Left panel: bolometric–to–X-ray correction (κ_bol,X = ﹩{L}_{\mathrm{bol},\mathrm{AGN}}^{(\mathrm{IR})}/{L}_{2-10}﹩) vs. galaxy separation. Right panel: bolometric–to–X-ray correction vs. IR-based Eddington ratio. The black solid line and gray shaded area represent the relation and its 1σ dispersion found by Lusso et al. (2012) for type 1 AGNs. The black dashed line shows a typical value of κ_bol,X = 20. Symbols and colors are the same as in Figure 3.