Hostname: page-component-848d4c4894-xfwgj Total loading time: 0 Render date: 2024-06-22T12:40:36.866Z Has data issue: false hasContentIssue false
  • English
  • Français

The Kyoto 3-D Spectrograph and an Imaging Fabry-Perot Observation of the Nuclear Region of NGC 4151

Published online by Cambridge University Press:  12 April 2016

H. Ohtani ,
T. Ishigaki ,
T. Hayashi ,
S. Ozaki ,
T. Hattori ,
M. Sasaki ,
K. Aoki ,
M. Yoshida  and
E. Watanabe
H. Ohtani
Affiliation:
Department of Astronomy, Kyoto University, Kyoto 606-01, Japan
T. Ishigaki
Affiliation:
Department of Astronomy, Kyoto University, Kyoto 606-01, Japan
T. Hayashi
Affiliation:
Department of Astronomy, Kyoto University, Kyoto 606-01, Japan
S. Ozaki
Affiliation:
Department of Astronomy, Kyoto University, Kyoto 606-01, Japan
T. Hattori
Affiliation:
Department of Astronomy, Kyoto University, Kyoto 606-01, Japan
M. Sasaki
Affiliation:
Shimonoseki City University, Shimonoseki 751, Japan
K. Aoki
Affiliation:
National Astronomical Observatory, Mitaka 181, Japan
M. Yoshida
Affiliation:
Okayama Astrophysical Observatory, Kamogata 719-02, Japan
E. Watanabe
Affiliation:
Okayama Astrophysical Observatory, Kamogata 719-02, 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.

The Kyoto 3-D Spectrograph was commissioned successfully at the 188-cm telescope of the Okayama Astrophysical Observatory in the spring of 1996. This instrument has four distinct modes (Ohtani et al. 1994): (1) narrow-band imager, which is an ordinary focal-reducer camera; (2) Spectro-NebulaGraph (long-slit spectrograph; Kosugi et al. 1995); (3) imaging Fabry-Perot interferometer, using either of two Fabry-Perot etalons from Queensgate Instruments (a tunable filter with R = 300 and another with R = 7000 for velocity-field observations. Broad-band (400–700 nm) coatings are deposited on both etalons. During observations, the etalon temperature is stabilized within 0.5°C); and (4) integral-field spectrograph of the TIGER-type (Bacon et al. 1995). In this mode, the spectra of 7 × 11 objects can be recorded simultaneously, along with 7 × 2 spectra of the sky 4′ away. The spatial resolution is 1″.3 and the field of view is 9″ × 14″.

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. 355 - 356
Copyright
Copyright © Astronomical Society of the Pacific 1997

References

Bacon, R., et al. 1995, A&AS, 113, 347.Google Scholar
Kosugi, G., et al. 1995, PASP, 711, 475.Google Scholar
Ohtani, H., et al. 1994, in Instrumentaion in Astronomy VIII, Proc. SPIE Symp. Vol. 2198, 229.Google Scholar
Robinson, A., et al., 1994, A&A, 291, 351.Google Scholar
Schulz, H. 1990, AJ, 99, 1442.CrossRefGoogle Scholar
Ulrich, M. 1973, ApJ, 181, 51.Google Scholar