Suzaku Monitoring of the Iron K Emission Line in the Type 1 AGN NGC5548

Details Suzaku Monitoring of the Iron K Emission Line in the Type 1 AGN NGC5548 Suzaku Monitoring of the Iron K Emission Line in the Type 1 AGN NGC5548

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21342001l&link_type=abstract

American Astronomical Society, AAS Meeting #213, #420.01; Bulletin of the American Astronomical Society, Vol. 41, p.235

Astronomy and Astrophysics

Astronomy

Scientific paper

The 6.4 keV iron K emission line is a common phenomenon in the X-ray observation of active galactic nuclei (AGN), and is seen with a range of widths, from relativistically broadened to narrow. The width of the line is usually used to estimate the distance of the emitting material from the central supermassive black hole, assuming virialized motions. This size should be consistent with the variability of the Fe-K line in response to continuum changes. We present 7 sequential weekly Suzaku observations of NGC5548 conducted in 2007. With the very good S/N of the summed Suzaku spectrum, we identify Ka and Kb line at 6.40 keV and 7.05 keV with mean EWs of 100 and 20 eV, respectively. The FWHM of Ka is about 5500 km/s placing the iron line emission at 3000 rg, or a few light-weeks, i.e. near the broad line region. However, during these observations, the 2-10 keV band exhibits variation of a factor 4, but the flux of the iron line is constant to within 10-15% of 2.0^{-5} cts/cm^2/s. The lack of response to the continuum within 8 weeks implies a distance for the line-emitting gas to the SMBH larger than 0.1 light year. We discuss this apparent contradiction in terms of non-Keplerian motions, unusual geometries or light-travel time delays. No obvious broad line appears in the spectra .

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