光傲——All For Light Puntino 天文望遠鏡調校系統

Puntino 天文望遠鏡調校系統

Puntino 簡介

Puntino 是基于Shack-Hartmann 波前探測原理的緊密儀器，用于測試 single focal ratio telescope 或光學元件。經常使用它的部分客戶有:

新墨西哥州 3.5m Apache Point?天文望遠鏡
美國Virginia大學?1m 的FAN?望遠鏡
Kavalur Observatory-2.3m VBT telescope ,
Indian Institute of Astrophysics-2m HIROT telescope
日本東京大學的 2m MAGNUM telescope
.......

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。

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：

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

Puntino 功能及特點

Puntino-Pro wavefront sensor in the laboratory and mounted at the telescope.

Wavelength range: 390 nm -1100 nm

產品主要特點

For testing astronomical telescopes
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
Wavefront analysis is done using a cooled camera for long integration times (to integrate out seeing effects)
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.
Standard sampling: 26 x 26 spots
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

Puntino 主要技術指標

Feature /項目	Specification / 說明
Type of element that can be measured	Astronomical telescopes (at Cassegrain, Prime and Newtonian focus). Telescopes in the laboratory. Lenses in external illumination
Focal ratios covered	f/1.8 to f/300 standard. Faster focal ratios can be tested with special setup
Diameter of optical element that can be tested	Practically any diameter
Diameter of lenslets	0.3 mm
Focal length of lenslets	41 mm
Standard sampling on the pupil	About 26 x 26 spots
Maximum sampling	Up to 70 x 70 spots can be used (camera dependent)
Analysis Software	Sensoft
Precision of Zernike polynomials coefficients (laboratory)	λ/300
Precision of Zernike polynomials coefficients (telescope)	0.01 "
Precision with which the wavefront is computed	λ/150 rms
Wavelength range	With standard camera from 0.375 μ up to 1.1 μ. With IR camera up to 2 μ
Reference source	LED with cooled camera. Remotely controlled
Distance from flange to instrument focus	54.8 mm
Height of optical axis from base	61.5 mm
Camera for SH	16-bit cooled CCD
Camera for finder	10-bit uncooled CMOS, 1280 x 1024 pixels, 7.5 μ pixel size or 14 or 16-bit cooled CCD
Dimensions (depends from focal ratios tested)	9 (Height) x 22 (Length) x 9 (Width) cm
Power requirement (stepper motor)	12V, 500 mA

應用說明

卡式 Cassegrain 焦點測試
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?測試配置說明： A telescope tested at the Cassegrain focus using external parallel light. The aberrations of the SH system itself are removed by taking a calibration frame, with a calibration source placed at the focus of Puntino. The incident light illuminating the system should be aberration free. In the case of an astronomical telescope, a natural star is used. It is not necessary to use parallel light for the test. The measured aberrations will then no longer refer to those for parallel light, but to one particular optical configuration that is used for the test.
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?牛頓焦點 Newtonian focus?測試
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測試配置說明 A telescope tested at the Newtonian focus using parallel light. The aberrations of the SH system itself are removed by taking a calibration frame, with a calibration source placed at the focus of Puntino. The incident light illuminating the system should be aberration free. In the case of an astronomical telescope, a natural star is used. It is not necessary to use parallel light for the test. The measured aberrations will then no longer refer to those for parallel light, but to one particular optical configuration that is used for the test.

: Opal 光學參數自動測量系統

產品一覽

: Lentino 鏡頭在線測試優化系統

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