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Fe XXV and Fe XXVI lines from low velocity, photoionised gas in the X-ray spectra of AGN
Astrophysics · Submitted 22 Nov 2004
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim As an extension to the work by Bianchi & Matt 2002, 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.
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The abstract, sentence by sentence
We have calculated the equivalent widths of the absorption lines produced by Fe XXV and Fe XXVI in a Compton-thin, low-velocity photoionised material illuminated by the nuclear continuum in AGN. The results, plotted against the ionisation parameter and the column density of the gas, are a complement to those presented by Bianchi & Matt 2002 for the emission lines from the same ionic species. As an extension to the work by Bianchi & Matt 2002, 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.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We have calculated the equivalent widths of the absorption lines produced by Fe XXV and Fe XXVI in a Compton-thin, low-velocity photoionised material illuminated by the nuclear continuum in AGN. | contribution 0.96 | 0.96 | 0.11 | asserted 0.99 |
| s1 | The results, plotted against the ionisation parameter and the column density of the gas, are a complement to those presented by Bianchi & Matt 2002 for the emission lines from the same ionic species. | result 0.43 | 0.83 | 0.13 | asserted 1.00 |
| s2 | As an extension to the work by Bianchi & Matt 2002, 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. | contribution 0.98 | 0.84 | 0.18 | asserted 0.97 |
| s3 | Future high resolution missions (e.g., Astro-E2) will allow us to fully take advantage of these plasma diagnostics. | future work 1.00 | 0.05 | 0.06 | hedged possibility 0.77 |
| s4 | 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. | contribution 0.68 | 0.81 | 0.08 | asserted 0.97 |
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The paper
Original abstract
We have calculated the equivalent widths of the absorption lines produced by Fe XXV and Fe XXVI in a Compton-thin, low-velocity photoionised material illuminated by the nuclear continuum in AGN. The results, plotted against the ionisation parameter and the column density of the gas, are a complement to those presented by Bianchi & Matt 2002 for the emission lines from the same ionic species. As an extension to the work by Bianchi & Matt 2002, 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.
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2 arXiv papers cite this in 6 sentences
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Cites it as background 1 paper
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In photoionized gas in particular, Fe K$α$ fluorescence emission may be dominated by the intercombination and forbidden transitions (e.g. for Fe xxv, see [ref] ; [ref] and references therein, see also [ref] ; [ref] for discussion of other He-like ions).
X-ray Absorption and Reflection in Active Galactic Nuclei · X-ray reprocessing in the Compton-thin regime · 0.84
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