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1.中国科学院 国家天文台,北京 100101
2.中国科学院大学 天文与空间科学学院,北京 100049
3.中国科学院 国家天文台 天文光学重点实验室,北京 100101
4.中国科学院 国家天文台 太阳活动重点实验室,北京 100101
[ "魏烨艳(1990-),女,江西赣州人,博士研究生,2016年于中国科学院大学获得硕士学位,主要从事天文红外光谱仪的研究。E-mail: yywei@bao.ac.cn魏烨艳(1990-),女,江西赣州人,博士研究生,2016年于中国科学院大学获得硕士学位,主要从事天文红外光谱仪的研究。E-mail: yywei@bao.ac.cn" ]
[ "冯志伟(1968-),男,吉林长春人,博士,高级工程师,2008年于中国科学院研究生院获得博士学位,主要从事天文探测技术与方法的研究。E-mail: zhwf@bao.ac.cn" ]
收稿日期:2021-01-20,
修回日期:2021-03-03,
纸质出版日期:2021-09-15
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魏烨艳,白先勇,张志勇等.太阳CO 4.66 μm光栅光谱仪的光学设计[J].光学精密工程,2021,29(09):2009-2018.
WEI Ye-yan,BAI Xian-yong,ZHANG Zhi-yong,et al.Optical design of grating spectrograph for solar CO 4.66 μm spectrum observation[J].Optics and Precision Engineering,2021,29(09):2009-2018.
魏烨艳,白先勇,张志勇等.太阳CO 4.66 μm光栅光谱仪的光学设计[J].光学精密工程,2021,29(09):2009-2018. DOI: 10.37188/OPE.20212909.2009.
WEI Ye-yan,BAI Xian-yong,ZHANG Zhi-yong,et al.Optical design of grating spectrograph for solar CO 4.66 μm spectrum observation[J].Optics and Precision Engineering,2021,29(09):2009-2018. DOI: 10.37188/OPE.20212909.2009.
为了实现对太阳中红外光谱CO 4.66 μm波段的观测,设计了一台光谱中心波长为4.667 μm的高分辨中红外光谱仪。基于科学观测需求分析了光谱仪的技术指标,为降低红外仪器的背景辐射,光谱仪整体置于真空制冷环境中;为达到高分辨率的观测需求,采用中阶梯光栅作为分光器件;为获得更优的像质,同时达到压缩光路的目的,光谱仪采用李特洛结构与离轴三反消像散技术相结合的光学设计,离轴三反同时承担了光谱仪中准直和成像的功能。在同轴三反系统的几何光学成像理论的基础上,研究了同轴三反结构、离轴三反结构以及光谱仪结构的求解和设计优化方法。光谱仪的焦距为1 300 mm,数值孔径为0.035,视场为20.3'×0.158',系统的整体尺寸小于700 mm。结果表明,在工作波段范围内,光谱仪点列图的均方根直径小于5 μm,能量集中于一个像元尺寸范围内,光谱仪系统设计结果满足要求。
To meet the requirements of the solar mid-infrared spectral band CO 4.66-μm spectrum observations, a high-resolution mid-infrared spectrograph with a 4.667-μm central wavelength was designed. First, the technical indicators were studied based on the requirements of the scientific observations that have to be made. The entire spectrograph was put in a vacuum liquid-nitrogen refrigeration vessel to reduce the background radiation from the infrared equipment. An echelle is used in the spectrograph as a spectrum splitter to increase the observation resolution. The optical configuration of the spectrograph uses a creative structure by combining the Littrow structure and the Three-Mirror Anastigmatic (TMA) technology. Such a structure provides better imaging quality and optical path compression. In addition, the TMA structure has dual functions, as the collimating and imaging optical paths. The design and optimization methods of the coaxial three-mirror structure, TMA structure, and spectrograph structure were also studied based on the coaxial three-mirror system's geometrical optical imaging theory. The designed spectrograph has a size of less than 700 mm, a focal length of 1 300 mm, a numerical aperture of 0.035, and a field of view of 20.3'×0.158'. The imaging quality of the spectrograph system was evaluated, with results indicating that, within the working wavelength, the root-mean-square diameter of the spot diagram is less than 5 μm, and the energy focuses on one pixel. Therefore, the spectrograph meets the design requirements.
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