Optical design of sub-angular second spatially resolved solar extreme ultraviolet broadband imaging spectrometer

Huang Yi-Fan; Xing Yang-Guang; Shen Wen-Jie; Peng Ji-Long; Dai Shu-Wu; Wang Ying; Duan Zi-Wen; Yan Lei; Liu Yue; Li Lin

doi:10.7498/aps.73.20231481

Abstract

The slit imaging spectrometer is one of the important tools for solar extreme ultraviolet (EUV) spectral imaging detection. However, at present, there is no such instrument load in China. The research of solar physics and space weather in the field of EUV spectral diagnosis mainly depends on foreign instrument data, which seriously restricts the development of related disciplines. The spectral imaging instruments that have been launched internationally have only a spatial resolution of $2''$, and it is difficult to observe the core characteristics of the plasma related to the coronal heating mechanism predicted by the theoretical model. In order to better understand the coupling process between different layers of the sun’s atmosphere, solar physics research requires the observed data with wider spectral coverage. In light of this, we propose and design a sub-angular second spatially resolved solar extreme ultraviolet broadband imaging spectrometer operating in a band range of 62–80 nm and 92–110 nm. Compared with the existing instruments, the system can achieve high spatial resolution and spectral resolution, and wide spectral range coverage. Performance evaluation results indicate that the imaging spectrometer’s spatial resolutions in both bands are better than 0.4'', and their spectral resolutions are both better than 0.007 nm, with spectral imaging quality approaching the diffraction limit. The system designed in this work holds significant reference value for developing the first Chinese space-based solar EUV spectroscopic instrument in the future.

Keywords:

Authors and contacts

1.
School of Optics&Photonics, Beijing Institute of Technology, Beijing 100081, China
2.
Beijing Institute of Spacecraft Environment Engineering, Beijing 100094, China
3.
Beijing Institute of Spacecraft Systems Engineering, Beijing 100094, China
4.
Beijing Institute of Astronautical Systems Engineering, Beijing 100076, China

Corresponding author: Xing Yang-Guang, xyg@bit.edu.cn

Funds: Project supported by the National Natural Science Foundation of China (Grant Nos. 62205027, 42274208) and the Strategic Priority Research Program of the Chinese Academy of Sciences (Grant No. XDA15018300).

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References

[1]	杨孟飞, 代树武, 王颖, 朱成林, 杨尚斌, 张也驰 2022 中国空间科学技术 42 1 Google Scholar Yang M F, Dai S W, Wang Y, Zhu C L, Yang S B, Zhang Y C 2022 Chin. Space Sci. Technol. 42 1 Google Scholar
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[6]	Wilhelm K, Axford W I, Curdt W, Gabriel A H, Grewing M, Huber M C E, Jordan S D, Kuehne M, Lemaire P, Marsch E 1995 Sol. Phys. 162 189 Google Scholar
[7]	Harrison R A, Sawyer E C, Carter M K, et al. 1995 Sol. Phys. 162 233 Google Scholar
[8]	Kosugi T, Matsuzaki K, Sakao T, et al. 2007 Sol. Phys. 243 3 Google Scholar
[9]	Culhane J L, Harra L K, James A M, et al. 2007 Sol. Phys. 243 19 Google Scholar
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[12]	Anderson M, Appourchaux T, Auchère F, et al. 2020 Astron. Astrophys. 642 A14 Google Scholar
[13]	Marirrodriga C G, Pacros A, Strandmoe S, et al. 2021 Astron. Astrophys. 646 A121 Google Scholar
[14]	Li C, Fang C, Li Z, et al. 2022 Sci. China-Phys. Mech. Astron. 65 289602 Google Scholar
[15]	Gan W Q, Zhu C, Deng Y Y, et al. 2019 Res. Astron. Astrophys. 19 156 Google Scholar
[16]	Zhang P, Hu X Q, Lu Q F, Zhu A J, Lin M Y, Sun L, Chen L, Xu N 2022 Adv. Atmos. Sci. 39 1 Google Scholar
[17]	Chen B, Zhang X X, He L P, et al. 2022 Light-Sci. Appl. 11 329 Google Scholar
[18]	Bai X Y, Tian H, Deng Y Y, et al. 2023 Res. Astron. Astrophys. 23 065014 Google Scholar
[19]	Tian H 2017 Res. Astron. Astrophys. 17 3 Google Scholar
[20]	Poletto L, Thomas R J 2004 Appl. Opt. 43 2029 Google Scholar
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图 1 太阳大气温度随表面高度变化曲线. 图上标注了本文设计的系统工作波段覆盖的极紫外强辐射谱线^[19]

Figure 1. Curve of solar atmospheric temperature versus surface height. The EUV strong emission lines covered by our design are marked on the figure^[19].

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图 2 亚角秒空间分辨的太阳极紫外宽波段成像光谱仪工作原理图

Figure 2. Operation principal diagram of sub-angular second spatial resolved solar extreme ultraviolet broadband imaging spectrometer

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图 3 亚角秒空间分辨的太阳极紫外宽波段成像光谱仪的光线追迹模型

Figure 3. Ray-tracing model for sub-angular second spatial resolved solar extreme ultraviolet broadband imaging spectrometer.

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图 4 成像光谱仪系统的设计流程

Figure 4. Design flow process for imaging spectrometer system

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图 5 亚角秒空间分辨的太阳极紫外宽波段成像光谱仪光学布局图

Figure 5. Optical layout of sub-angular second spatial resolved solar extreme ultraviolet broadband imaging spectrometer.

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图 6 TVLS光栅　(a) 基底表面矢高图; (b) 刻线密度分布曲线图

Figure 6. TVLS grating: (a) The substrate surface sag map; (b) the curve of the ruling density distribution.

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图 7 光线追迹结果　(a), (b) 不同离轴视场下RMS点列图半径随波长的变化; (c), (d) 不同波长下RMS点列图半径随视场的变化

Figure 7. Ray tracing results: (a), (b) RMS spots radii versus wavelengths under different off-axis FOV; (c), (d) RMS spots radii versus FOV in the different wavelengths.

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图 8 光学系统在不同波长处的调制传递函数　(a) λ = 62 nm; (b) λ = 80 nm; (c) λ = 92 nm; (d) λ = 110 nm

Figure 8. MTFs of optical system under different wavelengths: (a) λ = 62 nm; (b) λ = 80 nm; (c) λ = 92 nm; (d) λ = 110 nm.

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图 9 系统像元空间分辨率评价　(a) 垂直狭缝方向的像元空间分辨率; (b) 62—80 nm波段平行狭缝方向的像元空间分辨率; (c) 92—110 nm波段平行狭缝方向的像元空间分辨率

Figure 9. System spatial plate scale evaluation: (a) Spatial plate scale perpendicular to the slit; (b) spatial plate scale parallel to the slit in 62–80 nm wavelengths; (c) spatial plate scale parallel to the slit in 92–110 nm wavelengths.

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图 10 系统光谱分辨率评价　(a) 62—80 nm波段的光谱分辨率; (b) 92—110 nm波段的光谱分辨率

Figure 10. System spectral resolution evaluation: (a) Spectral resolution in 62–80 nm wavelengths; (b) spectral resolution in 92–110 nm wavelengths.

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图 11 反射膜层、滤光片、TVLS光栅效率和探测器量子效率随波长的变化曲线　(a) 热压B₄C单层膜的反射率曲线; (b) 厚度为150 nm铝滤光片的透过率曲线; (c) 光栅效率; (d) 探测器量子效率

Figure 11. Curves of reflective film, filter, TVLS grating efficiency and detector quantum efficiency change with wavelength: (a) Reflectance curve of hot-pressed B₄C single-layer film; (b) transmission curve of Al filter with thickness of 150 nm; (c) grating efficiency; (d) detector quantum efficiency.

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图 12 系统有效面积随波长的变化曲线　(a) 本文设计的系统, 红色加粗的曲线为系统观测波段内的有效面积; (b) SPICE

Figure 12. Curves of system effective area change with wavelength: (a) Our design, red bold curves represent the effective area within the observed wavelength range of the system; (b) SPICE.

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图 13 光谱(Smile)畸变和空间(Keystone)畸变　(a) 不同波长的Smile畸变; (b) 62—80 nm波段不同视场的Keystone畸变; (c) 92—110 nm波段不同视场的Keystone畸变

Figure 13. Spectral (Smile) distortion and spatial (Keystone) distortion: (a) Smile distortion of different wavelengths; (b) Keystone distortion of different field of view in 62–80 nm wavelengths; (c) Keystone distortion of different field of view in 92–110 nm wavelengths.

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表 1 亚角秒空间分辨的太阳极紫外宽波段成像光谱仪技术指标

Table 1. Specifications of the sub-angular second spatial resolved solar extreme ultraviolet broadband imaging spectrometer.

Performance parameters	Design values
Satellite orbit	Dawn-dusk solar synchronous orbit
Entrance aperture/mm²	156 × 156
Slit FOV/('' )	4.8
Wavelength range/nm	62—80 & 92—110 & 46—55 (2nd order)
Spectral resolution/nm	≤ 0.007
Spatial plate scale/(('' )·pixel^–1)	≤ 0.5
Spatial resolution/('' )	≤ 1.0
System focal length/mm	11000
Optical volume/mm³	≤ 2800 × 500 × 450
Pixel size of detector/μm	15 (1536 × 1536)

DownLoad: CSV

表 2 亚角秒空间分辨的太阳极紫外宽波段成像光谱仪技术指标和元件参数

Table 2. Specifications and optical element parameters of sub-angular second spatial resolved solar extreme ultraviolet broadband imaging spectrometer.

Specification
Wavelength range@SW/nm	62—80
Wavelength range@LW/nm	92—110 & 46—55 (2nd order)
Spectral resolution@SW/nm	0.00615
Spectral resolution@LW/nm	0.00642
Spatial plate scale @SW/(('' )·pixel^–1)	0.340(@71 nm)
Spatial plate scale @LW/(('' )·pixel^–1)	0.382(@101 nm)
System focal length/mm	11000
Optical volume/mm³	2600 × 420 × 400
Detector/μm	15 (1536 × 1536)
Telescope design
Aperture/mm²	156 × 156
R_T/mm	4320.025
Conic	–1
$\varDelta $/mm	120
Slit design
Slits width/('' )	0.28, 1, 2, 40
Slits length/('' )	288
Raster coverage/('' )	±144
TVLS grating design
m	+1 order
1/d₀/mm^–1	1500
β	5.177×@SW; 5.261×@LW
i/(°)	0.909
r_A/mm	440.667
R/mm	735.545
ρ/mm	737.138
b₂	0.0349
Groove density/(lines·mm^–1)	1500 ± 4
Ruling area/mm²	36 × 36
Two independent detectors design
Wavelength range/nm	Tilt angle/(°)
62—80	15.259
92—110	17.824

DownLoad: CSV

表 3 系统关键元件的公差容限

Table 3. Tolerance limits of key components of the system.

Component	Tolerance items	Values of tolerances
Primary mirror	Surface irregularity (RMS)	λ/20 (λ = 632.8 nm)
	Conic	±0.005
	Radius of curvature/mm	±3.6
	Microroughness (RMS)/nm	0.4
	Element decenter/μm	±50
	Element tilt/('' )	±15
TVLS grating	Substrate irregularity (RMS)	λ/30 (λ = 632.8 nm)
	Line density/ (groove·mm^–1)	±0.65
	Radius of curvature/mm	±0.3
	Microroughness (RMS)/nm	0.8
	Element decenter/μm	±20
	Element tilt/('' )	±60
Slit assembly	Element decenter/μm	±20
Slit assembly	Element tilt/(°)	±0.03

DownLoad: CSV

[1]	杨孟飞, 代树武, 王颖, 朱成林, 杨尚斌, 张也驰 2022 中国空间科学技术 42 1 Google Scholar Yang M F, Dai S W, Wang Y, Zhu C L, Yang S B, Zhang Y C 2022 Chin. Space Sci. Technol. 42 1 Google Scholar
[2]	颜毅华, 邓元勇, 甘为群, 丁明德, 田晖, 朱小帅 2023 空间科学学报 43 199 Google Scholar Yan Y H, Deng Y Y, Gan W Q, Ding M D, Tian H, Zhu X S 2023 Chin. J. Space Sci. 43 199 Google Scholar
[3]	陈鹏飞 2021 中国科学: 物理学力学天文学 51 119632 Google Scholar Chen P F 2021 Sci. Sin. -Phys. Mech. Astron. 51 119632 Google Scholar
[4]	白先勇, 田晖, 邓元勇, 陈亚杰, 侯振永, 杨子浩, 张志勇, 段帷, 李文显, 郭思璠 2023 空间科学学报 43 406 Google Scholar Bai X Y, Tian H, Deng Y Y, Chen Y J, Hou Z Y, Yang Z H, Zhang Z Y, Duan W, Li W X, Guo S F 2023 Chin. J. Space Sci. 43 406 Google Scholar
[5]	Domingo V, Fleck B, Poland A I 1995 Sol. Phys. 162 1 Google Scholar
[6]	Wilhelm K, Axford W I, Curdt W, Gabriel A H, Grewing M, Huber M C E, Jordan S D, Kuehne M, Lemaire P, Marsch E 1995 Sol. Phys. 162 189 Google Scholar
[7]	Harrison R A, Sawyer E C, Carter M K, et al. 1995 Sol. Phys. 162 233 Google Scholar
[8]	Kosugi T, Matsuzaki K, Sakao T, et al. 2007 Sol. Phys. 243 3 Google Scholar
[9]	Culhane J L, Harra L K, James A M, et al. 2007 Sol. Phys. 243 19 Google Scholar
[10]	Brosius J W, Daw A N, Rabin D M 2014 Astrophys. J. 790 1 Google Scholar
[11]	Müller D, St Cyr O C, Zouganelis I, et al. 2020 Astron. Astrophys. 642 A1 Google Scholar
[12]	Anderson M, Appourchaux T, Auchère F, et al. 2020 Astron. Astrophys. 642 A14 Google Scholar
[13]	Marirrodriga C G, Pacros A, Strandmoe S, et al. 2021 Astron. Astrophys. 646 A121 Google Scholar
[14]	Li C, Fang C, Li Z, et al. 2022 Sci. China-Phys. Mech. Astron. 65 289602 Google Scholar
[15]	Gan W Q, Zhu C, Deng Y Y, et al. 2019 Res. Astron. Astrophys. 19 156 Google Scholar
[16]	Zhang P, Hu X Q, Lu Q F, Zhu A J, Lin M Y, Sun L, Chen L, Xu N 2022 Adv. Atmos. Sci. 39 1 Google Scholar
[17]	Chen B, Zhang X X, He L P, et al. 2022 Light-Sci. Appl. 11 329 Google Scholar
[18]	Bai X Y, Tian H, Deng Y Y, et al. 2023 Res. Astron. Astrophys. 23 065014 Google Scholar
[19]	Tian H 2017 Res. Astron. Astrophys. 17 3 Google Scholar
[20]	Poletto L, Thomas R J 2004 Appl. Opt. 43 2029 Google Scholar
[21]	Poletto L, Gasparotto A, Tondello G, Thomas R J 2004 UV and Gamma-Ray Space Telescope Systems Glasgow, United Kingdom, June 21–25, 2004 p898
[22]	Larruquert J I, Keski-Kuha R A M 2000 Appl. Opt. 39 1537 Google Scholar
[23]	王丽辉, 何玲平, 王孝坤, 尼启良, 陈波 2008 光学精密工程 16 42 Google Scholar Wang L H, He L P, Wang X K, Ni Q L, Chen B 2008 Opt. Precis. Eng. 16 42 Google Scholar
[24]	汪毓明, 季海生, 王亚敏, 等 2020 中国科学: 技术科学 50 1243 Google Scholar Wang Y M, Ji H S, Wang Y M, et al. 2020 Sci. Sin. Technol. 50 1243 Google Scholar
[25]	林隽, 黄善杰, 李燕, 等 2021 空间科学学报 41 183 Google Scholar Liu J, Huang S J, Li Y, et al. 2021 Chin. J. Space Sci. 41 183 Google Scholar
[26]	季海生, 汪毓明, 汪景琇 2019 中国科学: 物理学力学天文学 49 059605 Google Scholar Ji H S, Wang Y M, Wang J X 2019 Sci. Sin. Phys. Mech. Astron. 49 059605 Google Scholar
[27]	杨孟飞, 汪景琇, 王赤, 等 2023 科学通报 68 859 Google Scholar Yang M F, Wang J X, Wang C, et al. 2023 Chin. Sci. Bull. 68 859 Google Scholar
[28]	邓元勇, 周桂萍, 代树武, 等 2023 科学通报 68 298 Google Scholar Deng Y Y, Zhou G P, Dai S W, et al. 2023 Chin. Sci. Bull. 68 298 Google Scholar

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