Bolometric luminosity versus redshift for our objects, plotted as red diamonds. Our bolometric luminosities are estimated from dust-corrected narrow emission lines and should be treated as upper limits. The black point in the bottom right corner shows the systematic uncertainty on the bolometric luminosity for Type-2 AGN. Systematic uncertainties are dominating our measurements. We compare our sample with previous JWST type-1 AGN (various coloured stars and diamonds; Bogdán et al. 2024; Carnall et al. 2023b; Kocevski et al. 2023; Kokorev et al. 2023; Furtak et al. 2024; Goulding et al. 2023; Maiolino et al. 2024a,b; Matthee et al. 2024; Übler et al. 2023; Chisholm et al. 2024), AGN from the KASHz and SUPER surveys at Cosmic Noon (grey and red crosses; Harrison et al. 2016; Kakkad et al. 2020) and QSOs samples across redshifts: SDSS QSOs (z = 2 − 6, grey shaded region; Wu & Shen 2022), extremely red quasars (blue-green crosses; Perrotta et al. 2019), blue QSOs (purple crosses; Shen 2016) and compilation of EoR QSOs (magenta crosses; Fan et al. 2023).