Intrinsic bolometric correction in the restframe [2−10] keV energy range (K_{X,  [2 − 10] keV}) as a function of the AGN bolometric luminosity. Coloured data points show the estimates for the selected AGN population obtained from the combined MCMC analysis, assuming the low-mass solution shown in Fig. 6. As a reference, we report with blue data points the results from Laurenti et al. (2022) for a population of highly accreting AGNs (λ_Edd > 1) observed at 0.4 ≤ z ≤ 0.75. Despite being characterised by typical bolometric luminosities ∼1 dex higher than our sample, these systems show a comparable intrinsic X-ray weakness.