Hostname: page-component-586b7cd67f-dlnhk Total loading time: 0 Render date: 2024-11-29T19:19:19.440Z Has data issue: false hasContentIssue false
  • English
  • Français

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 ,
G. Kosugi  and
K. Aoki
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

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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
Information
International Astronomical Union Colloquium , Volume 159: Emission Lines in Active Galaxies: New Methods and Techniques , 1997 , pp. 353 - 354
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.Google Scholar
Kosugi, G., et al. 1995, PASP, 107, 475.Google Scholar