Radiative transfer in clumpy tori: what happens to the 10-μm feature?

Details Radiative transfer in clumpy tori: what happens to the 10-μm feature? Radiative transfer in clumpy tori: what happens to the 10-μm feature?

Apr 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aipc..761..269d&link_type=abstract

THE SPECTRAL ENERGY DISTRIBUTIONS OF GAS-RICH GALAXIES: Confronting Models with Data; International Workshop. AIP Conference Pr

Computer Science

Galactic Nuclei, Circumnuclear Matter, And Bulges, Radiative Transfer, Scattering, Interstellar Dust Grains, Diffuse Emission, Infrared Cirrus, Active And Peculiar Galaxies And Related Systems

Scientific paper

We present radiative transfer models of clumpy dust tori around AGN. We address the question whether, as argued by Nenkova, Ivezic & Elitzur (henceforth NIE02), the infrared spectral properties of AGN are better explained by a clumpy dust distribution than a smooth one, in particular with regard to the 10 μm silicate feature. In contrast to NIE02 our calculations are based on multi-dimensional radiative transfer of the entire ensemble of clumps, albeit at present in axisymmetey (i.e. clumps are approximated as rings around the polar axis). We find that the 10 μm absorption feature in edge-on objects (Seyfert 2) is less deep for the clumpy models. As for the 10 μm emission feature in face-on (Seyfert 1) objects, we find no clear systematic weakening of this feature in our clumpy models in comparison to the smooth models, as was found by NIE02. We therefore question whether the absense of 10 μm emission in Seyfert 1 AGN points to clumpiness. We do not, however, dispute the clumpiness itself: we merely call for caution in the interpretation of infrared spectral data.

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