Dust temperature image of the W43-MM2&MM3 protocluster cloud, taken from Pouteau et al. (2022). It combines a 2.5″ resolution dust temperature image computed from a Bayesian spectral energy distribution fit for fluxes ranging from 70 µm to 3 mm (see Dell’Ova et al. in prep.) with the central heating and self-shielding of protostellar and pre-stellar cores, respectively, at 0.46″ resolution (see Sect. 4.2 of Pouteau et al. 2022, for more details). White, orange, and red contours correspond to the levels defined in Figs. 1b–c. Black polygons indicate the subregions defined in Section 2.2, and the ellipse in the bottom-left corner corresponds to the 1.3 mm beam.