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

  • H. Ohtani (a1), T. Ishigaki (a1), T. Hayashi (a1), S. Ozaki (a1), T. Hattori (a1), M. Sasaki (a2), K. Aoki (a3), M. Yoshida (a4) and E. Watanabe (a4)...

Extract

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″.

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References

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

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