Fe XXV and Fe XXVI lines from low-velocity, photoionized gas in the X-ray spectra of active galactic nuclei

被引:71
作者
Bianchi, S
Matt, G
Nicastro, F
Porquet, D
Dubau, J
机构
[1] Univ Roma Tre, Dipartimento Fis, I-00146 Rome, Italy
[2] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
[3] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany
[4] Univ Paris 11, Lab Interact Rayonnement X Avec Mat, F-91405 Orsay, France
关键词
line : formation; galaxies : Seyfert; X-rays : galaxies;
D O I
10.1111/j.1365-2966.2005.08661.x
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We have calculated the equivalent widths of the absorption lines produced by Fe XXV and Fe XXVI in a Compton-thin, low-velocity photoionized material illuminated by the nuclear continuum in active galactic nuclei. The results, plotted against the ionization parameter and the column density of the gas, are a complement to those presented by Bianchi & Matt for the emission lines from the same ionic species. As an extension to the work by Bianchi & Matt, we also present a qualitative discussion on the different contributions to the He-like iron emission line complex in the regimes where recombination or resonant scattering dominates, providing a useful diagnostic tool to measure the column density of the gas. Future high-resolution missions (e. g. Astro-E2) will allow us to fully take advantage of these plasma diagnostics. In the meantime, we compare our results with an up-to-date list of Compton-thick and unobscured (at least at the iron line energy) Seyfert galaxies with emission and/or absorption lines from H- and He-like iron observed with Chandra and XMM-Newton.
引用
收藏
页码:599 / 607
页数:9
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