A(Li) vs. ⟨[Fe/H]⟩ and ⟨T_eff⟩ respectively for the super-solar groups. Left panel: ⟨A(Li)⟩ vs. ⟨[Fe/H]⟩ for the super-solar groups of the sample, split into those with a direct detection of Li (LiD – round markers) and those with an upper limit estimate (LiUL – inverted triangle markers). In this representation, only the median of the top six stars with the highest A(Li) is shown in each marker. Dark magenta markers have been added to represent the meteoritic (⨂) and solar photospheric (⨀) values. The median ages of the stars represented by each marker are displayed on the legend. The black star-shaped markers display the data from Guiglion et al. (2016). It is worth mentioning that the errors associated with A(Li) are very small, and that is why they are not seen. Right panel: ⟨A(Li)⟩ vs. ⟨T_eff⟩. It is possible to see that A(Li) seems to decrease with decreasing T_eff. Indeed, the warmer temperatures seem to have a protective effect on A(Li) due to their thinner convective layers. A straight dotted black line is added to depict an approximate estimation of T_eff (i.e., at ∼5700 K) for unmodified A(Li), as shown in Romano et al. (2021).