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Astron. Nachr. / AN 326 (2005), Suppl. Issue 7 -- Short Contributions AG 2005 KÆln 1
Infrared Interferometry of the Seyfert Galaxy NGC 1068
G. WEIGELT 1 , Y. Y. BALEGA 2 , T. BECKERT 1 , W. J. DUSCHL 3 ,
K.­H. HOFMANN 1 , A. B. MEN'SHCHIKOV 4 , D. SCHERTL 1 , M. WITTKOWSKI 5
1 Max­Planck Institut fÝr Radioastronomie, Auf dem HÝgel 69, 53121 Bonn, Germany
2 Special Astrophysical Observatory, Nizhnij Arkhyz, Zelenchuk region, Karachai­Cherkesia 357147, Russia
3 Institut fÝr Theoretische Astrophysik, UniversitÄt Heidelberg, Albert­Ueberle­Str. 2, 69120 Heidelberg, Ger­
many
4 Institute for Computational Astrophysics, Saint Mary's University, Halifax, NS B3H 3C3, Canada
5 European Southern Observatory, Karl­Schwarzschild­Str. 2, 85748 Garching, Germany
Infrared interferometry is able to resolve the innermost region surrounding the accretion disk of AGN. H­ and
K­band bispectrum speckle interferometry of the nuclear region of NGC 1068 with the SAO 6 m telescope
(Wittkowski et al., 1998; Weigelt et al., 2004) allowed the reconstruction of the first diffraction­limited K­band
image of NGC 1068's elongated core with a resolution of 76 mas and the first H­band image with 57 mas
resolution. The compact, elongated core has a north­western, tail­shaped extension. The K­band FWHM diameter
of this compact core is 18 x 39 mas (± 4 mas) or 1.3â2.8 pc, and the position angle (PA) of the north­western
extension is ­16 degrees. This PA is very similar to the PA of the western wall of the ionization cone. This
suggests that the H­ and K­band emission from the compact core is both thermal emission and scattered light
from dust near the western wall of a low­density, conical cavity or from the innermost region of a parsec­scale
dusty torus that is heated by the central source (the dust sublimation radius of NGC 1068 is approximately 0.1
­ 1 pc). First long­baseline interferometry of NGC 1068 in the near­infrared K band (Wittkowski et al., 2004;
VINCI beam combiner instrument) and in the mid­infrared (Jaffe et al., 2004; MIDI beam combiner) has been
carried out with two 8.2 m Unit Telescopes of ESO's VLT Interferometer. The VINCI K­band observations show
that the squared visibility amplitude of NGC 1068 is approximately 0.16 at a projected baseline of 46 m. This
visibility corresponds to a substructure of less than 5 mas or 0.4 pc.
REFERENCES
W. Jaffe et al., 2004, Nature 429, 47
G. Weigelt et al., 2004, A&A 425, 77
M. Wittkowski, Y. Balega, T. Beckert, W. Duschl, K. Hofmann, G. Weigelt, 1998, A&A 329, L45
M. Wittkowski, P. Kervella, R. Arsenault, F. Paresce, T. Beckert, G. Weigelt, 2004, A&A 418, L39