中国科学院云南天文台机构知识库

杂散光由于光学表面散射和地球大气散射引起，降低了光谱图像的空间分辨率。光学系统都存在杂散光，要获得高分辨的光谱图像需要对杂散光进行抑制。多波段光谱仪的杂散光分为两类：（1）光谱桶内由于光机结构引起的杂射光；（2）混在成像光路中并参与色散的杂散光。第1种杂散光可直接测量，约占光谱能量的3％左右。第2种杂散光由于受多种因素影响，所以很难精确测量。从日食光谱测量中测得在观测目标周围对目标产生的杂散光的下限约为10％，并对空间方向的点扩散函数进行测量，为光谱的高分辨重建提供参考。

Stray-light is caused by the scattering of optical surfaces and the Earth's atmosphere; which degrades the spatial resolution of spectral images. Almost every optical system is affected by stray-light. To obtain high-resolution spectral images, we need to eliminate the effect caused by stray-light as much as possible. The stray-light of muhi-waveband spectrometer can be divided into two categories: (1)stray-light caused by the scattering of the optical and mechanical structures in the spectral barrel and (2)stray-light mixed in the imaging optical path and participating in dispersion. The first category can be measured directly, and it accounts for 3% of spectral energy. It is difficult to measure the second category precisely because it could be affected by many factors. We measured the stray-light around the target from the eclipse spectral observation, and found that the lower limit of the stray-light was about 10%. In addition, we measured the point spread function (PSF) of the multi-band spectrometer in the space direction. This work would provide reference for future high-resolution spectrum reconstruction.