Updating quasar bolometric luminosity corrections
  Bolometric corrections are used in quasar studies to quantify total energy
output based on a measurement of a monochromatic luminosity. First, we
enumerate and discuss the practical difficulties of determining such
corrections, then we present bolometric luminosities between 1 \mu m and 8 keV
rest frame and corrections derived from the detailed spectral energy
distributions of 63 bright quasars of low to moderate redshift (z = 0.03-1.4).
Exploring several mathematical fittings, we provide practical bolometric
corrections of the forms L_iso=\zeta \lambda L_{\lambda} and log(L_iso)=A+B
log(\lambda L_{\lambda}) for \lambda= 1450, 3000, and 5100 \AA, where L_iso is
the bolometric luminosity calculated under the assumption of isotropy. The
significant scatter in the 5100 \AA\ bolometric correction can be reduced by
adding a first order correction using the optical slope, \alpha_\lambda,opt. We
recommend an adjustment to the bolometric correction to account for viewing
angle and the anisotropic emission expected from accretion discs. For
optical/UV monochromatic luminosities, radio-loud and radio-quiet bolometric
corrections are consistent within 95% confidence intervals so we do not make
separate radio-loud and radio-quiet corrections. In addition, we provide
several bolometric corrections to the 2-10 keV X-ray luminosity, which are
shown to have very large scatter. Separate radio-loud and radio-quiet
corrections are warranted by the X-ray data.
