Volume 479, Number 2, February IV 2008
|Page(s)||389 - 396|
|Published online||04 December 2007|
Institut für Theoretische Physik und Astrophysik, Christian-Albrechts-Universität zu Kiel, Leibnizstr. 15, 24098 Kiel, Germany e-mail: firstname.lastname@example.org
2 Zentrum für Astronomie, ITA, Universität Heidelberg, Albert-Ueberle-Str. 2, 69120 Heidelberg, Germany
3 European Southern Observatory, Casilla 19001, Santiago 19, Chile
4 RIKEN Cosmic Radiation Lab, 2-1 Hirosawa, Wakoshi Saitama 351-0198, Japan
5 Steward Observatory, The University of Arizona, 933 N. Cherry Ave, Tucson, AZ 85721, USA
Accepted: 15 November 2007
Aims.We investigate mid-infrared and X-ray properties of the dusty torus invoked in the unification scenario for active galactic nuclei by using the relation between mid IR and hard X-ray luminosities to constrain the geometry and physical state of the dusty torus.
Methods.We present new VISIR observations of 17 nearby AGN and combined these with our earlier VISIR sample of 8 Seyfert galaxies. After combining these observations with X-ray data from the literature, we studied the correlation between their mid IR and hard X-ray luminosities.
Results.A statistically highly significant correlation is found between the rest frame m () and 2-10 keV () luminosities. Furthermore, with a probability of 97%, we find that Sy 1 and Sy 2 nuclei have the same distribution of over .
Conclusions.The high resolution of our MIR imaging allows us to exclude any significant non-torus contribution to the AGN mid IR continuum, thereby implying that the similarity in the / ratio between Sy 1s and Sy 2s is intrinsic to AGN. We argue that this is best explained by clumpy torus models. The slope of the correlation is in good agreement with the expectations from the unified scenario and indicates little to no change in the torus geometry with luminosity. In addition, we demonstrate that the high angular resolution is crucial for AGN studies in the IR regime.
Key words: galaxies: active / infrared: galaxies / X-rays: galaxies
© ESO, 2008
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