AbstractHigh resolution, multi-wavelength maps of a sizeable set of nearby galaxies have made it possible to study how the surface densities of H i, H₂ and star formation rate (Σ_HI, Σ_H2, Σ_SFR) relate on scales of a few hundred parsecs. At these scales, individual galaxy disks are comfortably resolved, making it possible to assess gas-SFR relations with respect to environment within galaxies. Σ_H2, traced by CO intensity, shows a strong correlation with Σ_SFR and the ratio between these two quantities, the molecular gas depletion time, appears to be constant at about 2 Gyr in large spiral galaxies. Within the star-forming disks of galaxies, Σ_SFR shows almost no correlation with Σ_HI. In the outer parts of galaxies, however, Σ_SFR does scale with Σ_HI, though with large scatter. Combining data from these different environments yields a distribution with multiple regimes in Σ_gas – Σ_SFR space. If the underlying assumptions to convert observables to physical quantities are matched, even combined datasets based on different SFR tracers, methodologies and spatial scales occupy a well define locus in Σ_gas – Σ_SFR space.