The Iron K Line Profile of IRAS 18325-5926
  IRAS 18325-5926 is an X-ray bright, Compton-thin, type-2 Seyfert galaxy and
it was the first Seyfert 2 in which the presence of a broad Fe K-alpha emission
line was claimed. However, although the structure of the Fe line appears broad,
there is tentative evidence that it may comprise multiple lines. Nevertheless,
previous analyses have only consisted of fitting standalone broad components to
the Fe K band. Here, we have analyzed all available X-ray CCD data from Suzaku,
XMM-Newton and ASCA to fully investigate the nature of the emission complex by
testing broad-band physical models and alternative hypotheses. We find that
both a model consisting of broad, blurred reflection from an ionized accretion
disc and a model consisting of cold, neutral reflection plus narrow emission
lines from highly-ionized photoionized gas (log \xi = 3.5) offer statistically
comparable fits to the data although the true reality of the Fe line cannot
currently be determined with existing data. However, it is hoped that better
quality data and improved photon statistics in the Fe K band will allow a more
robust distinction between models to be made.
