Star formation rate across the molecular gas spiral. The left panel shows the BPT diagnostic diagram for the combined MUSE WFM+NFM emission line maps, binned to 100 pc resolution. Ionised gas in NGC 4593’s innermost 1.3 kpc form a mixing sequence, with the star-forming fraction f_SF modelled using Rainbow. The right panel shows the resulting star formation rate surface density (Σ_SFR), overlaid with molecular gas spiral contours. Although the spatial distribution of Σ_SFR roughly aligns with the molecular gas, the peaks of the two structures are offset by up to ∼200 pc.