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Proceedings Paper

Narrowband filter system at the Subaru prime focus
Author(s): Tomoki Hayashino; Yoshiaki Taniguchi; Tohru Yamada; Yasuhiro Shioya; Tohru Nagao; Toshimitsu Yoshida; Mamoru Doi; Kazuhiro Shimasaku; Yutaka Komiyama; Fumiaki Nakata; Hisanori Furusawa; Hitohiko Kimura; Masami Ouchi; Tsutomu Aoki; Masaru Hamabe; Keiichi Kodaira; Satoshi Miyazaki; Naruhisa Takato; Masafumi Yagi; Naoki Yasuda; Masaki Sekiguchi; Sadanori Okamura
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Paper Abstract

The Subaru telescope has an excellent performance of wide field of view at the prime focus. A big area of 30 feet times 24 feet is observable at a time with the prime focus camera. Making the best use of the wide view, we are constructing narrowband (NB) filter system consisting of 20 bands. This system covers the wavelengths between 4,000 angstrom and 10,000 angstrom. The band width (BW) varies form 200 angstrom to 400 angstrom depending on the center wavelength (CW). The resolving power of the system is 23. Each filter has a big dimension of 205mm times 170mm and excellent uniformities on CW, BW and peak transmittance. Employing this filter system, spectroscopy for all objects recorded in fields of view is possible at the wavelength resolution of R23. The limiting magnitude would reach 27AB in reasonable observation time even at long wavelength bands. Such deep NB imaging spectroscopic survey should provide huge catalogue on cosmological objects. Especially, photometric redshift analyses with higher spectral resolution of R23 than ordinary broadband system of R approximately equals 4, will revolutionarily develop studies on formation and evolution of galaxies together with search for large scale structures at high redshift, based on enormous statistics, for example, 104 or more galaxies at high redshift of z > 3. Also, a lot of objects having strong emission lines as QSO/AGNs and Ly(alpha) or more galaxies will be discovered, because NB filter is strong in detection of emission line. The use of NB filter is strong in detection of emission line. The use of NB filter system in survey observations is surely quite conservative in concept and time consuming in general. However, combining this method with the wide field of view provided in the largest class telescope, new window to the universe is going to open.

Paper Details

Date Published: 16 August 2000
PDF: 8 pages
Proc. SPIE 4008, Optical and IR Telescope Instrumentation and Detectors, (16 August 2000); doi: 10.1117/12.395498
Show Author Affiliations
Tomoki Hayashino, Tohoku Univ. (Japan)
Yoshiaki Taniguchi, Tohoku Univ. (Japan)
Tohru Yamada, Tohoku Univ. (Japan)
Yasuhiro Shioya, Tohoku Univ. (Japan)
Tohru Nagao, Tohoku Univ. (Japan)
Toshimitsu Yoshida, Tohoku Univ. (Japan)
Mamoru Doi, Univ. of Tokyo (Japan)
Kazuhiro Shimasaku, Univ. of Tokyo (Japan)
Yutaka Komiyama, Univ. of Tokyo (United States)
Fumiaki Nakata, Univ. of Tokyo (Japan)
Hisanori Furusawa, Univ. of Tokyo (Japan)
Hitohiko Kimura, Univ. of Tokyo (Japan)
Masami Ouchi, Univ. of Tokyo (Japan)
Tsutomu Aoki, Univ. of Tokyo (Japan)
Masaru Hamabe, Univ. of Tokyo (Japan)
Keiichi Kodaira, National Astronomical Observatory of Japan (Japan)
Satoshi Miyazaki, National Astronomical Observatory of Japan (Japan)
Naruhisa Takato, National Astronomical Observatory of Japan (United States)
Masafumi Yagi, National Astronomical Observatory of Japan (Japan)
Naoki Yasuda, National Astronomical Observatory of Japan (Japan)
Masaki Sekiguchi, Univ. of Tokyo (Japan)
Sadanori Okamura, Univ. of Tokyo (Japan)

Published in SPIE Proceedings Vol. 4008:
Optical and IR Telescope Instrumentation and Detectors
Masanori Iye; Alan F. M. Moorwood, Editor(s)

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