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Title: The XMm Newton Iron Line Profile of NGC 3783
Authors: Reeves, J. N.
Nandra, K.
George, I. M.
Pounds, Kenneth Alwyne
Turner, T. J.
Yaqoob, T.
First Published: 2-Feb-2004
Publisher: IOP Publishing, American Astronomical Society
Citation: Astrophysical Journal, 2004, 602 (2), pp. 648-658
Abstract: We report on observations of the iron K line in the nearby Seyfert 1 galaxy, NGC 3783, obtained in a long, two-orbit (~240 ks) XMM-Newton observation. The line profile obtained exhibits two strong narrow peaks at 6.4 and 7.0 keV, with measured line equivalent widths of 120 and 35 eV, respectively. The 6.4 keV emission is the Kα line from near neutral Fe, while the 7.0 keV feature probably originates from a blend of the neutral Fe Kβ line and the hydrogen-like line of Fe at 6.97 keV. The relatively narrow velocity width of the Kα line (lesssim5000 km s-1), its lack of response to the continuum emission on short timescales, and the detection of a neutral Compton reflection component are all consistent with a distant origin in Compton-thick matter such as the putative molecular torus. A strong absorption line from highly ionized iron (at 6.67 keV) is detected in the time-averaged iron line profile, while the depth of the feature appears to vary with time, being strongest when the continuum flux is higher. The iron absorption line probably arises from the highest ionization component of the known warm absorber in NGC 3783, with an ionization of log ξ ~ 3 and column density of NH ~ 5 × 10[Superscript: 22] cm[Superscript: -2] and may originate from within 0.1 pc of the nucleus. A weak red wing to the iron K line profile is also detected below 6.4 keV. However, when the effect of the highly ionized warm absorber on the underlying continuum is taken into account, the requirement for a relativistic iron line component from the inner disk is reduced.
DOI Link: 10.1086/381091
ISSN: 0004-637X
eISSN: 1538-4357
Version: Publisher Version
Status: Peer-reviewed
Type: Journal Article
Rights: Copyright © 2004. The American Astronomical Society. All rights reserved. Deposited with reference to the publisher’s archiving policy available on the SHERPA/RoMEO website.
Appears in Collections:Published Articles, Dept. of Physics and Astronomy

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