1994 Fiscal Year Final Research Report Summary
High resolution observation by means of tomographic adaptive optics
| Project/Area Number |
04405008
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| Research Category |
Grant-in-Aid for General Scientific Research (A)
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| Allocation Type | Single-year Grants |
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| Research Field |
広領域
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| Research Institution | National Astronomical Observatory |
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Principal Investigator |
IYE Masanori Natl.Astr.Obs., Large Telescope Division, Prof., 大型光学赤外線望遠鏡計画推進部, 教授 (30111446)
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| Co-Investigator(Kenkyū-buntansha) |
TANAKA Wataru Natl.Astr.Obs., Opt.Infrared Astr.Div., Assoc.Pro, 光学赤外線天文学研究系, 助教授 (20011570)
TAKAMI Hideki Natl.Astr.Obs., Instr.R&D Center, Res.Assis, 天文機器開発実験センター, 助手 (00270455)
NOGUCHI Takashi Natl.Astr.Obs., Opt.Infrared Astr.Div., Assoc.Pro, 光学赤外線天文学研究系, 助教授 (10124679)
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| Project Period (FY) |
1992 – 1994
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| Keywords | Adaptive Optics / Tomography / DOme Seeing / Servo Control / Wavefront Measurement |
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| Research Abstract |
Researches carried out in this project were to establish the adaptive optics systems of practical use in order to improve the spatial resolution of large telescopes.
(1) The wavefront tilt correcting system, the so-called image stabilizer, optimized for the Coude infrared spectrograph of Okayama 188cm telescope was assembled and calibrated for actual usage. In order to enhance the efficieny of this system, an adptive control system of the servo loop was designed, tested, and implemented.
(2) A joint experiment with the CFHT group to evaluate the internal dome seeing at the existing telescope enclosure is outlined and a special original instrument, named a dome-seeing monitor, was fabricated and calibrated.
(3) A deformable mirror, 50mm in diameter, 0.5mm in thickness, mounted on 37 piezo actuators was fabricated and calibrated.
(4) A new type parallel-read CCD with skipper architecture to reduce the read noise and ensure fast frame rate was designed and manufactured in collaboration with the JPL.An electronic system to evaluate the performance of this system is under construction.
(5) Control algorithm to calculate the drive signal from wavefront error was etablished.
(6) Simulation of curvature sensing to evaluate the vertical structure of the turbulent atmosphere was made.
(7) Practical problems of evaluating the 3D structure of turbulent air using tomographic methods were assecced and possible ways to solve these difficulties were studied.
These achievements are in line with the original research goals of the present project and opened a practical way to establish an adaptive optives system useful for astronomy.
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