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

XMM-Newton Science Operation Center, VILSPA, ESA, Apartado 50727, 28080 Madrid, Spain

Corresponding author: M. Guainazzi, mguainaz@xmm.vilspa.esa.es

Received: 26 August 2002
Accepted: 30 January 2003

Abstract

This paper presents ASCA (July 1997), XMM-Newton (December 2000) and BeppoSAX (January 2001) observations of the Piccinotti Seyfert 1 galaxy ESO 198-G24. The BeppoSAX 0.1–200 keV spectrum exhibits reprocessing features, probably produced by an X-ray illuminated, relativistic accretion disk subtending a solid angle . During the XMM-Newton observation the fluorescent iron K_α line profile (centroid energy  keV) was broad and twice as bright as in the BeppoSAX observation. An additional emission feature ( keV), detected at the 96.3% confidence level, may be part of a relativistic, double-peaked profile. By contrast, in the earlier ASCA observation the line profile is dominated by a remarkably narrow “core” (intrinsic width,  eV). If this component is produced by reflection off the inner surface of a molecular torus, its large Equivalent Width ( 300 eV) most likely represents the “echo” of a previously brighter flux state, in agreement with the dynamical range covered by the historical X-ray light curve in ESO 198-G24.