Multipanel overview of the Li EWs for the eight SFRs (Cha I, η Cha, Lupus, Taurus, Orion OB1a, Orion OB1b, σ Ori, and CrA) in our sample. For each region, the left subpanel shows the Li EW versus T_eff. The red squares represent the EW corrected for blending with the Fe line ($E{W}_{\text{Li}}^{\text{Fe}}$), the black dots represent the EW after further correction for spectral veiling $E{W}_{\text{Li}}^{\text{veil+Fe}}$. K-type (T ≥ 4000 K) and M-type (T < 4000 K) stars are denoted by filled and open symbols, respectively. Arrows indicate upper limits due to the unresolved contribution of the FeI λ6707.4 line. The empirical model isochrones by Jeffries et al. (2023) at 5, 10, 15, and 20 Myr are overplotted. The right subpanels display the corresponding $E{W}_{\text{Li}}^{\text{veil+Fe}}$ distribution.