The ideal optical system can realize point-to-point imaging, but for an actual observation it is difficult to achieve this ideal phenomenon due to the instrumental effects of imaging system, which is usually described as the instrument profile in the imaging process of a grating spectrometer. The existence of the spectrometer instrument profiles introduces systematic errors in the observed spectral lines, which make the spectrum of the studied objects degenerate and blur. In this paper, we take the spectral data in the H α $\mbox{H}\upalpha $ band observed by the Multi-Band Spectrometer (MBS) of the New Vacuum Solar Telescope (NVST) as an example; according to the characteristics of its acquired spectral data, we calculate the instrument profiles of the MBS in the spatial and the dispersion direction. The results are, respectively, 0.25 ″ $0.25''$ and 115 mÅ, which might reflect the influence of the MBS optical instruments at that time in the H α $\mbox{H}\upalpha $ band. Then the spectral data is deconvolved separately in the two directions by the corresponding IP to obtain the higher spatial and spectral resolution of the NVST spectral data.

中文翻译：

---

新型真空太阳望远镜光谱数据的仪器剖面测量与校正

理想的光学系统可以实现点对点的成像，但由于成像系统的仪器效应，在实际观察中很难实现这种理想现象，通常将其描述为光栅成像过程中的仪器轮廓。光谱仪。光谱仪仪器剖面的存在会在观察到的谱线中引入系统误差，使被研究物体的光谱退化和模糊。在本文中，我们以新型真空太阳望远镜（NVST）的多波段光谱仪（MBS）所观测到的Hα$\mbox{H}\upalpha$波段的光谱数据为例；根据其获取的光谱数据的特征，我们计算出MBS在空间和色散方向上的仪器剖面。结果分别为 0.25 英寸 0 美元。25''$ 和 115 mÅ，这可能反映了当时 MBS 光学仪器在 H α $\mbox{H}\upalpha $ 波段的影响。然后光谱数据通过相应的IP在两个方向上分别进行去卷积，以获得NVST光谱数据更高的空间和光谱分辨率。