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Description
Metis was designed to capture images of the Solar Corona in visible (VL, 580-640 nm) and ultraviolet (UV, Ly-alpha, 121.6 nm) wavelengths. This work focuses on a preliminary characterization of the instrument's optical performance in the UV channel through Point Spread Function (PSF) analysis.
Our approach involves the study of stellar sources detected in the Metis UV Field of View (FOV). Through comparison with theoretical predictions from Zemax optical models, we evaluate the actual in-flight PSF profile and investigate potential deviations from expected behavior. This analysis allows us to establish a first assessment of the UV channel's optical quality and its response variations across the detector plane.
The preliminary findings contribute to understanding the operational characteristics of the Metis UV coronagraph in the space environment, offering initial validation of the instrument's imaging capabilities at Ly-alpha wavelengths and laying groundwork for future detailed performance studies.
