Telescope alignment based on the sharpness function of under-sampled images

Min Li; Xin Liu; Ang Zhang; Hao Xian

doi:doi:10.3788/COL201917.061101

Chinese Optics Letters, 2019, 17 (6): 061101, Published Online: Jun. 5, 2019

Telescope alignment based on the sharpness function of under-sampled images Download： 879次

Min Li ^1,2,3Xin Liu ²Ang Zhang ^1,2,*Hao Xian ^1,2,**

Author Affiliations

¹ Key Laboratory of Adaptive Optics, Chinese Academy of Sciences, Chengdu 610209, China

² Institute of Optics and Electronics, Chinese Academy of Sciences, Chengdu 610209, China

³ University of Chinese Academy of Sciences, Beijing 100049, China

Figures & Tables

Fig. 1. Cassegrain telescope system.

下载图片查看原文

Fig. 2. Process of telescope alignment.

下载图片查看原文

Fig. 3. Designed and misaligned images with different FWHMs. (a) Designed images. (b) Misaligned images.

下载图片查看原文

Fig. 4. Spectrum of the 0field designed image with FWHMs of 1, 2, 3, and 4 pixels.

下载图片查看原文

Fig. 5. Results of the telescope alignment. (a) Results of the on-axis correction. (b) Results of the all-fields correction.

下载图片查看原文

Fig. 6. Convergence curves of RMS during the correction. (a) RMS changes during the on-axis field correction. (b) RMS changes during the all-fields correction.

下载图片查看原文

Table1. Parameters of the Cassegrain Telescope System

Surface	Semidiameter (mm)	Radius (mm)	Thickness (mm)	Conic
PM	880	$- 5400$	$- 2292$	$- 1$
SM	142.9	$- 938$	1807	$- 1.688$

查看原文

Table2. Misalignment Errors of the Secondary Mirror

$D_{x}$ (μm)	$D_{y}$ (μm)	$D_{z}$ (μm)	$T_{x}$ (°)	$T_{y}$ (°)
600	880	80	0.1	0.03

查看原文

Table3. Residual Errors and Wavefront Residual Errors of Optical System Measured After Correction

FWHM(pixel)		1	2	3	4
Residual errors	$D_{x}$ (mm)	0.030	0.051	0.030	0.023
	$D_{y}$ (mm)	−0.276	−0.226	−0.133	−0.098
	$D z$ (mm)	0.008	0.008	0.008	0.008
	$T_{x}$ (°)	0.038	0.031	0.018	0.013
	$T_{y}$ (°)	0.004	0.007	0.004	0.003
RRE (%)		19.5	19.7	12.3	9.5
WRE ( $λ$ )		0.1074	0.1071	0.1014	0.0972

查看原文

Min Li, Xin Liu, Ang Zhang, Hao Xian. Telescope alignment based on the sharpness function of under-sampled images[J]. Chinese Optics Letters, 2019, 17(6): 061101.

Telescope alignment based on the sharpness function of under-sampled images Download： 879次

Fig. 1. Cassegrain telescope system.

Fig. 2. Process of telescope alignment.

Fig. 3. Designed and misaligned images with different FWHMs. (a) Designed images. (b) Misaligned images.

Fig. 4. Spectrum of the 0field designed image with FWHMs of 1, 2, 3, and 4 pixels.

Fig. 5. Results of the telescope alignment. (a) Results of the on-axis correction. (b) Results of the all-fields correction.

Fig. 6. Convergence curves of RMS during the correction. (a) RMS changes during the on-axis field correction. (b) RMS changes during the all-fields correction.

Table1. Parameters of the Cassegrain Telescope System

Table2. Misalignment Errors of the Secondary Mirror

Table3. Residual Errors and Wavefront Residual Errors of Optical System Measured After Correction

关于本站 Cookie 的使用提示

全站搜索

Telescope alignment based on the sharpness function of under-sampled images Download： 879次

Fig. 1. Cassegrain telescope system.

Fig. 2. Process of telescope alignment.

Fig. 3. Designed and misaligned images with different FWHMs. (a) Designed images. (b) Misaligned images.

Fig. 4. Spectrum of the 0field designed image with FWHMs of 1, 2, 3, and 4 pixels.

Fig. 5. Results of the telescope alignment. (a) Results of the on-axis correction. (b) Results of the all-fields correction.

Fig. 6. Convergence curves of RMS during the correction. (a) RMS changes during the on-axis field correction. (b) RMS changes during the all-fields correction.

Table1. Parameters of the Cassegrain Telescope System

Table2. Misalignment Errors of the Secondary Mirror

Table3. Residual Errors and Wavefront Residual Errors of Optical System Measured After Correction

相关论文

相关资讯

关于本站 Cookie 的使用提示

全站搜索