Astronomy and Astrophysics – Astrophysics
Scientific paper
2002-02-21
Astronomy and Astrophysics
Astrophysics
20 pages, 14 figures, A&A, accepted
Scientific paper
10.1051/0004-6361:20020170
We present the analysis of 31 observations of 20 bright Compton thin Seyfert 2s, in the 0.1-200 keV band, performed with the BeppoSAX satellite. The sample consists of all Seyfert 2s in the BeppoSAX public archive, with a 2-10 keV flux higher than 5x10^(-12) erg/cm^2/s. The good statistics available and the broad energy band permit a detailed study of the main continuum components of these sources, i.e. the primary power-law, the reflected component, the soft emission and the high-energy cut-off. The main results of our analysis are: (1) the 3-200 keV intrinsic power-law has a mean photon index Gamma=1.79+-0.01, with a dispersion of sigma=0.23. (2) The high-energy exponential cut-off at E~100-300 keV is not an ubiquitous property of Seyfert galaxies: in ~30% of the objects the continuum power-law does not drop up to energies of 300 keV or more. (3) A reflected component is present in almost all the sources (17 out of 21). The small variations of this component with respect to the intrinsic continuum, in objects with multiple observations, suggests that the reflector is not the accretion disk, but must be located much farther from the nucleus. (4) The range of ratios between the reflected and intrinsic components suggests that the circumnuclear medium is not homogeneous, and a significant fraction of the solid angle is covered by a gas thicker than that along the line of sight. (5) The iron Kalpha line is present is all but one the sources. The equivalent width is in the typical range of Seyfert 1s (EW=100-300 eV) in sources with low absorption (N_H < 3x10^23 cm^(-2)), and increases in more absorbed objects, as expected according to unified models. (6) The energy resolution of BeppoSAX is in general too low to measure the iron line width. However, in 6 cases we measured a significant line broadening.
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