Volume 473, Number 1, October I 2007
|Page(s)||67 - 76|
|Published online||26 June 2007|
A 100 ks XMM-Newton view of the Seyfert 1.8 ESO 113-G010
Discovery of large X-ray variability and study of the Fe K line complex
Observatoire Astronomique de Strabsourg, Université Louis Pasteur, CNRS, 11 rue de l'Université, 67000 Strasbourg, France e-mail: email@example.com
2 School of Physics and Astronomy, University of Southampton, Southampton SO17 1BJ, UK
3 Laboratory for High Energy Astrophysics, Code 662, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
4 Dept. of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA
5 Astronomy Group, School of Geographical and Physical Sciences, University of Keele, Keele, Staffordshire ST5 5BG, UK
6 Dipartimento di Fisica, Università degli Studi Roma Tre, via della Vasca Navale 84, 00146 Roma, Italy
7 Dept. of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK
8 Centre d'Étude Spatiale des Rayonnements, 9 avenue du Colonel Roche, BP 4346, 31028 Toulouse Cedex 4, France
9 Dept. of Physics, University of Maryland Baltimore County, 1000 Hilltop Circle, Baltimore, MD 21250, USA
Accepted: 18 June 2007
Context.The Seyfert 1.8 galaxy ESO 113-G010 had been observed for the first time above 2 keV by XMM-Newton during a short exposure (~4 ks) in May 2001. In addition to a significant soft X-ray excess, it showed one of the strongest (in EW) redshifted Fe Kα lines, at 5.4 keV.
Aims.We present here a long (100 ks) XMM-Newton follow-up of this source performed in November 2005, in order to study over a longer time-scale its main X-ray properties.
Methods.We use both timing analysis (Power Spectra Density analysis, rms spectra, flux-flux analysis) and spectral analysis which mainly focuses on the Fe Kα line complex.
Results.The source was found in a higher/softer time-averaged flux state, and timing analysis of this source reveals strong, rapid variability. The Power Spectral Density (PSD) analysis indicates (at 95% confidence level) a break at 3.7 10-4 Hz. This cut-off frequency is comparable to those measured in some other rapidly-variable Seyferts, such as MCG–6-30-15 and NGC 4051. From the mass-luminosity-time-scale, we infer that MBH ranges from 4 106–107 and the source is accreting at or close to the Eddington rate (or even higher). The existing data cannot distinguish between spectral pivoting of the continuum and a two-component origin for the spectral softening, primarily because the data do not span a broad enough flux range. In the case of the two-component model, the fractional offsets measured in the flux-flux plots increase significantly toward higher energies (similar to what is observed in MCG–6-30-15) as expected if there exists a constant reflection component. Contrary to May 2001, no significant highly redshifted emission line is observed (which might be related to the source flux level), while two narrow emission lines at about 6.5 keV and 7 keV are observed. The is not high enough to establish if the lines are variable or constant. As already suggested by the 2001 observation, no significant constant narrow 6.4 keV Fe Kα line (EW ≤ 32 eV) is observed, hence excluding any dominant emission from distant cold matter such as a torus in this Seyfert type 1.8 galaxy.
Key words: galaxies: Seyfert / galaxies: active / X-rays: galaxies / accretion, accretion disks / quasars: individual: ESO 113-G010
© ESO, 2007
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