Issue |
A&A
Volume 461, Number 3, January III 2007
|
|
---|---|---|
Page(s) | 917 - 922 | |
Section | Extragalactic astronomy | |
DOI | https://doi.org/10.1051/0004-6361:20065566 | |
Published online | 11 October 2006 |
XMM-Newton view of the double-peaked Fe Kα complex in E1821+643
1
Dipartimento di Fisica di l'Universita Roma Tre, via della Vasca Navale 84, 00146 Rome, Italy e-mail: ejimenez@fis.uniroma3.it
2
XMM-Newton Science Operations Centre, ESAC, ESA, Apartado 50727, 28080 Madrid, Spain
3
Osservatorio Astronomico di Roma (INAF), via Frascati 33, 00040 Monteporzio Catone, Italy
Received:
8
May
2006
Accepted:
22
August
2006
We present the results of the analysis of the hard band
XMM-Newton spectra of the luminous,
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 Kα 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.
Key words: galaxies: general / galaxies: active / galaxies: nuclei / X-rays: individuals: E 1821+643
© ESO, 2007
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