  We report the \Suzaku/XIS and HXD and \Chandra/ACIS-I results on the X-ray
spectra of the Phoenix cluster at the redshift $z=0.596$. The spectrum of the
intracluster medium (ICM) is well-reproduced with the emissions from a low
temperature ($\sim3.0$\,keV and $\sim0.76$\,solar) and a high temperature
($\sim11$\,keV and $\sim0.33$\,solar) plasmas; the former is localized at the
cluster core, while the latter distributes over the cluster. In addition to
these ICM emissions, a strongly absorbed power-law component is found, which is
due to an active galactic nucleus (AGN) in the cluster center. The absorption
column density and unobscured luminosity of the AGN are
$\sim3.2\times10^{23}$\,cm$^{-2}$ and $\sim4.7\times10^{45}$\,ergs\,s$^{-1}$
(2-10\,keV), respectively. Furthermore, a neutral iron (\ion{Fe}{1}) K-shell
line is discovered for the first time with the equivalent width (EW) of
$\sim150$\,eV at the rest frame. The column density and the EW of the
\ion{Fe}{1} line are exceptionally large for such a high luminosity AGN, and
hence the AGN is classified as a type 2 quasi-stellar object (QSO). We
speculate that the significant fraction of the ICM cooled gas would be consumed
to maintain the torus and to activate the type 2 QSO. The Phoenix cluster has a
massive starburst in the central galaxy, indicating suppression in the cooling
flow is less effective. This may be because the onset of the latest AGN
feedback has occurred recently and it has not yet been effective.
Alternatively, the AGN feedback is predominantly in radiative-mode not in
kinetic-mode and the torus may work as a shield to reduce its effect.
