Stellar mass-to-light ratio (M_*/L) maps in the i-band derived from stellar population models fit to the MUSE observations. The left and right panels show the effect of different IMF assumptions. Left: M_*, MW-IMF/L map derived from stellar population synthesis assuming a MW-like IMF (see Sect. 3.2). Right: M_{*, free-IMF}/L map derived using a varying IMF but not allowing for IMF slopes lower than 0.8 (see Sect. 3.3). Top and bottom: M_*/L_i map extracted from the MUSE observations shown within a zoom onto the centre of and across the full MUSE FoV, respectively. The M_*/L is significantly higher in the centre of FCC 47 – where the NSC is located – than in the rest of the galaxy. For comparison, the dynamical model with constant mass-to-light ratio M_*, const/L is best fitted with 1.82 M_⊙/L_⊙ (see Sect. 4). Radial profiles of these maps are shown in Fig. 4.