Relativistic Iron K Emission and absorption in the Seyfert 1.9 galaxy MCG-5-23-16 - AstrophysicsReportar como inadecuado

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Abstract: We present the results of the simultaneous deep XMM and Chandra observationsof the bright Seyfert 1.9 galaxy MCG-5-23-16, which is thought to have one ofthe best known examples of a relativistically broadened iron K-alpha line. Thetime averaged spectral analysis shows that the iron K-shell complex is bestmodeled with an unresolved narrow emission component FWHM < 5000 km-s, EW ~ 60eV plus a broad component. This latter component has FWHM ~ 44000 km-s and EW~ 50 eV. Its profile is well described by an emission line originating from anaccretion disk viewed with an inclination angle ~ 40^\circ and with theemission arising from within a few tens of gravitational radii of the centralblack hole. The time-resolved spectral analysis of the XMM EPIC-pn spectrumshows that both the narrow and broad components of the Fe K emission lineappear to be constant in time within the errors. We detected a narrow sporadicabsorption line at 7.7 keV which appears to be variable on a time-scale of 20ksec. If associated with Fe XXVI Ly-alpha this absorption is indicative of apossibly variable, high ionization, high velocity outflow. The variability ofthis absorption feature appears to rule out a local z=0 origin. The analysisof the XMM RGS spectrum reveals that the soft X-ray emission of MCG-5-23-16 islikely dominated by several emission lines superimposed on an unabsorbedscattered power-law continuum. The lack of strong Fe L shell emission togetherwith the detection of a strong forbidden line in the O VII triplet isconsistent with a scenario where the soft X-ray emission lines are produced ina plasma photoionized by the nuclear emission.

Autor: V. Braito 1,2, J.N. Reeves 1,2,3, G.C. Dewangan 4, I. George 1,5, R.E. Griffiths 4, A. Markowitz 1,2, K. Nandra 6, D. Porquet 7,


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