We present the results of the analysis of the hard band XMM-Newton spectra of the luminous, L2-10 keV similar to 3.4 x 10(45) erg/s, radio-quiet quasar, E 1821+643. Two emission features were observed in the 6 - 7 keV rest frame band, confirming previous Chandra detection of these structures. We interpret these features as two single emission lines, one consistent with the neutral Fe K alpha line at 6.4 keV and the other most likely due to FeXXVI. If related to the quasar, the high-energy emission line should originate in highly ionised matter, i.e. the accretion disc or the clouds of the emission line regions. Alternatively, it may be related to the intergalactic medium of the rich galaxy cluster in which E 1821+643 is embedded. A composite broad emission line in combination with an absorption line model, however, also fits the data well. We discuss the possible physical interpretations of the origin of these features.
Jimenez Bailon, E., Santos Lleo, M., Piconcelli, E., Matt, G., Guainazzi, M., Rodriguez Pascual, P. (2007). XMM-Newton view of the double-peaked FeK alpha complex in E1821+643. ASTRONOMY & ASTROPHYSICS, 461(3), 917-922 [10.1051/0004-6361:20065566].
XMM-Newton view of the double-peaked FeK alpha complex in E1821+643
MATT, Giorgio;
2007-01-01
Abstract
We present the results of the analysis of the hard band XMM-Newton spectra of the luminous, L2-10 keV similar to 3.4 x 10(45) erg/s, radio-quiet quasar, E 1821+643. Two emission features were observed in the 6 - 7 keV rest frame band, confirming previous Chandra detection of these structures. We interpret these features as two single emission lines, one consistent with the neutral Fe K alpha line at 6.4 keV and the other most likely due to FeXXVI. If related to the quasar, the high-energy emission line should originate in highly ionised matter, i.e. the accretion disc or the clouds of the emission line regions. Alternatively, it may be related to the intergalactic medium of the rich galaxy cluster in which E 1821+643 is embedded. A composite broad emission line in combination with an absorption line model, however, also fits the data well. We discuss the possible physical interpretations of the origin of these features.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
