Investigating the origin of the Fe emission lines of the Seyfert 1
  galaxy Mrk~205
  We have investigated the nature and origin of the Fe K emission lines in
Mrk~205 using observations with {\it Suzaku} and {\it XMM-Newton}, aiming to
resolve the ambiguity between a broad emission line and multiple unresolved
lines of higher ionization. We detect the presence of a narrow Fe K$\alpha$
emission line along with a broad band Compton reflection hump at energies $E>10
\rm \, keV$. These are consistent with reflected emission of hard X-ray photons
off a Compton thick material of $N_{\rm H} \ge 2.15\times 10^{24} \rm cm^{-2}$.
In addition we detect a partially covering ionized absorption with ionization
parameter $\log(\xi/\rm erg\, cm\, s^{-1})=1.9_{-0.5}^{+0.1}$, column density
$N_{\rm H}=(5.6_{-1.9}^{+2.0})\times 10^{22}\rm cm^{-2}$ and a covering factor
of $0.22_{-0.06}^{+0.09}$. We detect the presence of emission arising out of
ionized disk reflection contributing in the soft and the hard X-rays
consistently in all the observations. We however, could not definitely
ascertain the presence of a relativistically broadened Fe line in the X-ray
spectra. Using relativistic reflection model, we found that the data are unable
to statistically distinguish between the scenarios when the super-massive black
hole is non-rotating and when it is maximally spinning. Using the disk
reflection model we also find that the accretion disk of the AGN may be
truncated at a distance $6R_{\rm G}<R<12R_{\rm G}$, which may suggest why there
may not be any broad Fe line. The Eddington rate of the source is low
($\lambda_{\rm Edd}=0.03$), which points to an inefficient accretion, possibly
due to a truncated disk.
