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This paper presents ASCA (July 1997), XMM-Newton (December 2000) and BeppoSAX(January 2001) observations of the Piccinotti Seyfert 1 galaxy ESO198-G24. TheBeppoSAX 0.1-200 keV spectrum exhibits reprocessing features, probably producedby an X-ray illuminated, relativistic accretion disk subtending a solid angle\~2 pi. During the XMM-Newton observation the fluorescent iron K-alpha lineprofile (centroid energy E~6.4 keV) was broad and twice as bright as in theBeppoSAX observation. An additional emission feature (E~5.7 keV), detected atthe 96.3% confidence level, may be part of a relativistic, double-peakedprofile. By contrast, in the earlier ASCA observation the line profile isdominated by a remarkably narrow "core" (intrinsic width <50 eV). If thiscomponent is produced by reflection off the inner surface of a molecular torus,its large Equivalent Width (~300 eV) most likely represents the "echo" of apreviously brighter flux state, in agreement with the dynamical range coveredby the historical X-ray light curve in ESO198-G24.Comment: 9 Latex pages, 11 figures, To appear in Astronomy & Astrophysic

The history of the iron Kαline profile in the Piccinotti AGN ESO 198-G24

The history of the iron K_αline profile in the Piccinotti AGN ESO 198-G24