Power of SED decomposition to derive the AGN bolometric luminosity ($L_{\mathrm{bol}}^{\mathrm{AGN}}$), and the BHAR. The panels show the AGN bolometric luminosity derived from SED fitting by Gruppioni et al. (2016) for a local sample of AGN versus the AGN bolometric luminosity derived from different indicators: Left: X-ray (2−10 keV) luminosity. Right: [O IV] 25.9 μm FIR line. X-ray bolometric corrections are taken from Brightman & Nandra (2011). The dashed line represents the 1−1 relation. With PRIMA we will be able to perform similar decompositions up to z = 2. The stars in the left panel show how the X-ray-derived $L_{\mathrm{bol}}^{\mathrm{AGN}}$ increases for Compton-thick AGN once the hard X-ray spectrum is included (as shown by La Caria et al. 2019). The correlation found in the right panel can be used as a calibration for the SED-fitting results when FIR spectroscopy is not available.