Abstract
Recently many modern instruments and systems have been developed to study the Sun. For that, spectral instruments with high spectral resolution are most often used. It is relevant to achieve high spatial resolution along with spectral one for many scientific tasks. In practice, the achievement of both high spectral and spatial resolution can be done by the use of integral field spectroscopy. Current paper is devoted to searching for a system solution for an integral field unit (IFU), which will be implemented to the optical system of solar telescopecoronagraph. The diameter of the main mirror is D = 3 m. Telescope’s working spectral range is ∆λ = 390 − 1600 nm. The integral field unit is based on reflective elements. It divides the input field of a rectangular shape with a size of 0.7500 ×1200(0.145 mm×2.327 mm) into 8 parts with a size of 0.09400×9600(0.018 mm×18.617 mm) each. The possibility of creating an IFU optical system using a parabolic mirror for all (eight) channels is shown. The quality of the optical system was evaluated, as well as the effect of vignetting on the slicing mirrors.
Highlights
The development and refinement of the characteristics of the KST-3 solar telescope-coronograph [1,2] with the diameter of the main mirror D = 3 m is being conducted
The task of achieving high spatial resolution can be solved by building a spectral block by using the integral field spectroscopy technique
Integral field spectroscopy is an area in astronomy that allows to collect information about the spectrum of a two-dimensional field with high spectral resolution and the spatial one
Summary
The spectrometer 6 forms spectral images 7 of a slit 5 in the spectral range of 0.39 − 1.60 μm Today, projects such as MuSICa [3,4,5], MUSE [6,7,8,9,10], FISICa [11,12], developed by the use of integral field spectroscopy, merely begin to be implemented. Projects such as MuSICa [3,4,5], MUSE [6,7,8,9,10], FISICa [11,12], developed by the use of integral field spectroscopy, merely begin to be implemented There are no such implemented systems for studying the Sun in a wide spectral range (0.39 − 1.60 μm)
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