XMM-Newton observations of Broad FeKalpha emission from a Seyfert 1.9 galaxy MCG-5-23-16

Details XMM-Newton observations of Broad FeKalpha emission from a Seyfert 1.9 galaxy MCG-5-23-16 XMM-Newton observations of Broad FeKalpha emission from a Seyfert 1.9 galaxy MCG-5-23-16

2003-04-01

arxiv.org/abs/astro-ph/0304037v1

Astrophys.J. 592 (2003) 52-61

Astronomy and Astrophysics

Astrophysics

14 pages including 7 figures, To appear in ApJ

Scientific paper

10.1086/375640

XMM-Newton observations of the bright Seyfert 1.9 galaxy MCG-5-23-16 have revealed a broad FeKalpha emission line which is nearly symmetric in contrast to the broad and red-shifted asymmetric FeKalpha line sometimes observed from Seyfert 1 galaxies. The FeKalpha line has two distinct components - a narrow unresolved component with equivalent width of 40 eV and a broad component with full width at half maximum of 40000 km/s and equivalent width of 120 eV. An absorption feature at 7.1 keV has also been observed. The energies of the emission and absorption features are consistent with those arising from neutral iron. The broad component is consistent with an FeKalpha emission line expected from a relativistic accretion disk around a Schwarzschild or a Kerr black hole. Alternatively, most of the flux in the broad component could also be modeled as reflection emission which mimics emission line like feature due to the presence of iron K-shell edge at 7.1eV, however, the reflection fraction is much higher than that inferred from the BeppoSax observations. The disk inclination angle of about 47 deg, inferred from the disk-line fits, and the absorption column of about 10^{22} cm^{-2}, inferred from the low-energy spectral curvature due to photoelectric absorption, suggest that our line of sight passes through the outer edge of a putative torus and are consistent with those expected for a Seyfert 1.9 galaxy falling within the unification scheme. The strength of the narrow iron Kalpha emission and the optical depth of the iron K absorption edge suggest their origin in the putative torus with N_H about 10^{24} cm^{-2} in the inner regions and N_H about 10^{22} cm^{-2} in the outer edges.

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