Silicate emissions in active galaxies - From LINERs to QSOs

Details Silicate emissions in active galaxies - From LINERs to QSOs Silicate emissions in active galaxies - From LINERs to QSOs

2005-06-29

arxiv.org/abs/astro-ph/0506716v1

Astrophys.J.629:L21-L24,2005

Astronomy and Astrophysics

Astrophysics

Accepted by ApJL, 10 pages, 2 eps figures

Scientific paper

10.1086/444359

We report the first detection of ~10 and ~18 micron silicate dust emissions in a low-luminosity active galactic nucleus (AGN), obtained in Spitzer-IRS 7-37 micron spectroscopy of the Type 1 LINER galaxy NGC3998. Silicate emissions in AGN have only recently been detected in several quasars. Our detection counters suggestions that silicate emissions are present only in the most luminous AGN. The silicate features may be signatures of a dusty ``obscuring torus'' viewed face-on as postulated for Type 1 AGN. However, the apparently cool (~200 K) dust is inconsistent with theoretical expectations of much hotter torus walls. Furthermore, not all Type 1 objects are silicate emission sources. Alternatively, the silicate emission may originate in dust not directly associated with a torus. We find that the long-wavelength (>20 micron) tail of the emission in NGC3998 is significantly weaker than in the sample of bright QSOs recently presented by Hao et al. The 10 micron profile in our NGC3998 spectrum is inconsistent with ``standard'' silicate ISM dust. This may indicate differences in the dust composition, grain size distribution, or degree of crystallization. The differences between NGC3998, QSOs, and Galactic templates suggest that there are significant environmental variations.

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