Issue |
A&A
Volume 401, Number 3, April III 2003
|
|
---|---|---|
Page(s) | 903 - 910 | |
Section | Extragalactic astronomy | |
DOI | https://doi.org/10.1051/0004-6361:20030160 | |
Published online | 01 April 2003 |
The history of the iron Kα 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
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 Kα 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.
Key words: accretion, accretion discs / galaxies: active / galaxies: individual: ESO 198-G24 / X-rays: galaxies / galaxies / nuclei
© ESO, 2003
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