Spatially-resolved total gas Schmidt relation (Σ_SFR and Σ_H I+H2), where SFR is estimated using FUV (Eq. (5)) rather than using Hα. In each panel, blue dots with green error bars are the spatially-resolved data, and the solid black line shows the best-fit to the spatially-resolved data for all galaxies. We have assumed a Kroupa IMF and adopted a constant X(CO) factor = 2.0 × 10²⁰ cm⁻² (K km s⁻¹)⁻¹. Upper-left panel: no subtraction of diffuse background is done. The vertical dotted line corresponds to 10 M_⊙ pc⁻² around which atomic gas surface density saturates. Upper-right panel: the diffuse background is subtracted from the SFR tracers. Lower-left panel: the diffuse background is subtracted from the SFR tracers as well as from the atomic gas. Lower-right panel: the diffuse background is subtracted from the SFR tracers, HI and CO. The trend and best-coefficients of total gas Schmidt relations obtained using FUV agree with those obtained from Hα (see Fig. 8 and Table 6).