Properties of Galaxies around AGNs with Most Massive Supermassive Black
  Hole Revealed by the Clustering Analysis
  We present results of the clustering analysis between active galactic nuclei
(AGNs) and galaxies at redshift 0.1-1.0 for investigating properties of
galaxies associated with the AGNs, revealing the nature of fueling mechanism of
supermassive black holes (SMBHs). We used 8059 SDSS AGNs/QSOs for which virial
masses of individual SMBHs were measured, and divided them into four mass
groups. Cross-correlation analysis was performed and bias for each mass group
was derived. The averaged color and luminosity distributions of galaxies around
the AGNs/QSOs were also derived for each mass group. The galaxy color was
estimated for SED constructed from a merged SDSS and UKIDSS catalog. The
distributions of color and luminosity were derived by the subtraction method,
which does not require redshift information of galaxies. The main results of
this work are: (1) a bias increases by a factor two from the lower mass group
to the highest mass group; (2) the environment around AGNs with the most
massive SMBH (Mbh > 10^9 Msun) is dominated by red sequence galaxies; (3)
marginal indication of decline in luminosity function at dimmer side of M >
-19.5 mag is found for galaxies around AGNs with Mbh = 10^8.2 - 10^9 Msun and
nearest redshift group (z=0.1-0.3). These results indicate that AGNs with the
most massive SMBHs reside in haloes where large fraction of galaxies have been
transited to the red sequence. The accretion of hot halo gas as well as
recycled gas from evolving stars can be the most plausible mechanism to fuel
the SMBHs above ~10^9 Msun.
