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Astron. Astrophys. 318, L1-L4 (1997)

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Letter to the Editor

Mid-infrared spectroscopy of the hyperluminous infrared galaxy IRAS P09104+4109 *

Y. Taniguchi , Y. Sato 1, 2, K. Kawara 1, T. Murayama 3, 4 and H. Mouri 1, 5

1 Astronomical Institute, Tohoku University, Aoba, Sendai 980-77, Japan
2 Royal Greenwich Observatory, Madingley Road, Cambridge CB3 0EZ, UK
3 ISO Science Operations Centre, Astrophysics Division of ESA, Villafranca, 28080 Madrid, Spain
4 Institute of Space and Astronautical Science, Yoshinodai, Sagamihara, Kanagawa 229, Japan
5 Meteorological Research Institute, 1-1 Nagamine, Tsukuba 305, Japan

Received 25 October 1996 / Accepted 26 November 1996


We present mid-infrared spectroscopy of the hyperluminous infrared galaxy IRAS 09104+4109 based on observations with ISOCAM CVF. We have detected the emission peak around 8 µm as well as the absorption feature around 10 µm possibly due to silicate, providing evidence for a dusty torus around the central engine. Comparing the observational results with the dusty torus model studied by Pier & Krolik (1992), we show that the most mid infrared emission comes from a compact (a few pc in radius) dusty torus although the excess far infrared emission suggests the presence of an extended dusty torus with radius of [FORMULA] 100 pc.

Key words: hyperluminous infrared galaxy (IRAS P09104+4109) – active galactic nuclei – infrared emission

* Based on observations with ISO, an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, the Netherlands, and the United Kingdom) and with the participation of ISAS and NASA.

Send offprint requests to: Y. Taniguchi

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© European Southern Observatory (ESO) 1997

Online publication: July 8, 1998