| Project/Area Number |
07554001
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| Research Category |
Grant-in-Aid for Scientific Research (B)
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| Allocation Type | Single-year Grants |
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| Section | 試験 |
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| Research Field |
Astronomy
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| Research Institution | Nagoya University |
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Principal Investigator |
NAGATA Tetsuya Nagoya University, Department of physics, Assoc.Professor, 大学院・理学研究科, 助教授 (80208016)
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| Co-Investigator(Kenkyū-buntansha) |
YAMASHITA Takuya National Astronomical Pbservatory, Optical IR Research, Assoc.Professor, 光学赤外天文学研究系, 助教授 (00211631)
SATO Shuji Nagoya University, Department of physics, Professor, 大学院・理学研究科, 教授 (50025483)
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| Project Period (FY) |
1995 – 1996
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| Project Status |
Completed (Fiscal Year 1996)
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| Budget Amount *help |
¥7,500,000 (Direct Cost: ¥7,500,000)
Fiscal Year 1996: ¥1,700,000 (Direct Cost: ¥1,700,000)
Fiscal Year 1995: ¥5,800,000 (Direct Cost: ¥5,800,000)
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| Keywords | infrared detector / wide-field optics / metal mirror |
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| Research Abstract |
Elemnts required for the development of the cryogenic infrared camera were divided into three categories : cryogenics, optics, and electronics. Each development is nearly completed.
A cryostat with a large opening was designed and manufactured. Despite of large heat coming in from the window, the whole optics can be maintained below 80K and the detector unit below 30K,by using a closed cycle cooler. Indium seal and copper wires were employed to improve heat conduction and expel the heat from the cooler head efficiently. Cryogenic motors were made out of usual commmerical motors be changing bearings, and their tests have established their motion at the liquid nitrogen temperature.
Metal mirrors were manufactured and examined. First, several small test mirrors were made : offset parabolas, parabolas of 10 cm in diameter, and spherical mirrors of 15 cm in diameter. All of them turned out to have sufficient accuracy. A Ritchey-Chretien optics was adopted as the primary and secondary mirrors. The primary (25 cm in diameter) and secondary have been designed and manufactured. Two-pieceens for aberration correction was also manufactured.
Test electronics was completed and shows sufficiently low noise. MESSIA-III (National Astronomical Observatory of Japan) will be used as detector-independent part.
The above three elements will be integrated, and observation of the Galactic plane with it will be started this year.
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