NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-06-19 T12:28:22 PDT
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For refcode 2003A&A...401..903G:
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Copyright by European Southern Observatory (ESO). Reproduced by permission
2003A&A...401..903G The history of the iron K_{alpha}_ line profile in the Piccinotti AGN ESO 198-G24 M. Guainazzi 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 ~< 2 {pi}. During the XMM-Newton observation the fluorescent iron K_{alpha}_ line profile (centroid energy E_c_ ~= 6.4 keV) was broad and twice as bright as in the BeppoSAX observation. An additional emission feature ( E_c_ ~= 5.7 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, {sigma} < 50 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. 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 ~< 2 {pi}. During the XMM-Newton observation the fluorescent iron K_{alpha}_ line profile (centroid energy E_c_ ~= 6.4 keV) was broad and twice as bright as in the BeppoSAX observation. An additional emission feature ( E_c_ ~= 5.7 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, {sigma} < 50 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. Keywords: accretion, accretion discs, galaxies: active, galaxies: individual: ESO 198-G24, X-rays: galaxies, galaxies, nuclei
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