NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-06-27 T05:44:03 PDT
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For refcode 2010ApJ...710.1228L:
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2010ApJ...710.1228L Suzaku Monitoring of the Iron K Emission Line in the Type 1 Active Galactic Nucleus NGC 5548 Liu, Yuan; Elvis, Martin; McHardy, Ian M.; Grupe, Dirk; Wilkes, Belinda J.; Reeves, James; Brickhouse, Nancy; Krongold, Yair; Mathur, Smita; Minezaki, Takeo; Nicastro, Fabrizio; Yoshii, Yuzuru; Zhang, Shuang Nan Abstract. We present seven sequential weekly observations of NGC 5548 conducted in 2007 with the Suzaku X-ray Imaging Spectrometer (XIS) in the 0.2-12 keV band and Hard X-ray Detector (HXD) in the 10-600 keV band. The iron K{alpha} line is well detected in all seven observations and K{beta} line is also detected in four observations. In this paper, we investigate the origin of the Fe K lines using both the width of the line and the reverberation mapping method. With the co-added XIS and HXD spectra, we identify Fe K{alpha} and K{beta} line at 6.396^+0.009^_--0.007_ keV and 7.08^+0.05^_--0.05_ keV, respectively. The width of line obtained from the co-added spectra is 38^+16^_--18_ eV (FWHM = 4200^+1800^_--2000_ km s^--1^) which corresponds to a radius of 20^+50^_--10_ light days, for the virial production of 1.220 x 10^7^ M_sun_ in NGC 5548. To quantitatively investigate the origin of the narrow Fe line by the reverberation mapping method, we compare the observed light curves of Fe K{alpha} line with the predicted ones, which are obtained by convolving the continuum light curve with the transfer functions in a thin shell and an inclined disk. The best-fit result is given by the disk case with i = 30^degree^ which is better than a fit to a constant flux of the Fe K line at the 92.7% level (F-test). However, the results with other geometries are also acceptable (P>50%). We find that the emitting radius obtained from the light curve is 25-37 light days, which is consistent with the radius derived from the Fe K line width. Combining the results of the line width and variation, the most likely site for the origin of the narrow iron lines is 20-40 light days away from the central engine, though other possibilities are not completely ruled out. This radius is larger than the H{beta} emitting parts of the broad-line region at 6-10 light days (obtained by the simultaneous optical observation), and smaller than the inner radius of the hot dust in NGC 5548 (at about 50 light days). Key words: galaxies: active, galaxies: individual: NGC 5548, galaxies: Seyfert, quasars: emission lines, X-rays: galaxies
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