Stellar velocity dispersion fitting with pPXF. Observed MUSE spectra are in black, and the red curves are the pPXF best-fit models. The residuals of the data with respect to the model are shown in green. The regions masked, to avoid the impact of emission lines or of the subtraction of sky, laser, or telluric lines, are shaded in grey. The data minus model residuals in these regions are marked in blue. In the top-left corner, we show a JWST red-green-blue cutout of the object, 4″ on each side, and show the apertures used for the spectral extraction from the weighted MUSE cube. Measured σ_v and S/N values are shown above the plot.