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Tri-dimensional Spectroscopy of the Seyfert Galaxy NGC 1275: Kinematics and Excitation of the Cooling-Flow Gas

Published online by Cambridge University Press:  12 April 2016

M. Yoshida
Affiliation:
Okayama Astrophysical Observatory, Kamogata-cho, Asakuchi-gun, Okayama 719-02, Japan
G. Kosugi
Affiliation:
National Astronomical Observatory of Japan, Mitaka, Tokyo 181, Japan
K. Aoki
Affiliation:
National Astronomical Observatory of Japan, Mitaka, Tokyo 181, Japan
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Extract

NGC 1275, the Perseus cluster cD galaxy, is a well-known Seyfert 1 galaxy and also one of the strongest extragalactic radio sources (3C84). Although many studies have been done on the extended optical emission-line region of NGC 1275, which is thought to be associated with the X-ray cooling-flow phenomenon (e.g., Heckman et al. 1989, Ferruit and Pecontal 1994), the excitation mechanism of the emission-line gas and two-dimensional gas kinematics are still unclear. We made tri-dimensional spectroscopy of NGC 1275 in order to reveal two-dimensional kinematics and- the relation between the gas motion and the excitation of the emission lines.

Type
VI. The Narrow-Line Regions and Beyond
Copyright
Copyright © Astronomical Society of the Pacific 1997

References

Ferruit, P., & Pécontal, E. 1994, A&A, 288, 65.Google Scholar
Heckman, T., et al. 1989, ApJ, 338, 48.CrossRefGoogle Scholar
Inoue, M., et al. 1996, AJ, 111, 1852.CrossRefGoogle Scholar
Kosugi, G., et al. 1995, PASP, 107, 475.CrossRefGoogle Scholar

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Tri-dimensional Spectroscopy of the Seyfert Galaxy NGC 1275: Kinematics and Excitation of the Cooling-Flow Gas
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