Panel a) MUSE reconstructed V-band image of NGC 3115 obtained through the MUSE pipeline. Panel b) photometric V-band model of NGC 3115 from Emsellem et al. (1999). The model flux is scaled to the MUSE V-band image, which is in arbitrary units. Panel c) normalised residuals of the MUSE reconstructed V-band image obtained by subtracting the Emsellem et al. (1999)  model. The overall flatness of the residuals shows the good quality of our data reduction process (see Sect. 2.2). The significant residual structures (inner-disc, spirals, etc.) are discussed in Sect. 5.1.