The Bolometric Luminosity Correction of Radio-Quiet and Radio-Loud
  Quasars at 1<z<2
  To understand the impact of active galactic nuclei (AGN) on their host
galaxies and large scale environment it is crucial to determine their total
radiative power across all wavelengths (i.e., bolometric luminosity). In this
contribution we describe how quasar accretion disk spectral energy distribution
(SED) templates, parameterized by the black hole (BH) mass, Eddington ratio,
and spin can be used to estimate their total radiated luminosity. To estimate
the bolometric luminosity of AGN, we integrate the accretion disk SEDs from
1$\mu$m to 10keV. Our approach self-consistently covers any gaps in
observations and does not include reprocessed emission from the torus. The
accretion disk SED, and consequently the bolometric correction inferred from
it, strongly depend on the BH mass, the Eddington ratio, and spin. In
particular, the bolometric correction in the visible bands
(5100$\,\mathring{A}$ and 3000$\,\mathring{A}$) strongly depends on BH mass,
and at X-ray strongly depends on the Eddington ratio. At wavelengths closer to
the peak of the accretion disk SED the dependence becomes weaker. Additionally,
maximally-rotating (spin = 1) quasars require a higher bolometric correction
than their non-rotating (spin = 0) counterparts at all wavelengths. The SEDs
and the bolometric correction presented in this work can determine the
radiative power of any sample of radio-quiet to radio-loud Type 1 AGN with
observations in the range from 1$\mu$m to 10$\,$keV provided the observations
are corrected for extinction.
