Top row: maximum energy provided by SNe in a dissipation timescale versus the turbulent component of the observed energy, both for the atomic gas (left) and the molecular gas (right). Left panel: the orange points and the blue triangles are respectively for the cases of CNM and of WNM with Σ_SFR from Leroy et al. (2008) and Bigiel et al. (2010), while the yellow diamonds and the light blue triangles show the corresponding cases with Σ_SFR from Muñoz-Mateos et al. (2009). Each point is for a single galaxy and for a single radius. Right panel: the light green crosses and the green stars are the same quantities for the molecular gas obtained with the two Σ_SFR. The red and the dark red lines show the relations built with the “global” efficiencies for the atomic gas ⟨η_atom⟩ and the molecular gas ⟨η_mol⟩ respectively (see text), with grey areas indicating the uncertainty. The solid grey lines show the same relation with efficiencies of 1, while the dotted lines are obtained, from top to bottom, with efficiencies of 0.1, 0.01, 0.001, and 0.0001. Bottom row: summary of the best efficiency for our sample of galaxies, in the case of the atomic (left) and molecular (right) gas. The symbols are the same as in the top row. The red and dark red horizontal lines are the median ⟨η_atom⟩ and ⟨η_mol⟩ (also indicated above each panel) with 1σ error (grey area). Overall, the results of this “global” analysis are consistent with those obtained with the “spatially-resolved” approach, showing that low-efficiency SN feedback can sustain the gas turbulence.