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.
Categories: astro-ph.HE astro-ph.GA