Investigating the origin of the Fe emission lines of the Seyfert 1 galaxy Mrk~205

Abstract

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 $E>10\mathrm{keV}$. These are consistent with reflected emission of hard X-ray photons off a Compton thick material of $N_{\mathrm{H}}\ge 2.15\times 10^{24}\mathrm{c}{\mathrm{m}}^{-2}$. In addition we detect a partially covering ionized absorption with ionization parameter $\log (\xi /\mathrm{erg}\mathrm{cm}{\mathrm{s}}^{-1})=1.9_{-0.5}^{+0.1}$, column density $N_{\mathrm{H}}=(5.6_{-1.9}^{+2.0})\times 10^{22}\mathrm{c}{\mathrm{m}}^{-2}$ 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 $6R_{\mathrm{G}}<R<12R_{\mathrm{G}}$, which may suggest why there may not be any broad Fe line. The Eddington rate of the source is low (${\lambda }_{\mathrm{Edd}}=0.03$), which points to an inefficient accretion, possibly due to a truncated disk.

arXiv commentAccepted for publication in MNRAS

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