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AKARI observations of the multiphase intergalactic medium of Stephan's Quintet

Published online by Cambridge University Press:  17 August 2012

Toyoaki Suzuki ,
Hidehiro Kaneda ,
Takashi Onaka  and
Tetsu Kitayama
Toyoaki Suzuki
Affiliation:
Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3–1–1 Yoshinodai, Chuo-ku, Sagamihara, Kanagawa 252–5210, Japan email: [email protected]
Hidehiro Kaneda
Affiliation:
Graduate School of Science, Nagoya University, Furu-cho, Chikusa-ku, Nagoya 464–8602, Japan
Takashi Onaka
Affiliation:
Department of Astronomy, Graduate School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan
Tetsu Kitayama
Affiliation:
Department of Physics, Toho University, Funabashi, Chiba 274-8510, Japan
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Abstract

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Stephan's Quintet (SQ, HCG92) is a well studied compact group of galaxies with a disturbed intergalactic medium (IGM). An “intruder” galaxy NGC 7318b is currently colliding with the IGM at a relative velocity of 1000 km s−1, causing a large-scale shock front. We observed SQ with the Far-Infrared Surveyor (FIS) aboard AKARI in four far-infrared (far-IR) bands at 65, 90, 140, and 160μm. The 160μm image clearly shows an additional peak of emission overlying structure extending in the North-South direction along the shock ridge seen in the 140μm band, and in H2 and X-ray emission. Whereas most of the far-IR emission in the shocked region is from cold dust (20 K), the [CII]158μm emission - whose luminosity is comparable to that of the warm H2 gas - can significantly contribute to the single peak emission in the 160μm band. We conclude that the [CII] line emission comes from the warm H2 gas in the shock. Our result represents the first detection of shock-excited [CII] line emission.

Keywords

ISM: structure - galaxies: individual - galaxies: interactions - infrared: ISM
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S284: The Spectral Energy Distribution of Galaxies , September 2011 , pp. 342 - 344
Copyright
Copyright © International Astronomical Union 2012

References

Allen, R. J. & Hartsuiker, J. W. 1972, Nature, 239, 324CrossRefGoogle Scholar
Appleton, P. N. et al. 2006, Ap. Lett., 639, L51.CrossRefGoogle Scholar
Boselli, A., Gavazzi, G., Lequeux, J., & Pierini, D. 2002, A&A, 385, 454Google Scholar
Cardelli, J. A., Meyer, D. M., Jura, M., & Savage, B. D. 1996, ApJ, 467, 334CrossRefGoogle Scholar
Cluver, M. E. et al. 2010, ApJ, 710, 248Google Scholar
Hickson, P. 1982, ApJ, 255, 382Google Scholar
Hickson, P., Mendes de Oliveira, C., Huchra, J. P., & Palumbo, G. G. 1992, ApJ, 399, 353CrossRefGoogle Scholar
Kawada, M. et al. 2007, PASJ, 59, 389Google Scholar
Langer, W. D., Velusamy, T., Pineda, J. L., Goldsmith, P. F., Li, D., & Yorke, H. W. 2010, A&A, 521L, 17L.Google Scholar
Murakami, H. et al. 2007, PASJ, 59, 369Google Scholar
Pietsch, W., Trinchieri, G., Arp, H., & Sulentic, J. W. 1997, A&A, 322, 89Google Scholar