Kyoto Tridimensional Spectrograph II

Hajime Sugai; Hiroshi Ohtani; Tsuyoshi Ishigaki; Tadashi Hayashi; Shinobu Ozaki; Takashi Hattori; Motomi Ishii; Minoru Sasaki; Norihide Takeyama

doi:10.1117/12.316800

9 July 1998 Kyoto Tridimensional Spectrograph II

Hajime Sugai, Hiroshi Ohtani, Tsuyoshi Ishigaki, Tadashi Hayashi, Shinobu Ozaki, Takashi Hattori, Motomi Ishii, Minoru Sasaki, Norihide Takeyama

Author Affiliations +

Proceedings Volume 3355, Optical Astronomical Instrumentation; (1998) https://doi.org/10.1117/12.316800
Event: Astronomical Telescopes and Instrumentation, 1998, Kona, HI, United States

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.

Citation Download Citation

Hajime Sugai, Hiroshi Ohtani, Tsuyoshi Ishigaki, Tadashi Hayashi, Shinobu Ozaki, Takashi Hattori, Motomi Ishii, Minoru Sasaki, and Norihide Takeyama "Kyoto Tridimensional Spectrograph II", Proc. SPIE 3355, Optical Astronomical Instrumentation, (9 July 1998); https://doi.org/10.1117/12.316800

ACCESS THE FULL ARTICLE

INSTITUTIONAL
Select your institution to access the SPIE Digital Library.

SELECT YOUR INSTITUTION

PERSONAL
Sign in with your SPIE account to access your personal subscriptions or to use specific features such as save to my library, sign up for alerts, save searches, etc.

PERSONAL SIGN IN

No SPIE Account? Create one

PURCHASE THIS CONTENT

SUBSCRIBE TO DIGITAL LIBRARY

50 downloads per 1-year subscription

Members: $195

Non-members: $335 ADD TO CART

25 downloads per 1 - year subscription

Members: $145

Non-members: $250 ADD TO CART

PURCHASE SINGLE ARTICLE

Includes PDF, HTML & Video, when available