Volume 548, December 2012
|Number of page(s)||19|
|Published online||19 November 2012|
Jet and torus orientations in high redshift radio galaxies⋆
European Southern Observatory,
Karl Schwarzschild Straße 2,
Garching bei München,
2 Institut d’Astrophysique de Paris, 98bis boulevard Arago, 75014 Paris, France
3 CSIRO Astronomy & Space Science, PO Box 76, Epping, NSW 1710, Australia
4 Jet Propulsion Laboratory, California Institute of Technology, Mail Stop 169-221, Pasadena, CA 91109, USA
5 Astronomisches Institut, Ruhr-Universität Bochum, Universitätstr. 150, 44801 Bochum, Germany
6 Oceanit Laboratories, 828 Fort Street Mall, Suite 600, Honolulu, HI 96813, USA
Received: 19 July 2012
Accepted: 19 September 2012
We examine the relative orientation of radio jets and dusty tori surrounding the active galactic nucleus (AGN) in powerful radio galaxies at z > 1. The radio core dominance serves as an orientation indicator, measuring the ratio between the anisotropic Doppler-beamed core emission and the isotropic lobe emission. Assuming a fixed cylindrical geometry for the hot, dusty torus, we derive its inclination i by fitting optically-thick radiative transfer models to spectral energy distributions obtained with the Spitzer Space Telescope. We find a highly significant anti-correlation (p < 0.0001) between R and i in our sample of 35 type 2 AGN combined with a sample of 18 z ~ 1 3CR sources containing both type 1 and 2 AGN. This analysis provides observational evidence both for the Unified scheme of AGN and for the common assumption that radio jets are in general perpendicular to the plane of the torus. The use of inclinations derived from mid-infrared photometry breaks several degeneracies which have been problematic in earlier analyses. We illustrate this by deriving the core Lorentz factor Γ from the R-i anti-correlation, finding Γ ≳ 1.3.
Key words: galaxies: high-redshift / galaxies: active / radio continuum: galaxies / infrared: galaxies / galaxies: jets / quasars: general
Figures 11, 12, and Tables 1, 2, 6 are available in electronic form at http://www.aanda.org
© ESO, 2012
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