On the Anomalous Silicate Absorption Feature of the Prototypical Type-2 AGN NGC 1068

Details On the Anomalous Silicate Absorption Feature of the Prototypical Type-2 AGN NGC 1068 On the Anomalous Silicate Absorption Feature of the Prototypical Type-2 AGN NGC 1068

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21541121k&link_type=abstract

American Astronomical Society, AAS Meeting #215, #411.21; Bulletin of the American Astronomical Society, Vol. 42, p.243

Astronomy and Astrophysics

Astronomy

Scientific paper

The first detection of the silicate absorption feature in AGNs was made at 9.7 micrometer for the prototypical Seyfert 2 galaxy NGC 1068 over 30 years ago by Rieke & Low (1975) and Kleinmann et al. (1976), indicating the presence of a large column of silicate dust in the line-of-sight to the nucleus. It is known now that most of the type 2 AGNs display
silicate absorption bands, while the silicate features of type 1 AGNs appear in emission.
Recently, using the Mid-Infrared Interferometric Instrument (MIDI) on the ESO's Very Large Telescope Interferometer (VLTI), Jaffe et al. (2004) by the first time spatially resolved the parsec-sized dust torus around NGC 1068 and found that the 10 micrometer silicate absorption feature of the innermost hot component exhibits an anomalous profile differing from that of the interstellar medium: the 9.7 micrometer silicate absorption spectrum of NGC 1068 shows a relatively flat profile from 8 to 9 micrometer and then a sharp drop between 9 and 10 micrometer probably indicative of gehlenite (Ca2Al2SiO7), a calcium aluminium silicate species; in comparison, the Galactic silicate absorption profiles begin to drop already at about 8 micrometer (Jaffe et al. 2004).
We propose a dust model consisting of a mixture of silicon carbide and gehlenite to closely reproduce the observed spectrum while satisfying the cosmic abundance constraints.

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