow line in the left panel shows the same model obtained with the parameters as derived in Fujimoto et al. (2020), multiplied by the magnification factor 450.