Bolometric correction factors for Active Galactic Nuclei
  The bolometric luminosity of active galactic nuclei (AGN) is difficult to
determine and various approximations have been used to calibrate it against
different observed properties. Here I combine theoretical calculations of
optically thick, geometrically thin accretion disks, and observed X-ray
properties of AGN, to provide new bolometric correction factors (\kbol) over a
large range of black hole (BH) mass, accretion rate, and spin. This is
particularly important in cases where the mass accretion rate cannot be
determined from the observed spectral energy distribution, and in cases where
luminosity-independent correction factors have been used. Simple powerlaw
approximations of \kbol\ are provided for L(5100\AA), L(3000\AA), L(1400\AA),
L(2-10 keV) and L(narrow \hb). In all cases the uncertainties are large mostly
due to the unknown BH spin. Prior knowledge of the BH mass reduces the
uncertainty considerably.
