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Puntino 天文望遠鏡調校測試系統
 
唯一可以直接用于天文望遠鏡現場裝調測試的波前探測器，自帶內置校正光源！
Puntino 波前探測系統是一個非常緊湊的測試儀器(外形尺寸取決于focal ratio),可以用于天文望遠鏡作為離線測試和在線（主動光學元件）測試應用。也可以在實驗室用于測試光學元件。
到今天為止， Puntino 作為大型天文望遠鏡觀測站日常調校的工具，已經用在全球幾乎所有的天文觀測站臺！
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產品結構
Puntino 波前探測系統有2個CCD探測器，一個用于獲取SH圖像，一個用于獲取星像。第二個CCD還可以獲得鏡面或透鏡的瞳像。這樣可以獲得更多的光學參數及成像質量信息。對于一個1.9米的鏡面，將獲得一下信息：
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- 鏡面拋光的殘留物清晰可見
- 光孔不夠圓（側面的支撐調節不到位，過大）
- 亮點是由于鏡面表面的氣流影響
- 中間的洞是副鏡的陰影
- 十字形是副鏡的支撐架造成的陰影
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功能描述
- For testing astronomical telescopes
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Wavefront sensor with in-built motorized light source for getting the reference calibration image in remote mode (to compensate for temperature changes and that flexure caused by the change of telescope position
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Wavefront analysis is done using a cooled camera for long integration times (to integrate out seeing effects)
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Second uncooled camera is used for analysis of the out-of-focus pupil of the telescope, giving additional information like alignment of the spiders of the primary and secondary mirrors, zones on the mirror surface, support problems etc.
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Standard sampling: 26 x 26 spots
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Focal ratios from f/1.8 up to f/300
軟件功能
- Measure the aberrations ( up to 70 terms of the Zernike polynomials)
- Estimate optical quality and Strehl ratio
- Inspect the wavefront corresponding to any aberration
- Focus your telescope. The program gives the magnitude (in mm) and the direction for effecting the correction
- Align your telescope in minutes instead of hours. Use the indications given by the software (magnitude and direction) to move the secondary mirror for effecting the alignment. It takes the guesswork out of alignment
- Find out the correct focal plane using the spherical aberration measured by PuntinoPro. The program again gives you the magnitude and direction in which to move the secondary mirror or the focal plane
- Helps identifying support errors at the zenith by shown by the wavefront map after mathematically subtracting the lower order aberration
- Optimize dome and mirror seeing by inspecting the plots of the residuals
- On-line display of how the aberrations change during the night
- Based on the Shack-Hartmann data, the MTF of the telescope can be computed
- Build/refine a sophisticated pointing model for the telescope using the indications given by PuntinoPro of the shift of image in the focal plane of the telescope for different positions in the sky
- PuntinoPro comes with detailed on-line help and a hardware and software user's manual containing both theory and practical examples to guide you in getting the correct interpretation out of the Shack-Hartmann analysis
- Measurement of combined external seeing, dome and mirror seeing using the second CCD camera
產品資料下載
 SpotOptics_Puntino.pdf
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| 技術參數 |
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Feature /項目
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Specification / 說明
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Type of element that can be measured
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Astronomical telescopes (at Cassegrain, Prime and Newtonian focus). Telescopes in the laboratory. Lenses in external illumination
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Focal ratios covered
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f/1.8 to f/300 standard. Faster focal ratios can be tested with special setup
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Diameter of optical element that can be tested
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Practically any diameter
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Diameter of lenslets
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0.3 mm
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Focal length of lenslets
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41 mm
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Standard sampling on the pupil
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About 26 x 26 spots
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Maximum sampling
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Up to 70 x 70 spots can be used (camera dependent)
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Analysis Software
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Sensoft
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Precision of Zernike polynomials coefficients (laboratory)
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λ/300
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Precision of Zernike polynomials coefficients (telescope)
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0.01 "
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Precision with which the wavefront is computed
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λ/150 rms
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Wavelength range
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With standard camera from 0.375 μ up to 1.1 μ. With IR camera up to 2 μ
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Reference source
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LED with cooled camera. Remotely controlled
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Distance from flange to instrument focus
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54.8 mm
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Height of optical axis from base
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61.5 mm
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Camera for SH
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16-bit cooled CCD
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Camera for finder
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10-bit uncooled CMOS, 1280 x 1024 pixels, 7.5 μ pixel size or 14 or 16-bit cooled CCD
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Dimensions (depends from focal ratios tested)
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9 (Height) x 22 (Length) x 9 (Width) cm
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Power requirement (stepper motor)
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12V, 500 mA
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產品資料下載
SpotOptics_Puntino.pdf
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| 參考用戶 |
- 云南天文臺麗江觀測站
- 上海天文臺
- 南京天文臺
- 成都光電研究院
- 3.5m TNG primary mirror at Zeiss Oberkochen (Germany)
- 1.82m Asiago Cima Ekar (Italy)
- 1.5m Loiano Loiano (Italy)
- 1.2m Crete Crete (Greece)
- 2.5m Nordic Optical Telescope (NOT) La Palma, Canary Islands
- 1.5m Sanchez Tenerife, Canary Islands
- 1.5m TT1 of the Observatory of Napoli Potenza (Italy)
- 1.2m Yerkes Observatory Williams Bay, USA
- 0.75m Yerkes Observatory Williams Bay, USA
- 1m San Diego San Diego (USA)
- 3.5m Apache Point Observatory New Mexico, USA
- 1m Apache Point Observatory New Mexico, USA
- 1.8m Kottamia Kottamia, Egypt
- 1m University of Virginia Charlotteville (USA)
- 2.5m VBT Bangalore (India)
- 1m Zeiss Bangalore (India)
- 2m HIROT at EOST Tucson, (USA)
- 2m HIROT Hanle, Himalayas (India)
- 2m MAGNUM* Maui,Hawaii (USA)
- 3.5m Calar Alto Almeria (Spain)
- 2.3m Aristarchos telescope Athens, (Greece)
- 1m Catania Telescope* Catania (Italy)
- Multi Mirror Telescope (MMT)* Tucson, (USA)
- Mount Abu 1.2m IR telescope* Mount Abu, Rajasthan (India)
- 4m Vista Telescope* La Silla (Chile) 26. Las Cumbres Telescope * USA 27. Telescope Technology Ltd* UK 28. 1.8m Kottamia Telescope* NRIAG, Egypt
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產品
