Stellar and gas E(B − V) for three example galaxies. The stellar E(B − V)_stars is determined from the Voronoi binned data cubes used for stellar population analysis, while the gas E(B − V)_gas is computed from the Balmer decrement, derived from the spaxel-level analysis of the ionised gas emission lines (only regions with S/N >  4 in the line emission are considered). The colour bars for the gaseous E(B − V) is stretched by a factor of two to account for the average ratio E(B − V)_stars ∼ 0.5 E(B − V)_gas. E(B − V)_stars traces similar structures as E(B − V)_gas, although jumps are evident when comparing the average level of some MUSE pointings to that of their neighbours (e.g., the bottom-right pointing in NGC 4535 and the three left-most pointings in NGC 4254).