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Proceedings Paper

Kyoto Tridimensional Spectrograph II
Author(s): Hajime Sugai; Hiroshi Ohtani; Tsuyoshi Ishigaki; Tadashi Hayashi; Shinobu Ozaki; Takashi Hattori; Motomi Ishii; Minoru Sasaki; Norihide Takeyama
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Paper Abstract

We are building the second version of the Kyoto Tridimensional Spectrograph (Ohtani et al., this symposium). This will be mounted on the MAGNUM, a 2-m telescope under construction at Haleakala, and also on the SUBARU. The spectrograph has four observational modes: Fabry-Perot imager, integral field spectrograph (IFS) with a microlens array, long-slit spectrograph, and filter-imaging modes. The new spectrograph is significantly better than the first version in several ways. The IFS has as many as 37 X 37 microlenses, each of which subtends 0' .39 at the MAGNUM. The optics is designed to be used in wide wavelength ranges from 360 nm to 900 nm. The transmission at any wavelength between 370 and 900 nm is designed to exceed 50% for the collimator plus camera system, and to reach almost 40% even at 360 nm. In order to achieve high efficiency at short wavelengths, we use an anti- reflection coated backside-illuminated 2K X 2K CCD. We are also planning a further improvement by using multi-layer anti- reflection coatings for lenses, in collaboration with National Astronomical Observatory, Japan. In order to assure good image quality under a severe weight limit of 150 kg for this instrument, we have carried out mechanical design by calculating the flexure of the instrument for all telescope attitudes with finite element analysis, and succeeded in limiting the maximum flexure to 30 micrometer. This does not degrade image quality. The movements on the CCD of the light from the center of the focal plane have also been simulated, depending on the telescope attitudes. This is important to obtain not only a good image, but also a correct flat field and wavelength calibration in the IFS mode. The movements are expected to be confined almost within one pixel for an attitude, which is considered to be small enough.

Paper Details

Date Published: 9 July 1998
PDF: 10 pages
Proc. SPIE 3355, Optical Astronomical Instrumentation, (9 July 1998); doi: 10.1117/12.316800
Show Author Affiliations
Hajime Sugai, Kyoto Univ. (Japan)
Hiroshi Ohtani, Kyoto Univ. (Japan)
Tsuyoshi Ishigaki, Kyoto Univ. (Japan)
Tadashi Hayashi, Kyoto Univ. (Japan)
Shinobu Ozaki, Kyoto Univ. (Japan)
Takashi Hattori, Kyoto Univ. (Japan)
Motomi Ishii, Kyoto Univ. (Japan)
Minoru Sasaki, Shimonoseki City Univ. (Japan)
Norihide Takeyama, Genesia Corp. (Japan)


Published in SPIE Proceedings Vol. 3355:
Optical Astronomical Instrumentation
Sandro D'Odorico, Editor(s)

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