Deep X-ray spectroscopy and imaging of the Seyfert 2 galaxy, ESO 138-G001

We present a spectral and imaging analysis of the XMM–Newton and Chandra observations of the Seyfert 2 galaxy ESO138-G001, with the aim of characterizing the circumnuclear material responsible for the soft (0.3–2.0 keV) and hard (5–10 keV) X-ray emission. We confirm that the source is absorbed by Co...

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Bibliographic Details
Published in:Monthly notices of the Royal Astronomical Society 2015-10, Vol.453 (2), p.2155-2162
Main Authors: De Cicco, M., Marinucci, A., Bianchi, S., Piconcelli, E., Violino, G., Vignali, C., Nicastro, F.
Format: Article
Language:English
Subjects:
Density
Emission
Emissions
Imaging
Iron
Line of sight
Seyfert galaxies
Spectrum analysis
Stars & galaxies
X-ray astronomy
X-rays
XMM (spacecraft)
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Summary:We present a spectral and imaging analysis of the XMM–Newton and Chandra observations of the Seyfert 2 galaxy ESO138-G001, with the aim of characterizing the circumnuclear material responsible for the soft (0.3–2.0 keV) and hard (5–10 keV) X-ray emission. We confirm that the source is absorbed by Compton-thick gas. However, if a self-consistent model of reprocessing from cold toroidal material is used (mytorus), a possible scenario requires the absorber to be inhomogenous, its column density along the line of sight being larger than the average column density integrated over all lines of sight through the torus. The iron emission line may be produced by moderately ionized iron (Fe xii-Fe xiii), as suggested by the shifted centroid energy and the low K β/K α flux ratio. The soft X-ray emission is dominated by emission features, whose main excitation mechanism appears to be photoionization, as confirmed by line diagnostics and the use of self-consistent models (cloudy).
ISSN:0035-8711
1365-2966
DOI:10.1093/mnras/stv1702