Theoretical and experimental study on the testing accuracy of the image stabilization system of a space astronomical telescope

Chenghao Li; Chenghao Li; Xu He; Qi Ji; Xiaohui Zhang; Kuo Fan; Kuo Fan

doi:10.1364/AO.388891

Applied Optics
Vol. 59,
Issue 22,
pp. 6658-6670
(2020)
•https://doi.org/10.1364/AO.388891

Theoretical and experimental study on the testing accuracy of the image stabilization system of a space astronomical telescope

Chenghao Li, Xu He, Qi Ji, Xiaohui Zhang, and Kuo Fan

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Chenghao Li, Xu He, Qi Ji, Xiaohui Zhang, and Kuo Fan, "Theoretical and experimental study on the testing accuracy of the image stabilization system of a space astronomical telescope," Appl. Opt. 59, 6658-6670 (2020)

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Abstract

Space astronomical telescopes must test the image stabilization accuracy of their image stabilization system prior to entering the orbit. According to the position characteristics of the fine guidance sensor of telescopes required by the China National Space Administration, a simulation model of moving guide stars is proposed in this study to test the image stabilization accuracy of space telescopes. The simulation model for synchronous moving guide stars is based on the principle of mutual collimation of the diagonal field of view of the optical system of telescope. Realize the multi-field moving guide stars with high synchronization accuracy simulated by the same target source. Compared to traditional methods, this method requires simple manufacturing and has high flexibility. The error sources affecting the simulation accuracy of the moving guide stars are analyzed, and an error model is established. Analysis results show that the simulation accuracy of the moving guide stars can reach ${{0}.{046^{\prime\prime}}}$. The simulation model of guide stars is verified through experiments in which the influence of the vibration isolation platform is considered. Experiment results show that the simulation accuracy of motion guide stars is ${{0}.{036^{\prime\prime}}}$, satisfying the accuracy requirements (${\lt}{{0}.{08^{\prime\prime}}}$) of the accuracy test for the telescope image stabilization of telescopes.

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Model	$ε$	$ζ$
S-330.2SL	0.05 µrad	0.1%
S-330.4SL	0.25 µrad	0.2%
S-330.8SL	0.5 µrad	0.25%

Serial Number	Analysis of the Condition	Error ( $^{''}$ )
a	$L = 20 m m$ , $ε = 0.05 µ r a d$ , $ζ = 0.1 %$	$1.617 \times 1 0^{- 5}$
b	$L = 30 m m$ , $ε = 0.05 µ r a d$ , $ζ = 0.1 %$	$2.744 \times 1 0^{- 5}$
c	$L = 40 m m$ , $ε = 0.05 µ r a d$ , $ζ = 0.1 %$	$4.813 \times 1 0^{- 5}$
d	$L = 20 m m, ε = 0.25 µ r a d$ , $ζ = 0.2 %$	$3.722 \times 1 0^{- 4}$
e	$L = 30 m m, ε = 0.25 µ r a d$ , $ζ = 0.2 %$	$7.997 \times 1 0^{- 4}$
f	$L = 40 m m, ε = 0.25 µ r a d$ , $ζ = 0.2 %$	$1.215 \times 1 0^{- 3}$
g	$L = 20 m m$ , $ε = 0.5 µ r a d$ , $ζ = 0.25 %$	$1.485 \times 1 0^{- 3}$
h	$L = 30 m m$ , $ε = 0.5 µ r a d$ , $ζ = 0.25 %$	$2.813 \times 1 0^{- 3}$
i	$L = 40 m m$ , $ε = 0.5 µ r a d$ , $ζ = 0.25 %$	$4.957 \times 1 0^{- 3}$

Serial Number	Analysis of the Condition	Error ( $3 σ$ )
a	$L = 20 m m, ε < 0.05 µ r a d$ , $ζ < 0.1 %$	$< 5.746 \times 10^{- 5^{''}}$
b	$L = 20 m m$ , $ε < 0.25 µ r a d$ , $ζ < 0.2 %$	$< 1.426 \times 10^{- 4^{''}}$
c	$L = 20 m m, ε < 0.5 µ r a d$ , $ζ < 0.25 %$	$< 1.985 \times 10^{- 4^{''}}$
d	$L = 20 m m$ , $ε < 0.05 µ r a d$ , $ζ < 0.1 %$ , $Δ 1 < 0.5 %$ , $Δ 2 < 0.5 %$	$< 4.634 \times 10^{- 2^{''}}$
e	$L = 20 m m$ , $ε < 0.25 µ r a d$ , $ζ < 0.2 %$ , $Δ 1 < 0.5 %$ , $Δ 2 < 0.5 %$	$< 4.651 \times 10^{- 2^{''}}$
f	$L = 20 m m$ , $ε < 0.5 µ r a d$ , $ζ < 0.25 %$ , $Δ 1 < 0.5 %$ , $Δ 2 < 0.5 %$	$< 4.656 \times 10^{- 2^{''}}$
g	$L = 20 m m, ε < 0.05 µ r a d$ , $ζ < 0.1 %$ , $Δ 1 < 1 %$ , $Δ 2 < 1 %$	$< 9.253 \times 10^{- 2^{''}}$
h	$L = 20 m m$ , $ε < 0.25 µ r a d$ , $ζ < 0.2 %$ , $Δ 1 < 1 %$ , $Δ 2 < 1 %$	$< 9.269 \times 10^{- 2^{''}}$
i	$L = 20 m m$ , $ε < 0.5 µ r a d$ , $ζ < 0.25 %$ , $Δ 1 < 1 %$ , $Δ 2 < 1 %$	$< 9.475 \times 10^{- 2^{''}}$

Error Source	Error Types	Error Range
Fast-steering mirror electrical noise	Gaussian distribution	$- 0.05 µ r a d \sim 0.05 µ r a d$
Fast-steering mirror linear error	Uniform distribution	$- 0.1 % \sim 0.1 %$
Focal length difference of the field lens	Uniform distribution	$- 0.5 % \sim 0.5 %$
Focal length difference between M1 and M2	Uniform distribution	$- 0.5 % \sim 0.5 %$
Vibration isolation platform error	Gaussian distribution	${0.02}^{''}$

Serial Number	Residual of A (Abs)	Residual of B (Abs)
1	$0 . 012^{''}$	$0 . 036^{''}$
2	$0 . 019^{''}$	$0 . 042^{''}$
3	$0 . 011^{''}$	$0 . 034^{''}$
4	$0 . 015^{''}$	$0 . 039^{''}$
5	$0 . 018^{''}$	$0 . 041^{''}$
6	$0 . 009^{''}$	$0 . 032^{''}$
7	$0 . 017^{''}$	$0 . 040^{''}$
8	$0 . 014^{''}$	$0 . 037^{''}$
9	$0 . 012^{''}$	$0 . 029^{''}$
10	$0 . 020^{''}$	$0 . 044^{''}$
11	$0 . 013^{''}$	$0 . 036^{''}$
12	$0 . 014^{''}$	$0 . 024^{''}$
13	$0 . 016^{''}$	$0 . 041^{''}$
14	$0 . 017^{''}$	$0 . 028^{''}$
15	$0 . 019^{''}$	$0 . 041^{''}$
Average value	$0 . 015^{''}$	$0 . 036^{''}$

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Applied Optics