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Fig. A.1.


Five arcseconds circle cutout of the white-light image of the bright star used as PSF in this work. Left: white-light image without post-processing. A faint source on the right part of the star’s PSF is clearly evident. Right: white-light image after replacing the faint source values with the symmetric portion of the MUSE dataset. After this correction, the PSF is well behaved at any wavelength out to five arcseconds (Fig. A.2 and Appendix A for details).

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