Contribution of the accretion disk, hot corona, and obscuring torus to
  the luminosity of Seyfert galaxies: INTEGRAL and Spitzer observations
  We estimate the relative contributions of the supermassive black hole (SMBH)
accretion disk, corona, and obscuring torus to the bolometric luminosity of
Seyfert galaxies, using Spizter mid-infrared (MIR) observations of a complete
sample of 68 nearby active galactic nuclei from the INTEGRAL all-sky hard X-ray
(HX) survey. This is the first HX-selected (above 15 keV) sample of AGNs with
complementary high angular resolution, high signal to noise, MIR data.
Correcting for the host galaxy contribution, we find a correlation between HX
and MIR luminosities: L_MIR L_HX^(0.74+/-0.06). Assuming that the observed MIR
emission is radiation from an accretion disk reprocessed in a surrounding dusty
torus that subtends a solid angle decreasing with increasing luminosity (as
inferred from the declining fraction of obscured AGNs), the intrinsic disk
luminosity, L_D, is approximately proportional to the luminosity of the corona
in the 2-300 keV energy band, L_C, with the L_D/L_C ratio varying by a factor
of 2.1 around a mean value of 1.6. This ratio is a factor of ~2 smaller than
for typical quasars producing the cosmic X-ray background (CXB). Therefore,
over three orders of magnitude in luminosity, HX radiation carries a large, and
roughly comparable, fraction of the bolometric output of AGNs. We estimate the
cumulative bolometric luminosity density of local AGNs at ~(1-3)x10^40
erg/s/Mpc^3. Finally, the Compton temperature ranges between kT_c~2 and ~6 keV
for nearby AGNs, compared to kT_c~2 keV for typical quasars, confirming that
radiative heating of interstellar gas can play an important role in regulating
SMBH growth.
