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 Suzaku and 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 Kα emission line along with a broad band Compton reflection hump at energies E > 10 keV. These are consistent with reflected emission of hard X-ray photons off a Compton thick material of N H 2.15 × 10 24 cm −2 . In addition we detect a partially covering ionized absorption with ionization parameter log(ξ/ erg cm s −1 ) = 1.9 +0.1 −0.5 , column density N H = (5.6 +2.0 −1.9 ) × 10 22 cm −2 and a covering factor of 0.22 +0.09 −0.06 . 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 models, 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 G < R < 12R G , which may suggest why there may not be any broad Fe line. The Eddington rate of the source is low (λ Edd = 0.03), which points to an inefficient accretion, possibly due to a truncated disk.

A Radio, Optical, UV, and X-Ray View of the Enigmatic Changing-look Active Galactic Nucleus 1ES 1927+654 from Its Pre- to Postflare States

“…Popular theories suggest that it could arise out of thermal Comptonization of the UV seed photons by a warm corona (Done et al 2012) or it can also arise out of the reflection of hard X-ray photons from the corona off the accretion disk (García et al 2014). Even after a considerable number of studies on the subject (Laha et al 2011(Laha et al , 2013(Laha et al , 2014aEhler et al 2018;García et al 2019;Laha et al 2019;Tripathi et al 2019;Waddell et al 2019;Ghosh & Laha 2020;Laha et al 2020;Ursini et al 2020;Laha & Ghosh 2021), there has not been a consensus on the physics of the origin of the soft X-ray excess. X-ray reverberation lead/lag studies too have yielded conflicting results for different sources (Kara et al 2016).…”

An X-ray spectral study of the origin of reflection features in bare Seyfert 1 galaxy ESO 511--G030

“…We have used only MYTorusS and the MYTorusL component in our spectral fitting and tied their column densities together. The column density of MYTorus gives a value in an equatorial direction of a dusty torus, so a Compton-thick value is expected even in type 1 sources (Yaqoob et al 2016;Laha et al 2019;Ghosh & Laha 2020). When made free, the MYTorus column density pegged at 10 25 cm −2 and we got a lower limit of 2.9 × 10 24 cm −2 .…”

A radio, optical, UV and X-ray view of the enigmatic changing look Active Galactic Nucleus 1ES~1927+654 from its pre- to post-flare states

“…Popular theories suggest that it could arise out of thermal Comptonization of the UV seed photons by a warm corona (Done et al 2012) or it can also arise out of the reflection of the hard X-ray photons from the corona off the accretion disk (García et al 2014). Even after considerable studies on the subject (Laha et al 2011(Laha et al , 2013(Laha et al , 2014aEhler et al 2018;Laha et al 2020;García et al 2019;Waddell et al 2019;Laha et al 2019;Tripathi et al 2019;Ghosh & Laha 2020;Ursini et al 2020;Laha & Ghosh 2021) there has not been a consensus on the physics of the origin of the soft X-ray excess. Xray reverberation lead/lag studies too have yielded conflicting results for different sources (Kara et al 2016).…”