Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006rmxac..26..208v&link_type=abstract
XI IAU Regional Latin American Meeting of Astronomy (Eds. L. Infante & M. Rubio) Revista Mexicana de Astronomía y Astrofísica (S
Astronomy and Astrophysics
Astronomy
Scientific paper
It is currently well established that the physical process responsible for the emission from the active nucleus of a galaxy is matter accretion into a supermassive black hole. In order to explain the differences observed in galaxies with active nuclei, Antonucci (1993) proposed the existence of a dusty torus beyond the accretion disk that absorbs a considerable fraction of the radiation emitted at wavelengths shorter than 1 μm (Unified Scheme). If we observe the torus face-on (i.e. the symmetry axis parallel to the line of sight) we will be observing the accretion disk and the broad line region (BLR), and the galaxy will be classified as type 1. On the other hand, if we observe the torus edge-on (i.e. the symmetry axis perpendicular to the line of sight), the central region will be hidden from our direct view and the galaxy will be classified as type 2. The dust in the vicinity of the active nucleus typically reaches temperatures of a few hundred degrees and therefore its emission peaks somewhere in the mid-infrared. It is therefore in this regime where the torus can be detected allowing us to determine its physical and geometrical properties. We want to unveil the properties of the dusty torus, and to do that we have obtained images of 50 Seyfert 2 (Sy 2) galaxies in 6 IR bands (J, H, K, L, M and N). We will separate the contribution of the host galaxy from the contribution of the nucleus (due to the torus) and compare its emission with theoretical models (Nenkova, Ivezic, & Elitzur 2002).
Lira Paulina
Videla Liza
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