Log(L_[O III])–Log(L_{2–10 keV}) plane. The dot-dashed, dotted, and dashed lines represent respectively the best fits for the Panessa et al. (2006), Meléndez et al. (2008), and Ueda et al. (2015) samples. Other luminous high-redshift samples with currently available [O III] and X-ray data from the WISSH (Vietri et al. 2018; Zappacosta et al. 2020) and SUPER (Kakkad et al. 2020) surveys, as well as the less luminous sample from Laurenti et al. (2022) including some X-ray weak objects, are also shown. Our objects where the [O III] is barely detectable (i.e. J0303−0023 and J1425+5406) are represented as upper limits. The circled data are defined as radio loud by the authors. BAL J0945+2305 is shown as an open pentagon. The typical uncertainties for the WISSH, SUPER, and Laurenti et al. (2022) samples are shown at the bottom of the plot.