Dust lanes, thick absorbers, and the unification model for Seyfert galaxies

A modification of the popular unification model for Seyfert galaxies is proposed, which takes into account recent observational findings on the statistical properties of both type 1 and type 2 Seyferts. In the proposed scenario, Compton-thick Seyfert 2 galaxies are those sources observed through compact, thick matter (the `torus'), while Compton-thin/intermediate Seyfert galaxies are obscured by dust lanes at larger distances.Comment: 4 pages, 1 figure. Accepted for publication in A&A Letter

A receding torus model for the Iwasawa-Taniguchi effect for Compton-thick AGN

Recently, Boorman et al. (2018) reported on the discovery of the Iwasawa-Taniguchi (I-T) effect (a.k.a. X-ray Baldwin effect) for Compton-thick AGN. They measured a decrease of the 6.4 keV iron line equivalent width with the 12mu luminosity, assumed as a proxy for the intrinsic X-ray luminosity, which in Compton-thick AGN is not directly observable. One of the most popular explanations of the classic I-T effect is the so-called receding torus model, i.e. the decrease of the covering factor of the molecular `torus' with X-ray luminosity. In this paper we show that an I-T effect for Compton-thick AGN is indeed expected in the receding torus model, assuming that the torus is funnelling the primary X-ray luminosity which is then scattered in a `hot mirror'. We found that the observed relation is well reproduced provided that the typical column density of the `hot mirror' is about 7.5x10^{22} cm^{-2}.Comment: 4 pages, 2 figures. Accepted for publication in MNRA

The properties of the absorbing and line emitting material in IGR J16318-4848

We have performed a detailed analysis of the XMM-Newton observation of IGR J16318-4848, to study the properties of the matter responsible for the obscuration and for the emission of Fe and Ni lines. Even if the line of sight material has a column density of about 2x10^24 cm^-2, from the Fe Kalpha line EW and Compton Shoulder we argue that the matter should have an average column density of a few x10^23 cm^-2, along with a covering factor of about 0.1-0.2. The iron Kalpha line varies on time scales as short as 1000 s, implying a size of the emitting region smaller than about 3x10^13 cm. The flux of the line roughly follows the variations of the continuum, but not exactly, suggesting a variation of the geometrical properties of the emitting region on similar time scales.Comment: accepted for publication in MNRAS, pink page

The iron Kalpha Compton Shoulder in transmitted and reflected spectra

We calculate the Equivalent Widht of the Core and the centroid energy and relative flux of the 1st order Compton Shoulder of the iron Kalpha emission line from neutral matter. The calculations are performed with Monte Carlo simulations. We explore a large range of column densities for both transmitted and reflected spectra, and study the dependence on the iron abundance. The Compton Shoulder is now becoming observable in many objects thanks to the improved sensitivity and/or energy resolution of XMM-Newton and Chandra satellites, and the present work aims to provide a tool to derive informations on the geometry and element abundances of the line emitting matter from Compton Shoulder measurements.Comment: 4 pages; accepted for publication in MNRA

The Contribution of the Obscuring Torus to the X--Ray Spectrum of Seyfert Galaxies: A Test for the Unification Model

The presence of an obscuring torus around the nucleus of Seyfert galaxies, as supposed in the popular unification scheme, can strongly modify the X--ray spectrum for both type 1 and 2 Seyfert galaxies. We find that if the torus is Compton thick, it can scatter at small angles a significant fraction of the nuclear radiation, and contribute to the continuum of Seyfert 1 galaxies above $\sim$10 keV, and to the fluorescence iron line at 6.4 keV. At large inclination angles and for large torus column densities, the spectrum is attenuated by photoabsorption and Compton scattering, while the iron fluorescence line produced by the torus can have large equivalent widths. Even after dilution by the continuum scattered by the warm material outside the torus, this iron line could be strong enough to explain the ``cold" component in the spectrum of NGC 1068. We stress that the complex pattern of the predicted variability can be a powerful tool for constraining the parameters of the model, such as the column density of the torus, its inclination and the amount of warm scattering material.Comment: 19 pages, Plain Tex, SISSA ref. 175/93/

X-ray spectra transmitted through Compton-thick absorbers

X-ray spectra transmitted through matter which is optically thick to Compton scattering are computed by means of Monte Carlo simulations. Applications to the BeppoSAX data of the Seyfert 2 galaxy in Circinus, and to the spectral modeling of the Cosmic X-ray Background, are discussed.Comment: 10 pages. Accepted for publication in New Astronom