Relativistic Fe Kα features in the XMM‐Newton spectrum of the intermediate Seyfert galaxy 4U 1344‐60

Abstract

We present the analysis of optical and X-ray XMM-Newton data of the source 4U 1344-60. On the basis of the optical data we propose to classify 4U 1344-60 as a Seyfert 1.5 galaxy and we measured a redshift value z=0.012±0.001. The observed X-ray spectrum is complex. The continuum emission can be described as a power law obscured by two neutral absorption components. 4U 1344-60 exhibits a broad and skewed iron line at 6.4 keV most likely originated in a few gravitational radius of an accretion disc. The analysis also reveals the presence of two narrow emission line-like features at ∼4.9 keV and ∼5.3 keV. Assuming that hot spots on the surface of the accretion disc, orbiting very close to the black hole is responsible of these emission lines, the accretion disc would present an inclination of 20• and the active regions would be located in the 6-10 Rg radius range.

Detection of blueshifted emission and absorption and a relativistic iron line in the X-ray spectrum of ESO 323−G077★

“…This value is higher than the mean EW of a local sample of Seyfert 1 galaxies, EW = 91 ± 13 eV (Nandra et al 2007), but comparable to the values of relativistically broaden Fe lines [e.g. EW (NGC 3516) = 394 +72 −63 eV, EW (MGC 6)−30−15) = 198 33 −30 eV, Nandra et al 2007; EW (4U 1344)-60) = 393 122 −107 eV, Piconcelli et al 2006;Jiménez-Bailón et al 2006; see other examples in Nandra et al 2007]. When the KYGline model is considered, the EW measured resulted to be 450 +15 −110 eV.…”