We present the results of a systematic analysis of Fe K emission lines in low-luminosity AGNs (LLAGNs) observed with ASCA. We used a sample of LLAGNs with small intrinsic absorption to compare with luminous AGNs and accretion models. Some objects show an Fe line at 6.4 keV or 6.7 keV, and the rest of the objects show no significant Fe K emission line. We made a composite spectrum of sources without detected Fe emission lines to search for weak lines and obtained an upper limit on the equivalent width (EW) of a narrow line at 6.4 keV of 145 eV, which is marginally consistent with EWs seen in Seyfert 1s. Even in those objects with detected Fe lines, a skewed broad component, typically observed in Seyfert 1s, is not seen. The weakness of the Fe line is consistent with the absence of an optically thick disk in the vicinity of a central black hole. Alternatively, it might be due to the ionization of a standard disk. The lack of big blue bump favors the former.
- Pub Date:
- February 2002
- 4 pages, In ``X-ray Emission from Accretion onto Black Holes'', proceedings of a workshop held by JHU and LHEA, in Baltimore, MD, June 20-23, 2001, eds. T. Yaqoob, &