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 stand-alone 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 \sim 3.5 ) offer statistically comparable fits to the data although the true reality of the Fe line can not 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 .