Σ_SFR vs. Σ(H₂+H I). The galaxies associated with a “clumpy CO” distribution are reported in bold in Table A.2 and correspond to P_clumpy ≥ 0.4 (see Eq. (11)), while the others correspond to a “diffuse CO” distribution. Plain lines correspond to the best fits obtained for those two categories, with their 95% confidence intervals shown as shaded-areas, as well as the relations derived for starbursting galaxies and non-starbursting galaxies from Kennicutt & De Los Reyes (2021) and de los Reyes & Kennicutt (2019), respectively.