Star formation surface density Σ_SFR as a function of total (left), thermal (middle), and turbulence (right) pressure of the ISM measured at the galactic mid-plane. The Σ_SFR measurement is the same as in Fig. 3. The black solid line in the left panel presents the relation given by Ostriker & Kim (2022) based on simulations of solar metallicity ISM boxes, while the green and red dashed lines present the metallicity-dependent relation given by Kim et al. (2024). We noticed that the numerical experiments performed by Kim et al. (2024) only extend to Z = 0.1 Z_⊙. Therefore, the red dashed line is obtained by extrapolating their fitting function to Z = 0.02 Z_⊙. The full feedback simulations follows this metallicity-dependent superlinear relation, which exhibit steeper slopes and lower intercepts compared to 0.02 Z_⊙/noRT.