光傲——All For Light Puntino 天文望远镜调校系统

Puntino 天文望远镜调校系统

Puntino 简介

Puntino 是基于Shack-Hartmann 波前探测原理的紧密仪器，用于测试 single focal ratio telescope 或光学元件。经常使用它的部分客户有:

新墨西哥州 3.5m Apache Point 天文望远镜
美国Virginia大学 1m 的FAN 望远镜
Kavalur Observatory-2.3m VBT telescope ,
Indian Institute of Astrophysics-2m HIROT telescope
日本东京大学的 2m MAGNUM telescope
.......

Puntino 波前探测系统是一个非常紧凑的测试仪器(外形尺寸取决于focal ratio),可以用于天文望远镜作为离线测试和在线（主动光学元件）测试应用。也可以在实验室用于测试光学元件。

Puntino 波前探测系统有2个CCD探测器，一个用于获取SH图像，一个用于获取星像。第二个CCD还可以获得镜面或透镜的瞳像。这样可以获得更多的光学参数及成像质量信息。对于一个1.9米的镜面，将获得一下信息：

镜面抛光的残留物清晰可见
光孔不够圆（侧面的支撑调节不到位，过大）
亮点是由于镜面表面的气流影响
中间的洞是副镜的阴影
十字形是副镜的支撑架造成的阴影

Puntino 功能及特点

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

Wavelength range: 390 nm -1100 nm

产品主要特点

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

软件功能

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 主要技术指标

Feature /项目	Specification / 说明
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

应用说明

卡式 Cassegrain 焦点测试

测试配置说明： 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.


牛顿焦点 Newtonian focus 测试

测试配置说明 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 光学参数自动测量系统

光学精密测量装调

: Lentino 镜头在线测试优化系统

发送给朋友| 打印

All For Light---光傲科技股份有限公司
上海市徐汇区宜山路515号环线广场1号楼12层F座
Tel:+86-21-51029613 64827985 Fax:+86-21-64827995
Email:sales#light-all.com