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Puntino天文望遠(yuǎn)鏡調(diào)校系統(tǒng)

直接聯(lián)系

光傲科技股份有限公司

美國(guó)

產(chǎn)品規(guī)格型號(hào)

參考報(bào)價(jià)：

面議

關(guān)注度：

600

產(chǎn)品介紹

Puntino 簡(jiǎn)介

Puntino 是基于Shack-Hartmann 波前探測(cè)原理的緊密儀器，用于測(cè)試 single focal ratio telescope 或光學(xué)元件。經(jīng)常使用它的部分客戶有:

新墨西哥州 3.5m Apache Point 天文望遠(yuǎn)鏡

美國(guó)Virginia大學(xué) 1m 的FAN 望遠(yuǎn)鏡

Kavalur Observatory-2.3m VBT telescope ，

Indian Institute of Astrophysics-2m HIROT telescope

日本東京大學(xué)的 2m MAGNUM telescope

.......

Puntino 波前探測(cè)系統(tǒng)是一個(gè)非常緊湊的測(cè)試儀器(外形尺寸取決于focal ratio)，可以用于天文望遠(yuǎn)鏡作為離線測(cè)試和在線（主動(dòng)光學(xué)元件）測(cè)試應(yīng)用。也可以在實(shí)驗(yàn)室用于測(cè)試光學(xué)元件。

Puntino 波前探測(cè)系統(tǒng)有2個(gè)CCD探測(cè)器，一個(gè)用于獲取SH圖像，一個(gè)用于獲取星像。第二個(gè)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(xué)參數(shù)及成像質(zhì)量信息。對(duì)于一個(gè)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(jiàn)

光孔不夠圓（側(cè)面的支撐調(diào)節(jié)不到位，過(guò)大）

亮點(diǎn)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(diǎn)

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

Wavelength range: 390 nm -1100 nm

產(chǎn)品主要特點(diǎn)

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(shù)指標(biāo)

Feature /項(xiàng)目	Specification / 說(shuō)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

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