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

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.

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Table 1. Parameters of the Cassegrain Telescope System
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Table 1. Parameters of the Cassegrain Telescope System
Surface Semidiameter (mm) Radius (mm) Thickness (mm) Conic
PM 880 $- 5400$ $- 2292$ $- 1$
SM 142.9 $- 938$ 1807 $- 1.688$

Table 2. Misalignment Errors of the Secondary Mirror
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Table 2. 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

Table 3. Residual Errors and Wavefront Residual Errors of Optical System Measured After Correction

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Table 3. 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

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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

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