The Bolometric Luminosity Correction of Radio-Quiet and Radio-Loud Quasars at 1<z<2

To better understand how active galactic nuclei (AGN) impact their nearby environments and host galaxies, it is crucial to determine their total radiative power (their bolometric luminosities). Here, we describe new quasar accretion disk spectral energy distribution (SED) templates, parameterized by black hole (BH) mass, Eddington ratio, and spin, and use them to estimate total radiated AGN luminosities from 1 μm to 10 keV. Our approach self-consistently covers wavelength gaps and avoids double-counting reprocessed emission from the torus. The visible-wavelength (5100 and 3000 AA) bolometric corrections (BCs) strongly depend on BH mass, while in the X-ray regime, the BCs strongly depend on the Eddington ratio. At ultraviolet wavelengths (2000 AA), closer to the accretion disk SED peaks, the dependence is weaker. Maximally rotating (spin = 1) quasars require higher BCs than their non-rotating (spin = 0) counterparts at all wavelengths. The SEDs and BCs presented here can be used to determine the total radiative power of any radio-quiet or radio-loud Type 1 AGN with photometry from 1 μm to 10 keV.