Hyper Suprime-Cam

被引：261

作者：

Miyazaki, Satoshi ^{[1
]}

Komiyama, Yutaka ^{[1
]}

Nakaya, Hidehiko ^{[1
]}

Kamata, Yukiko ^{[1
]}

Doi, Yoshi ^{[1
]}

Hamana, Takashi ^{[1
]}

Karoji, Hiroshi

Furusawa, Hisanori ^{[1
]}

Kawanomoto, Satoshi ^{[1
]}

Morokuma, Tomoki

Ishizuka, Yuki ^{[1
]}

Nariai, Kyoji ^{[1
]}

Tanaka, Yoko ^{[1
]}

Uraguchi, Fumihiro ^{[1
]}

Utsumi, Yosuke ^{[1
]}

Obuchi, Yoshiyuki ^{[1
]}

Okura, Yuki ^{[1
]}

Oguri, Masamune

Takata, Tadafumi ^{[1
]}

Tomono, Daigo ^{[1
]}

Kurakami, Tomio ^{[1
]}

Namikawa, Kazuto ^{[1
]}

Usuda, Tomonori ^{[1
]}

Yamanoi, Hitomi ^{[1
]}

Terai, Tsuyoshi ^{[1
]}

Uekiyo, Hatsue ^{[1
]}

Yamada, Yoshihiko ^{[1
]}

Koike, Michitaro ^{[1
]}

Aihara, Hiro

Fujimori, Yuki

Minco, Sogo

Miyatake, Hironao

Yasuda, Naoki

Nishizawa, Jun

Saito, Tomoki

Tanaka, Manobu

Uchida, Tomohisa

Katayama, Nobu

Wang, Shiang-Yu

Chen, Hsin-Yo

Lupton, Robert

Loomis, Craig

Bickerton, Steve

Price, Paul

Gunn, Jim

Suzuki, Hisanori

Miyazaki, Yasuhito

Muramatsu, Masaharu

Yamamoto, Koei

Endo, Makoto

机构：

[1] Natl Astron Observ Japan, Mitaka, Tokyo 1818858, Japan

来源：

GROUND-BASED AND AIRBORNE INSTRUMENTATION FOR ASTRONOMY IV | 2012年 / 8446卷

关键词：

Wide field; imaging; CCD; SQUARE DEGREE FIELD;

D O I：

10.1117/12.926844

中图分类号：

V [航空、航天];

学科分类号：

08 ; 0825 ;

摘要：

Hyper Suprime-Cam (HSC) is an 870 Mega pixel prime focus camera for the 8.2 m Subaru telescope. The wide field corrector delivers sharp image of 0.25 arc-sec FWHM in r-band over the entire 1.5 degree (in diameter) field of view. The collimation of the camera with respect to the optical axis of the primary mirror is realized by hexapod actuators whose mechanical accuracy is few microns. As a result, we expect to have seeing limited image most of the time. Expected median seeing is 0.67 arc-sec FWHM in i-band. The sensor is a p-ch fully depleted CCD of 200 micron thickness (2048 x 4096 15 mu m square pixel) and we employ 116 of them to pave the 50 cm focal plane. Minimum interval between exposures is roughly 30 seconds including reading out arrays, transferring data to the control computer and saving them to the hard drive. HSC uniquely features the combination of large primary mirror, wide field of view, sharp image and high sensitivity especially in red. This enables accurate shape measurement of faint galaxies which is critical for planned weak lensing survey to probe the nature of dark energy. The system is being assembled now and will see the first light in August 2012.

引用

页数：9

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