FUV based estimates of the star formation rate densities Σ_SFR and H I gas mass surface densities Σ_HI (left panel) shown with red triangles for the 6 H I peaks in the Leo ring with non-negligible FUV emission. The open triangles indicate H I peak data not listed by Schneider et al. (1986) relative to cloudlets towards M 96. Filled dots trace the relation for the median values of the large database on outer disks of spiral galaxies (black color) and on dwarf galaxies (blue color) obtained by Bigiel et al. (2010) and their dispersion. For this panel we use the same star formation rate coefficient as in Bigiel et al. (2010). Right panel: star formation rate densities for the same 6 H I peaks in the ring but computed with the conversion coefficient relative to Starburst99 continuous star formation models with M_up = 35 M_⊙ and dispersion due to IMF stochastic sampling. The coefficients C_FUV are in M_⊙ yr⁻¹/[erg s⁻¹ Å⁻¹]. For reference, we show the lines relative to constant depletion times of 10 and 100 Gyr.